CENTRUM BADAŃ KOSMICZNYCH POLSKA AKADEMIA NAUK

SPACE RESEARCH CENTRE, Polish Academy of Sciences

ANNUAL REPORT 2018

WARSAW CENTRUM BADAŃ KOSMICZNYCH Polskiej Akademii Nauk SPACE RESEARCH CENTRE Polish Academy of Sciences Bartycka 18A, 00-716 Warsaw, Poland Phone: (48-22) 49 66 200 Fax: (48-22) 840 31 31 e-mail: [email protected] Achievements: 2018 - the year of diversity

The year 2018 shows activity of Centrum Badań Kosmicznych PAN in a variety of fields and topics. Close coupling of scientific research and technical constructions and close collaboration between scientific and engineering teams resulted in realizing several remarkable projects (enterprises). At present CBK PAN is an institute that comprehensively approaches the research and exploration of space and the Earth's environment by leading a broad spectrum of basic and applied research, creating and manufacturing new methods, techniques and innovative technologies. It is a trustful partner in European and worldwide space research. BepiColombo Europe's first mission to Mercury was set off on 20 October, 2018 on a journey to the smallest and least explored terrestrial planet in our Solar System. It is a joint mission between ESA and the Japan Aerospace Exploration Agency , executed under ESA leadership. When it arrives at Mercury in late 2025, it will gather data during its 1 year nominal mission, with a possible 1-year extension. The mission comprises two spacecraft: the Mercury Planetary Orbiter (MPO) and the Mercury Magneto- spheric Orbiter (MMO). Centrum Badań Kosmicznych PAN is involved in the MPO-MERTIS expe- riment. The MERTIS (MErcury Radiometer and Thermal Infrared Spectrometer) experiment is led by the German Space Institute at Berlin. MERTIS is dedicated to mineralogical mappings, and measure- ments of surface temperatures and thermal inertia in the spectral range 7–14 µm. CBK PAN is responsible for the Pointing Unit of this instruments. Centrum Badań Kosmicznych PAN has been involved in Chinese missions Longjiang-1 and Longjiang-2 within the project „Discovering the Sky at Longest Wavelength-Pathfinder”. China's Chang'e-4 lander and rover performed the first ever soft-landing on the far side of the Moon. Two microsatellites Longjiang-1 and Longjiang-2 launched along with a required communications relay satellite has quietly been allowing radio operators to download images from the spacecraft taken along its elliptical lunar orbit. The integrated system of electronics and antennae developed in CBK PAN made the radio measurements obtained from the instruments on board of microsatellites possible. Unfortunately, the contact with Longjiang-1 has been lost but Longjiang-2 is still in operation and offers a unique opportunity to study exceptional environment not polluted by radio frequencies interference of civilization origin. Centrum Badań Kosmicznych PAN is participating in a NASA space mission Interstellar Mapping and Acceleration Probe (IMAP), scheduled for launch in 2024. The selection of the winning proposal submitted in response to the Announcement of Opportunity was announced in Washington DC on June 1, 2018 - CBK PAN is a part of the winning team. This mission will be a more advanced continuation of Interstellar Boundary Explorer Mission IBEX, where the Polish Group was the most active team in investigation and analysis of experimental data. The objective of the IMAP mission is to investigate the interaction of the solar wind with the Sun's galactic environment and cosmic ray acceleration processes. Realization of the scientific program will result in a better understanding of the three-dimensional structure of solar wind and its evolution during the cycle of solar activity, and in a pioneering study of the temperature of solar wind electrons near the Sun. It is a great opportunity to develop one more technical specialization in the close collaboration between engineering and scientific teams. The IMAP program will be one of the most important topics of research during the coming decade in CBK PAN. The Laser Ranging Station in Astrogeodynamic Observatory has recorded a breakthrough in 2018 detecting 1857 tracks of 43 satellites and 10 debris. Expert competences developed in CBK PAN related to processing and analyzing of the SST data were recognized at the end of 2018: the Borowiec Laser Ranging Service Station became a full member of the Polish part of the Consortium Space Sur- veillance and Tracking (SST).

3 The wide expertise and involvement in conducting theoretical and experimental space research has been acknowledged by inviting CBK PAN to join the Association of European Space Research Establi- shments (ESRE). ESRE is a non-profit organization of several European space organizations: Italian Aerospace Research Centre (CIRA), the German Aerospace Center (DLR), the National Institute of Aerospace Technology (INTA), Netherlands Aerospace Centre (NRL), the French Aerospace Lab (ONERA). ESRE has been established to intensify the co-operation between European countries, integrate space research with other scientific subjects, as well as elevate competitiveness of European space sector present on the global market, and harmonize the strategy of European science and research by Euro- pean Commission and European space agency. Participation in this prestigious organization makes it possible to contribute directly to the development of European space policy. CBK PAN attaches great importance to application of current scientific achievements in space and nearest Earth's environment. Belgium, Cyprus, Finland, Germany, Italy, Netherlands, Poland and the United Kingdom appointed Belgium to create European group PECASUS on November the 7th 2018 to prepare information on current space weather conditions, and forecast for International Civil Aviation Organization ICAO. It has decided to elect global and regional organizations for information on space weather. The PECASUS Group has been qualified as global supplier. Work of start-ups of preparatory services is in course. In our promotional and educational activities (such as doctoral studies), we aim to demonstrate the significance of space research and its results to the society. Education of postgraduate students is one of the main tasks of the GeoPlanet school in the area related to environmental analysis of Earth and space. Apart from the CBK PAN, six other institutes of Polish Academy of Sciences participate in this enter- prise, namely: Nicolaus Copernicus Astronomical Centre, Center of Theoretical Physics, Geophysical Institute, Institute of Geography and Spatial Organization, Institute of Geological Sciences and Insti- tute of Oceanology. An important aspect of CBK work is continuous expert and personal support to a number of uni- versities in Poland, as well as to emerging private companies starting their operations in space.

(I. Stanisławska)

4 SPACE PROJECTS ARIEL (Atmospheric Remote-sensing Infrared Exoplanet Large-survey) This project concerns measurements of the spectral chara- • the opto-mechanical part of the FGS; cteristics of the atmosphere of planets orbiting stars of type • its warm front end electronics; F, G, K and M. These planets have temperatures in the • its control electronics; range of 250–1,000 K, and masses that range from a few • mechanical structures for the above items; and to 100 Earth masses. The Polish team is involved in techni- • mechanical, engineering and optical ground cal and scientific aspects. On the technical side, we are res- support equipment for the above items. ponsible for the so-called Fine Guidance System (FGS). Engineering, Qualification, Flight and Spare On the research side, we are simulating the measurements models of the FGS will be developed. Laboratory and interpretation of the data that is collected. performance models are at an early stage of deve- The FGS measures the spectral characteristics of lopment. The FGS operates at a temperature of distant planets at high resolution, with high- 50–55 K with detectors and so-called 'cold' front precision positioning. The optical axis jitter is end electronics; the other electronic devices will designed to be of the order of a single milli-arc operate at a temperature of 250–300 K. second. This instrument determines the highest In 2018, the ARIEL mission was selected by the possible measurement precision, and can hold the European Space Agency and phase B1 of the mis- position for a few minutes while measurements sion stared on 1 May. The CBK PAN has been able are taken. It continuously sends data to a satellite to accelerate its work schedule to meet the needs system to ensure the correct measurement direc- of this phase. Furthermore, the CBK PAN has tion. The system also takes parallel photometric contributed to the consortium in other ways, nota- measurements of selected objects. The team is bly by providing an update to the FGS design to responsible for the following items, and for provi- enable a new, four-channel approach, and new ele- ding any equipment needed to adjust and com- ctronics to be used. mission the device: (M. Rataj)

ASIM

ISS / ASIM / MXGS Gamma-ray Sensor designed by the University of Bergen The aim of the Atmosphere-Space Interactions Monitor and the University of Valencia in cooperation with the (ASIM) onboard the International Space Station is to Centrum Badań Kosmicznych PAN. The CBK PAN is study high-altitude optical emissions from the stratosphere responsible for the design and manufacture of the Power and mesosphere related to thunderstorms. One of the two Supply Unit and its autonomous (FPGA-based) House- main ASIM instruments is the Miniature-X and keeping System.

Fig. 1. The photo of US astronaut Ricky Arnold taken outside ISS 14 June 2018. The part of COLUMBUS module with the ASIM experiment mounted on CEPA platform is visible. Courtesy of NASA.

5 ASIM was launched April 2nd, 2018, with CRS-14 BUS module of ISS. Then the commissioning Falcon-9/Dragon by SpaceX. The instrument phase of the instruments has been performed was mounted on external platform of COLUM- showing the full operability of ASIM. (P. Orleański, W. Bujwan) ATHENA ATHENA (Advanced Telescope for High Energy cedented, simultaneous, high time resolution and Astrophysics) is a European Space Agency (ESA) mis- high count rate capabilities for the observation of sion, contributing to the ESA's Cosmic Vision Program- bright sources, with low pile-up and high effi- me Theme, the “Hot and Energetic Universe”. ciency. The Wide Field Imager (WFI) is one of the two The Centrum Badań Kosmicznych PAN is invol- scientific instruments proposed for the ATHE- ved in the development of two subunits: the Filter NA X-ray observatory. The lead institution for Wheel Assembly (FWA) and the Power Distribu- this project is the Max Planck Institute for Extra- tion Unit (PDU). The FWA is the current priority, terrestrial Physics (Germany). The WFI will as it contains a filter that is 200 nm thick, which provide imaging in the 0.1–15 keV band over a has to survive mechanical and acoustic loads. In wide field, with simultaneous spectral and time- 2018, we carried out further simulations and ana- resolved photon counting. The instrument is lyses, and prepared a detailed design. Further aco- designed to make optimal use of the grasp (the ustics tests to verify the simulation software were product of the collecting area and solid angle) that carried out at AGH University of Science and is provided by the optical design of the ATHENA Technology Kraków, and the results of these tests mirror system. The WFI is a very powerful survey are being evaluated. In addition, a preliminary instrument, significantly surpassing current analysis of the PDU was carried out. capabilities. In addition, it will provide unpre- (M. Rataj) BepiColombo The BepiColombo project is a joint venture between space tempt to recreate the geological past of the planet. agencies European Space Agency (ESA) and Japan The maps made by MERTIS will be the first of its (JAXA). It designs Mercury and his closest cosmic sur- kind - the instrument records the range of roundings using two independent probes. The first, weigh- infrared radiation, which has never been included ing 1150 kg Mercury Planetary Orbiter, corresponds to in the missions of space probes sent to Mercury. ESA. For preparing the second, four times lighter Mercury Centrum Badań Kosmicznych PAN was involved Magnetospheric Satellite, JAXA responds. Both were in the design, production and testing of one of the launch together, on board the Ariane-5ECA rocket from key subsystems of MERTIS: the module of ai- the European spaceport in French Guiana (South Ame- ming the optical axis of the instrument (pointing rica). The launch of the rocket took place on the 19th of unit). It is from the setting of the mirror, which is October 2018. part of the modules, what determines the line of The task of the Mercury Planetary Orbiter is to sight of MERTIS. Strictly controlled mirror measure the geophysical properties of the Mercu- movement allows you to scan the planet's surface rian globe. The probe will observe the planet with (to acquire scientific data), but also to regularly vi- eleven scientific instruments, including the MER- sualize calibration standards (ie to collect engi- TIS spectrometer (MErcury Radiometer and neering data necessary for the correction of scien- Thermal Infrared Imaging Spectrometer) develo- tific data). The CBK PAN engineers worked clo- ped with the participation of Poles. The device sely with colleagues from the German Space A- will provide information on the mineral compo- gency (DLR), who were responsible for all work sition of rocks and thermal properties of Mercu- on MERTIS. ry's surface. On this basis, the scientists will at-

6 Fig. 2. Engineers prepare the BepiColombo Mercury Transfer Module (left) and the two science orbiters (right) for integration to complete the spacecraft stack. (Credit ESA).

Fig. 3. Artist's impression of the BepiColombo spacecraft in cruise configuration, with Mercury in the background. BepiColombo will approach Mercury in 2025 after its 7 year journey (Credit ESA).

(M. Rataj) CHANG'E

Antennas for the CHANG'E 4 mission the landing site. It incorporated an orbiter, equipped with The Chinese Chang'e 4 lunar exploration mission was suc- antenna sets. Centrum Badań Kosmicznych PAN desig- cessfully completed in 2018. The main objective was to soft ned and manufactured both the electronics and mechanics land on the Moon's surface and explore areas surrounding of these instruments, together with its tubular booms.

Fig. 4. Antenna Flight Models in stowed configuration packed for shipment to China.

(Mechanical Team: T. Kowalski, J. Musiał, A. Sikorski, J. Baran, T. Barciński)

7 Chang'E-4 DSL-P mission The Chang'e-4 DSL-P (Discovering the Sky at Longest wavelengths) mission is a pathfinder for future higher-resolution, higher-sensitivity ultra-long wavelength radio diagnostic missions. The Chang'E-4 mission was succes- sfully launched from the Xi-chang Sa- tellite Launch Centre in Sichuan Pro- vince at 5:28 pm on 21 May, 2018. Two microsatellites, Longjiang-1 and Longjiang-2 (meaning Dragon River) equipped to carry out radio diagnostics in the frequency range 1–30 MHz are part of the mission. Their aim is to col- lect radio emissions from the solar sys- Fig. 5. Microsatellite Longjiang during the with test. tem, and galactic and extra galactic sources. Un- ped by the National Space Science Centre of the fortunately, manoeuvres during the lunar orbit Chinese Academy of Sciences and Centrum Ba- failed, and contact with Longjiang-1 was lost. dań Kosmicznych PAN. In particular, the CBK However, Longjiang-2 did not experience the sa- PAN was responsible for designing and building me problems, and is currently operational in an part of the radiowave analyser, and the dipole elliptical lunar orbit (200–9000 km). The far side antenna system. Initial recordings show that the of the moon serves as a natural shield against ele- instrument is operating well. In Figure 9, radio ctromagnetic interference from Earth. emissions from Earth's broadcasting stations are Both Longjiang-1 and Longjiang-2 were equipped shielded during the far side orbit of the Moon. with low-frequency radio spectrometers develo-

Fig. 6. Visual inspection: Top, Bottom, Connection views.

Fig. 7. Mounting, gluing and antenna check connection checkout views.

8 Fig. 8. Assembly and labels antenna check connection checkout views.

Fig. 9. The radio spectrum detected on the far side Lunar orbit.

9 The current mission is a pilot for a future project ding ultra-steep spectrum extragalactic sour-ces, involving eight microsatellites and a mother satel- pulsars, and (galactic and extragalactic) transients; lite. The themes of this mission will include pio- a full-sky map of continuum diffuse emission; neering searches for the unknown, and explo- solar-terrestrial physics; planetary sciences; and ratory science such as the search for signatures of cosmic ray physics. the cosmological Dark Ages. This work will com- (Co-PI H. Rothkaehl, plement current (e.g. LOFAR) searches and con- M. Morawski, Electrical Lead (Co-I) tribute to future studies on topics such as: a full- T. Barciński, Mechanical Lead (Co-I)) sky continuum survey of discrete sources, inclu- The Netherlands–China Low-Frequency Explorer

The NCLE (the Netherlands–China Low-Frequ- ency Explorer) is part of the Chang'E'-4 Lunar Pro- ject. This unique mission seeks to address a wide range of science topics, such as: constraining the Dark Ages 21-cm line and Cosmic Dawn signal; measuring auro- ral radio emissions from the large planets in our solar system; determining the background radio spectrum at the Earth–Moon L2 point; studying solar activity and space weather at low frequencies; the creation of a new, low-frequency map of the radio sky; studying the Earth's ionosphere; and the detection of bright pulsars and other transient phenomena at very low frequencies. performed at radio astronomy datacentres in Access to a previously-unexplored frequency Europe and China. On 21 May 2018, at 5:28 AM, regime will undoubtedly lead to other new disco- the Queqiao satellite, including the NCLE instru- veries. The main frequency band is 1–30 MHz, ment, was successfully launched. Currently, the extending down to 0.1 MHz, and up to about 50 spacecraft is at the L2 Lagrange point, and com- MHz. The NCLE will support a variety of obser- missioning is being performed. In 2019, we expect vational modes, including broad-band spectral to deploy the antenna system. analysis for Dark Ages, radio-interferometric The Centrum Badań Kosmicznych PAN is invol- cross-correlations for imaging, and a flexible raw ved in the development of the radio analyser. data downlink capability. Data processing will be (H. Rothkaehl Co-PI, M. Morawski) The DESIS Pointing Unit The DESIS (DLR Earth Sensing Imaging Spectrometer, that allows the instrument's line of sight to be steered under Fig. 10 is hosted on the Earth Observation Platform, as different in-track viewing angles, and provide views of in- part of the EXPRESS Logistics Carrier on the Inter- flight calibration units. The main part of the unit is the national Space Station (ISS). It consists of a hyperspectral mirror, which is rotated by a stepper motor. imaging spectrometer that covers the visible and near- The Pointing Unit is integrated into the DESIS infrared spectral range, in combination with separate power field of view (FOV) targeting system. Its main ta- and instrument control units. The DESIS was developed sk is to orient the FOV towards five different tar- for the MUSES (Multi-User System for Earth Sensing) gets for sequential data collection. These targets platform, where it is part of the Teledyne Space System are: responsible for in-orbit transportation to the ISS. The • Launch position at 0° – out of view, Pointing Unit is the part of the imaging spectrometer

10 • Earth view Default +40° (+15° off Nadir line of sight) for scientific data collection, • Earth view at +47.5° (Nadir line of sight) for scientific data collection, • Earth view at + 55° (–15° off Nadir line of sight) for scientific data collection, • Dark/ bright calibration view at +114°. In 2018, the second part of the Flight Model was manufactured, tested and delivered, and a new version of the control software was implemented and tested in time for the launch of the mission in August. Fig. 10. DESIS view from the mirror side. (M. Rataj) INSIGHT InSight (Interior Exploration using Seismic Investi- and Physical Properties Probe (HP3) destined to gations, Geodesy and Heat Transport) is a Mars lander burrow down into Mars' surface. It is meant to designed to give the Red Planet its first thorough checkup study the heat coming from Mars' interior, which since it formed 4.5 billion years ago. It is the first outer space can potentially help to answer the questions about robotic explorer to study in-depth the "inner space" of the origin and evolution of the Red Planet. MO- Mars: its crust, mantle, and core. This mission is part of LE penetrator, which is a mechatronic system car- NASA's Discovery Program for highly focused science rying the sensors that will allow this investigation, missions that ask critical questions in solar system science. was designed and manufactured by CBK PAN It was launched on May 5, 2018 from Vandenberg Air and Astronika consortium. It was successfully de- Force Base on the central coast of California. livered to Mars' surface on November 26, 2018 and has started its operation at the beginning of One of the scientific instrument is the Heat Flow 2019.

Fig. 11. InSight lander with HP3 Instrument (Credit NASA).

11 Hp3 Mole penetrator can drill up to 5 meters be- low the surface and measure how much heat is co- ming from Mars' core. The CBK PAN provided parts for the drive mechanism of the HP3 instru- ment. The manufacturing process consisted not only of machining, but also surface treatments in cooperation with Warsaw and Lodz University of Technology. (T. Barciński, J. Baran, R. Przybyła) Fig. 12. The Outer Clutch.

IONOSAT-MICRO mission Antenna for the IONOSAT-MICRO mission (Ukraine) Another antenna instrument was developed for the Ionosat-Micro mission. The tubular booms were produ- ced by the Centrum Badań Kosmicznych PAN.

Fig. 13. Antenna Flight Model in stowed configuration packed for shipment to Ukraine.

(Mechanical Team: T. Kowalski, J. Musiał, A. Sikorski, J. Baran, T. Barciński)

A high-frequency wave analyser for the IONOSAT-MICRO mission The primary objective of the IONOSAT-MI- Scientists and engineers from the CBK’s Space CRO project, led by the Ukrainian Space Agency, Plasma Group developed and constructed the is to monitor the Earth's space environment. high-frequency wave analyser. This cutting-edge More specifically, it seeks to obtain a much more equipment will make it possible to diagnose 3D complete picture of its electromagnetic plasma electric field components (spectra and wave environment and a description of the near-Earth forms) with extremely high time resolution. Data turbulent structures region. This project is one of gathered by different sensors located onboard the initial phases of the IONOSAT mission, IONOSAT-MICRO will enable investigations of which is devoted to multi-point global monitoring the fol-lowing topics: of dynamic processes in the ionosphere. IONO- - the spatial-temporal structure of inhomoge- SAT-MICRO will be launched in 2020 onboard neities in the neutral atmosphere and the iono- the Ukrainian microsatellite MICROSAT with a sphere; polar orbit of around 800 km. The payload will - the global structure and dynamics of electric contain a magneto-wave complex (fluxgate ma- currents, electric and magnetic fields; gnetometer, wave probes, electric probe), a radio - wave structures and turbulence at different frequency analyser, a density analyser and an ion scales; and drift meter. - synchronous experiments with ground support In 2018, the fight model of the radiofrequency facilities. instrument and antenna set were shipped to Ukra- ine for an onboard test campaign.

12 Fig. 14. Radiofrequency satellite configuration: Ebox and antenna system. (H. Rothkaehl, M. Morawski, T. Barciński, T. Kowalski, J. Musiał, A. Sikorski, K. Chęciński, M. Winkler) JONOSOND mission Within the framework of a contract with Russian LAERT ionosondes for top-side ionosphere, were designed by the Centrum Badań Kosmicznych PAN (Fig. 15). New, advanced so- unding techniques were developed for the space-borne exploration of the Earth's magnetosphere and topside ionosphere. The mission's four iden- tical spacecraft will be located in a polar orbit at altitudes of 600 and 800 km.

Fig. 15. Two sets of FM fight model LAERT ionosondes.

13 Each instrument consists of two parts: receiver ted with resonance plasma properties, but are de- and transmitter boxes, and an antenna pream- termined by the magnitude of the magnetic field plifier. and electron concentrations in the transparency This active investigation of the near-Earth envi- band for the considered waves. Special LAERT ronment is a unique opportunity to diagnose its regimes will be designed to register both first and complex space plasma. The project is a milestone second wave harmonics using both a trans-iono- for future spaceborne services, which will focus spheric sounding regime and the satellite itself in on diagnoses of ionospheric perturbations cau- sounding and radio-spectrometer modes. sed by seismic activity. Nonlinear resonance of In 2018, work began on the next two flight modes. extraordinary waves has already been examined. (H. Rothkaehl, A. Rokicki, M. Morawski, This found that plasma conditions are unconnec- J. Krasowski, M. Winkler) JUICE – SWI (Submillimeter Wave Instrument) The JUICE (Jupiter Icy Moons Explorer) spacecraft is an L-class mission administered by the European Space Agency (ESA), under its Cosmic Vision 2015–2025 programme. Its launch is planned for 2022. The JUICE payload is a combination of remote sensing and in-situ instruments, destined to inve- stigate the Jovian system and advance our know- ledge. The spacecraft is specifically designed to characterise the conditions that may have led to the emergence of habitable environments among the Jovian icy satellites, with special emphasis on the three ocean-bearing worlds, Ganymede, Eu- ropa and Calisto. The mission will determine the characteristics of liquid-water oceans below the icy surfaces of the moons. JUICE will also seek to characterise diverse processes in the Jupiter sys- tem that may be required to provide a stable envi- ronment on Ganymede, Europa and Calisto on geologic time scales, including gravitational coupling between the Galilean satellites and their long-term tidal influence on the system as a whole. Additionally, studies of Jupiter's atmo- sphere (its structure, dynamics and composition) and magnetosphere (three-dimensional proper- ties of the magneto-disc and coupling processes), Fig. 16. The JUICE satellite. and their interaction with the Galilean satellites the exploration of their habitable zones; 3) study will enhance our understanding of the evolution Ganymede as a planetary object and possible ha- and dynamics of the Jovian system. bitat, and study and explore Europa's young icy The Submillimeter Wave Instrument (SWI) is crust in recently active zones; and 4) explore the one of 11 instruments on-board JUICE. Its scien- Jovian system as an archetype for gas giants when tific goals are to: 1) study the Jovian system, with characterising the Jovian atmosphere and its particular emphases on the chemistry, meteoro- satellite and ring systems. logy and structure of Jupiter's middle atmosphe- The SWI is a passive heterodyne microwave spec- re, and atmospheric coupling processes; 2) trometer, sensitive to radiation in the 530–625 and characterize the regoliths, icy-crusts, atmospheres 1080–1275 GHz frequency bands. Radiation is and exospheres of Ganymede, Europa and received through a quasi-optical off-axis telescope Callisto, thereby providing important inputs for with 30 cm aperture diameter, providing a spatial

14 resolution of 2 mrad at 600 GHz. The telescope is nufacturing and testing of pre-EM DCDC, equipped with a two-axis mechanism to allow HKSW and BIAS models, then recording upda- scanning around the nadir in a range of ±76° ted power requirements for EM and flight mo- within the spacecraft's orbital plane and ±4.3° dels. perpendicular to the plane. Both the DPU and PSU pre-EMs (manufactured Two, independent, double sideband receivers pro- in 2017) were tested and delivered to the Principal vide simultaneous observing capability for two Investigator. The DPU and PSU EM1 were later frequencies in the 530–625 range of the baseline integrated with EM1 subsystems and successfully frequency band. Each receiver is connected to its delivered to the ESA. In parallel, the DPU EM2 own high-resolution chirp transform spectrome- was manufactured. Currently the board is being ter, providing a total bandwidth of 1 GHz at 100 tested. kHz resolution (10000 equidistant channels). The PSU DCDC, SWHK and BIAS EM2 models Polish participation in the SWI consists of the were comprehensively redesigned to meet the up- following work-packages: dated power specifications. Currently the docu- 1. Data Processing Unit (DPU), including mentation is being finalized before manufacturing boot software; of the PSU EM2 begins in early 2019. 2. Power Supply Unit (PSU); Development of the Radiator was conducted at 3. Radiator; the CBK PAN's Micromechanical and Photonics 4. Structural and Thermal Modelling of Laboratory. The Radiator must be able to cool the DPU, PSU and Radiator subunits. heterodyne mixers to the range of ~130K, in or- Development of the DPU and PSU is conducted der to reduce noise. Recent activities include its at the Space Applications Laboratory of FPGA at mechanical design, including finite-element ana- the Centrum Badań Kosmicznych PAN. In 2018 lysis and thermal analysis. At the end of 2018, the work on the DPU mainly related to the design and Radiator EM Manufacturing Readiness Review manufacturing of the engineering model (EM2). was successfully conducted, followed by prepa- Work on the PSU mainly related to the design, ma- rations for its manufacture.

Fig. 17. DPU Em2. Fig. 18. DPU EM2.

15 Fig. 19. DPU and PSU EM1 in flat configuration. Fig. 20. DPU and PSU EM1 model.

Fig. 21. Radiator assembly CAD model. Fig. 22. FEA of the Radiator assembly. First modal frequency. (K. Skup) The PROBA-3 mission PROBA-3 is the latest in the Eu- ropean Space Agency's line of de- monstration satellites. The mis- sion, which will launch in late 2020, is dedicated to the in-flight demonstration of precise formation flying techniques and technologies. It consists of two spacecraft, and hosts two scientific instruments: DARA (the Davos Absolute Ra- diometer), which is an absolute ra- diometer for measuring Total Solar Irradiance; and ASPIICS (Asso- ciation of Spacecraft for Polarime- Fig. 23. ASPIICS (Association of Spacecraft for Polarimetric and Imaging tric and Imaging Investigation of Investigation of the Corona of Sun. the Corona of the Sun).

16 ASPIICS is a coronagraph (a telescopic attach- sion of outputs to the scientific and wider com- ment designed to block out direct light), with the munities. The Centre's contributions are as fol- external occulter placed on one spacecraft and the lows: optical telescope on the other. The two spacecraft • Together with the Institute of Space Science will fly on a highly elliptical orbit around the (ISS) in Romania, the Centre is responsible for the Earth. The precise alignment of the telescope and independent testing and verification of perfor- occulter will create a unique opportunity to obser- mance. Both the ISS and the Centre are also invo- ve the Sun's corona close to the solar limb under lved in the development of a Parametrizable In- very low straylight conditions, and study dynamic strument Emulator, which will be used to gene- plasma processes in its magnetized atmosphere in rate data for end-to-end testing of the ASPIICS eclipse-like conditions for extended periods of Data Processing Pipeline. time. • The limited telemetry budget and limited on- The latest phase of the ASPIICS project began in board mass memory mean that an emulator is nee- July 2014. Hardware is being developed by the ded. The purpose of this software is to provide industrial consortium, including the Centrum information and make forecasts about the state of Badań Kosmicznych PAN, which is responsible on-board mass memory. The aim is to plan future for the onboard computer and filter wheel assem- observation programs and avoid overwriting exis- bly. Current work is focused on the preparation of ting data that could contain scientifically-intere- long- and short-term operational plans, the opti- sting measurements. mization of scientific outcomes, and the provi- The PROBA-3 Coronagraph Control Box The proposed PROBA-3 Coronagraph System will be the • interface with the spacecraft's on-board com- first space coronagraph to cover radial distances ranging puter (ADPMS), between 1.08 and 3 solar radii, a zone where the magnetic • drive the Camera Electronic Box, field plays a crucial role in coronal dynamics. This will pro- • drive the Filter Wheel Assembly (FWA), vide continuous observational conditions that are very simi- • drive the Front Door Assembly, lar to those found during a total solar eclipse, but without • drive the Shadow Position Sensor, the effects of the Earth's atmosphere. The system will com- • drive the Coronagraph instrument thermal bine observations of the corona in white light and polari- hardware. sation brightness with images of prominences in the He I 5876 Å line. It will also provide novel solar observations Figure 24 shows a block schematic of the CCB's that will be used to achieve two, major, solar physics science main functional subsystems, namely: the power objectives: to understand the physical processes that govern supply; the control and data processing module; the quiescent solar corona; and to understand the physical and the AEU that is used to power up and down, processes that lead to coronal mass ejections and determine and control other parts of the Coronagraph in- space weather. strument. ADPMS supplies power to, and con- trols the whole Coronagraph instrument (through The optical design of the coronagraph follows the the CCB), which, in turn, is designed to use cold general principles of a classic, externally occulted redundancy. The design of the CCB, DPU and Lyot coronagraph. The external occulter, which is PCU, system engineering, housing and harness hosted by the Occulter Spacecraft, blocks light manufacturing are all managed and executed by from the solar disc, while coronal light passes the Centrum Badań Kosmicznych PAN, while ot- through the circular aperture of the Coronagraph her manufacturing tasks and some design activi- Optical Box, which is situated on the Corona- ties have been outsourced to subcontractors. In graph Spacecraft. The Coronagraph Control Box particular, N7 Space have been contracted for so- (CCB) is the main controller, providing all pro- ftware design and to manufacture the CCB, while cessing capabilities and supplying power to the Creotech Instruments will design and manu- rest of the scientific equipment. In particular, it is facture the EGSE and the AEU, and manufacture designed to: the DPU. The main activities in 2018 were:

17 • manufacture and integration of the CCB Struc- software design, tural-Thermal Model, environment testing at • laboratory testing of development models of the CBK PAN and the Institute of Aviation, subsystems, • advanced electrical sub-systems design of the • organization of the Critical Design Review and DPU, the AEU and the PCU, progress on resolving discrepancies. • advanced boot software design and application

Fig. 24 (left). The block scheme of CCB. Fig. 25 (above). The structural-thermal model of CCB before vibration testing.

Fig. 26. The structural-thermal model for CCB before thermal-vacuum testing. (R. Graczyk)

18 The PROBA-3 CORONAGRAPH Filter Wheel Assembly Wheel Assembly (FWA) subsystem. This opto- PROBA-3 is the third PROBA (Project for Onboard mechanical system is situated in front of the focal Autonomy) mission. This experimental mission is devoted plane assembly. Its main task is to sequentially to the in-orbit demonstration of formation flying techniques position the different filter/polarisers in the opti- and technologies. The mission's high-level objectives are: cal beam of the Coronagraph Instrument. The - development to technology readiness level 9, FWA consists of: and in-orbit demonstration of formation flying • a wheel disc, including: techniques and associated technologies; - a broad-band 540–570 nm filter and its - development and validation of the engineering holder; approach, ground verification tools and forma- - a polarising broad-band 540–570 nm filter (a tion flying facilities; and filter combined with a linear polariser) and its - observation of the solar corona as part of the holder; demonstration of formation flying, based on a - a polarising narrow-band filter Fe XIV at coronagraph. 530.3 nm (∆λ = 2 nm FWHM) (a filter com- The mission will be carried out by a pair of small bined with a linear polariser) and its holder; spacecraft, which together form a coronagraph. - a polarising narrow-band filter He I D3 at The two-year mission (including commissioning) 587.6 nm (∆λ = 2 nm FWHM) (a filter com- is based on a highly elliptical orbit. The two bined with a linear polariser) and its holder; spacecraft will fly in formation, which requires - a polarising narrow-band filter Fe X at 637.5 millimetre accurate relative positioning, and con- nm (∆λ = 2 nm FWHM) (a filter combined sistently precise relative navigation. The space- with a linear polariser) and its holder; craft can manoeuvre independently of one ano- - a narrow-band filter Hα at 656.3 nm (∆λ = 2 ther, and they will typically be separated by about nm FWHM) and its holder. 150 m. • a mechanism that includes: One spacecraft will carry the Coronagraph In- strument and auxiliary units, while the second will - a stepper motor with its bearing, gearbox and carry the occulting disk. The PROBA-3 corona- coupling to the wheel disc; graph system is designed to fully exploit the un- - a position sensor and printed circuit board; precedented access to the inner solar corona, - an electrical harness routed to the Equip- which is offered by the use of formation flight. ment Box (EQB) connector bracket. Conceptually, it is a classical, white light, exter- • a mechanical bracket for mounting on the nally-occulted Lyot coronagraph, which has been EQB. modified for the formation flying configuration. • a mechanical holder for the adjusted polariser. The coronagraph is entirely protected from direct • potentially, a hold-down system for the launch sunlight by the shadow of the occulting disk that phase. is hosted by the second spacecraft. The long inter- In 2018, the Centrum Badań Kosmicznych PAN satellite distance makes it possible to reach the continued work aimed at finalising the FWA's corona, close to the solar limb, with very little stray Critical Design Review. Reports from the current light and almost none of the vignetting that degra- phase of the project were prepared and delivered des spatial resolution. to the prime contractor. The Coronagraph Instrument includes a Filter (M. Rataj) The RESONANCE High Frequency Analyser

The High Frequency Analyser (HFA) instrument will be to 1.0 MHz, and take phase difference measurements of located onboard four spacecraft within the framework of monochromatic signals at frequencies of 5.0 MHz and the RESONANCE mission. The HFA is an electronic 15.0 Mhz. module designed to measure electrical and magnetic com- The HFA instrument consists of a main unit that ponents of radio emissions at a frequency range of 10 kHz includes two, Digital Vector Receivers and a Data

19 Processing Unit. Signals to be analysed come from the three-dimensional low-frequency elec- tric field antenna set, the three-dimensional ma- gnetic field antenna set, and narrow band (5MHz and 15 MHz) antenna sets. The primary objective of the RESONANCE project is to diagnose and monitor the Earth's space environment and obtain a much more com- plete picture of the transport of energy between the inner magnetosphere and the ionosphere. Particular attention is paid to: - describing the origin and interrelation of discrete, noise-like emissions, in particular the Fig. 27. The HFA: view of the main box. generation of whistler-mode chorus waves; fine structure, and propagation features of - studying the regular and stochastic dynamics Auroral Kilometric Radiation (AKR); of energetic particles in the Earth's radiation - examining the formation and decay of the belts to reveal the mechanisms and nature of ring current and the dynamics of ions; particle energisation via wave–particle inte- - the investigation of plasma instabilities and ractions; wave excitation in radiation belts. - the investigation of the relative role of vario- In 2018, four flight models were tested and us wave modes in particle acceleration (ener- completed. Their launched is planned for 2022. gisation), pitch-angle diffusion, and precipi- (H. Rothkaehl, R. Schreiber, M. Morawski, tation; M. Walczyk, G. Juchnikowski, D. Cacko, - understanding the generation mechanism, J. Krasowski, M. Winkler) The SolpeX instrument In 2018, work continued on the development of the Sol- mission. SolpeX consists of three components: an X-ray peX instrument, which will be mounted onboard the Inter- polarimeter (B-POL), a Rotating Drum Spectrometer national Space Station as part of the Russian KORTES (RDS), and a Pin-Hole X-ray Imager. The Bragg POLarimeter In 2018, we designed the mechanical model for shifts, and make it possible to check whether the the B-POL polarimeter (Fig. 28). This device con- rotation axis is indeed directed exactly towards the sists of two identical, cylindrically bent mono-cry- centre of flaring region. The use of two, identical, stal wafers, and two Complementary Metal Oxide independent co-rotating sections will make it Semiconductor (CMOS) detectors fixed together possible to separate the rotational modulation of at an angle of ~45°. Both sections are firmly fixed the signal due to polarization, from that caused by to a table that continuously rotates along the axis the source offset. During its rotation, the position of the source of observed radiation. of the crystal dispersion plane with respect to the The crystal detector sections (see Fig. 29) face in incoming light beam will continuously change. opposite directions, and are mounted on a This will modulate the intensity of the reflected rotating table with co-aligned dispersion planes. beam provided the incident X-ray beam is linearly This X-ray Dopplerometer arrangement will ena- polarized. ble the precise determination of possible Doppler

20 Fig. 28. Left: the B-POL CAD model. Right: the B-POL mechanical model.

Fig. 29. Left: the B-POL polarimeter. Right: reflections from the silicon crystal are bent to a radius of 821 mm. The orange line is the ray path when the source is on the rotation axis. If it is offset (blue rays), the spectral line will move back and forward as the table rotates, making it possible to estimate the misalignment and automatically correct the orientation.

21 The Rotating Drum Spectrometer iron. The instrument can measure emission lines and (uniquely) the X-ray continuum. The configu- The Rotating Drum X-ray Spectrometer (RDS) ration consists of crystals that face each other on will allow us to investigate very rapid changes in opposite sides of a rotating drum. The novelty of solar spectra, and enable the creation of an atlas the approach is that very fast scanning (10 drum of contiguous spectra in the entire soft X-ray turns per second) becomes possible. Typically, the range for various plasma temperatures. In turn, Bragg-reflected spectrum would be of poor the spectral atlas will make it possible to study the statistical quality, but the instrument will make it differential emission measure distribution for va- possible to build up count statistics over time by rious plasma conditions and determine absolute assigning every recorded photon position to its abundances of elements ranging from oxygen to respective wavelength.

Fig. 30. Left: the RDS CAD model. Right: the RDS mechanical model. The pin-hole soft X-ray imager-spectrophotometer

Both the RDS and B-POL require timely informa- This imager will be used to observe active regions tion regarding X-ray activity on the solar disc. of the Sun and to locate flares. The device consists Such information can be obtained from a simple of a collimator with a pin-hole, equipped with a pinhole telescope/imager/spectrometer equip- CMOS image sensor. The filter that we developed ped with a thermal filter that transmits soft X-rays is made of aluminized polyimide that transmits in and rejects thermal/optical/extreme ultraviolet the range >0.35 keV. The image of the solar disk is emissions. Therefore, a new CAD model for the formed behind the pin-hole. pin-hole X-ray imager was developed (Figure 31).

Fig. 31. Pin-hole imager measurement block and the collimator.

(M. Kowaliński)

22 STIX (X-ray Spectrometer/Telescope Instrument) for the Solar Orbiter Mission) In October 2011, the Solar Orbiter was adopted by the SPC/European Space Agency for implementation as an M1 Mission, with a targeted launch date of 2018. The Solar Orbiter payload, designed to address the mission's scientific goals, includes a set of in- situ and remote sensing instruments, with a total mass of 180 kg. In-situ instruments consist of detectors for observing particles and events in the immediate vicinity of the spacecraft: in particular, the charged particles and magnetic field of the solar wind, radio and magnetic waves in the solar wind, and energetic charged particles flung out by Fig. 32. The Solar Orbiter Satellite. the Sun. Remote sensing instruments will observe 3. Thermal Modeling of the instrument and the Sun's surface and atmosphere. The atmo- its subsystems, (K. Seweryn) sphere is best seen via its emissions of short-wave 4. Instrument electrical ground support ultraviolet rays, which a full-Sun, high-resolution equipment (M. Kowaliński) imager and a high-resolution spectrometer will be IDPU development was conducted by the Labo- tuned to. The outer atmosphere will be investi- ratory of Space Applications of FPGA. The main gated by ultraviolet and visible-light coronagraphs challenges were to finalize the manufacturing of that blot out the bright disc of the Sun. The Sun's the IDPU flight spare model, and its integration surface will be examined using measurements of with the Power Supply Unit in the IDPU Flight visible light and local magnetic fields, detected System (FS) Box. The integrated IDPU FS Box with the Solar Orbiter's high-resolution telescope was delivered to the Principal Investigator (PI) in and magnetograph. Switzerland, and integrated into STIX's other The X-ray Spectrometer/Telescope Instru- flight spare instrumentation. ment (STIX) is one of 6 remote sensing instru- Work related to manufacturing began with finali- ments on-board the Solar Orbiter; it provides zing the assembly, and performing functional tests imaging spectroscopy of solar thermal and non- to ensure that components were correctly instal- thermal X-ray emissions. STIX will provide led. Then, flight boot software was programmed quantitative information on the timing, location, into the IDPU's EEPROM memory and the intensity, and spectra of accelerated electrons, IDPU FS was delivered to the Centrum Badań together with high temperature thermal plasmas, Kosmicznych PAN, where test environment engi- mostly associated with flares and/or microflares. neers ensured that it would work properly under Instrument Principal Investigator: Dr Sam different conditions. Meanwhile the Power Supply Krucker, FHNW, Windisch, Switzerland. Unit FS was received and tested. Finally, the IDPU Collaborating countries (HW and SW): Poland, FS and Power Supply Unit FS were integrated into Switzerland, Germany, France, Czech Republic. a common mechanical frame and these integrated Polish participation in STIX consists of the follo- subsystems were named the IDPU Box FS. wing work-packages: The IDPU Box FS was post-integration tested 1. Participation in the scientific program and and delivered to the PI in Switzerland where it was Data Reduction and Archiving (J. Sylwester) once again checked and tested. Next, it was inte- 2. Instrument Data Processing Unit (ID- grated with the Detector Box FS, creating the PU) including IDPU hardware, low level flight DEM Box FS. Following functional tests, the software and mechanical frames for the IDPU DEM was integrated with the Imager that inclu- and Power Supply Unit (delivered by the Czech ded the Aspect System (see below), creating the Republic) (K. Skup) STIX instrument.

23 In addition to its work on the IDPU, CBK PAN ct System FS was delivered to the PI. engineers also finalized work on the STIX Aspect Currently planned launch date of the Solar Orbi- System flight spare model. After testing, the Aspe- ter is February 2020.

Fig. 33. IDPU FS stack. Fig. 34. IDPU FS.

Fig. 35. IDPU FS. Fig. 36. STIX Aspect System FS. (K. Skup) TARANIS mission - MEXIC Power Units The MEXIC Power Units are two blocks (MPU1 and MPU2) of electronics that are responsible for the con- version, distribution and management of electrical power for the entire scientific payload on-board the French, Centre National d'Études Spatiales, TARANIS satellite. TA- RANIS is a low Earth orbit microsatellite mission that will provide a set of unprecedented and complementary me- asurements on the physics of TLEs (Transient Luminous Events) and TGFs (Terrestrial Gamma ray Flashes). In 2018, work continued on integrating the flight models of the MPU modules with other payload instruments and the TARANIS satellite bus. The satellite is undergoing tests and its launch is Fig. 37. The TARANIS satellite (credits: Prodigma Films, currently scheduled for the beginning of 2020. “CNES - Taranis - AIT Préparation”). (R. Wawrzaszek and the Team)

24 OTHER INNOVATIVE TECHNOLOGIES SPACE TECHNOLOGIES the robotic arm and the clamp. Numerical simula- tions were performed using the Compliant Con- The e.Deorbit Consolidation Pha- trol simulator. This tool, based on a model of the se Study system, was also developed and validated within the framework of the study. In 2018, the Centrum Badań Kosmicznych PAN took Verification of the compliant control algorithm part in the e.Deorbit Consolidation Phase Study funded by was divided into two parts. In the first part, the European Space Agency (ESA) under the General simulations were performed for the nominal case. Support Technology Programme. The purpose of the mis- In this case, the algorithm was compared with a sion is to capture and deorbit the defunct Envisat satellite. simple position controller. When contact forces The aim of the study, led by Airbus DS GmbH, was to act on the clamp and the Launch Adapter Ring consolidate results obtained in e.Deorbit Phases A and B1 (LAR), the loads on the gripper are much smaller and to work on specific topics selected by the ESA (i.e., in the case the Compliant Control is used. In the mission definition, communication block-ages, simulations second part, a Monte Carlo simulation campaign and spacecraft definition). was conducted with the following objectives: (i) to The CBK PAN was responsible for development test the proposed control for a wide range of and verification of a 6DOF cartesian force/ tor- parameters, (ii) to estimate loads induced by the que Compliant Control for the robotic arm. This motion of the arm, and (iii) to identify parameters control is needed during the clamping operation that have the most significant influence on the to ensure that the forces and torques (especially performance of the Compliant Control. The ob- those acting on the gripper) are maintained within tained results (Figs. 1 and 2) show that the Com- a certain limit preventing damage to the gripper, pliant Control is a viable solution.

Fig. 1. Results of the Monte Carlo simulation (100 runs): force and torque acting on the gripper during the clamping operation.

Fig. 2. The Compliant Control simulator: main modules and flow.

(T. Rybus)

25 Improving the mobility of a Fig. 3, where J-subsystem refers to a joint subsystem, nonholonomic space robot T-subsystem refers to the cold-gas thrusters subsystem and IMU-subsystem refers to the Inertial The main goal of our project is to define a new class of Measurement Unit subsystem. The final system planning and control algorithms dedicated to nonholonomic will consist of a satellite equipped with a planar, systems with drift in the presence of surrounding obstacles. three-link robotic arm. The space robot itself will The project is funded by National Science Center, and be equipped with two stereovision cameras. One executed by the Centrum Badań Kosmicznych PAN and will be mounted on the satellite, while the other Wrocław University of Technology. will be mounted on the end-effector of the robo- In 2018, various algorithms were developed, such tic arm. These came-ras can be used to detect as: robotic arm path planning using a rapid- obstacles in the robot's surroundings. exploration random trees method, robotic arm Special attention has to be paid to drift related to path planning using an artificial potential field angular motion. Consequently, this was the sub- method, and robotic arm path planning using an ject of extensive research and a specially-designed endogenous configuration space approach. A sphere was developed. This sphere will be placed second aspect was satellite path planning using on a spherical air bearing, giving the satellite that is natural splines with a trapezoidal velocity profile. mounted inside it the ability to rotate around all These algorithms were verified by numerical three axes at once. simulations for defined scenarios and will be CAN-BUS PC Wireless J1-Subsystem verified by experimen- USB 3.0 tal tests in 2019. M CAN-BUS J2-Subsystem

These tests will be con- a i

External vision n Synchronization CAN-BUS J3-Subsystem ducted using our 2D system microgravity test-bed CAN- BUS J4-Subsystem for the validation of Stereo camera 1 space robot control al- CAN- BUS IMU-Subsystem Stereo camera 2 gorithms, and the test- CAN- BUS T-Subsystem bed is currently being updated. The archi- Space robot tecture of the updated system is presented in Fig. 3. The space robot system architecture. (J. Sąsiadek, F. Basmadji) Investigating the influence of microgravity on mechanical subsystems

Beyond Earth, the gravity field is significantly different and the direction of the field may not be normal to the with respect to its amplitude and relations between surface. In some cases (e.g. Phobos) gravity is weak and components, as well as its spatial and temporal variability. changeable due to the significant impact of Mars. For example, any device operating on an artificial satellite The first order impact of a reduced or zero gravity is affected by the weakening of Earth's gravity field field on mechatronic devices seems to be positive. (according to the Kepler equation), which is compensated by In all static cases the gravity load is lower, which centrifugal forces due to the satellite's motion around -5 -2 seems to have the benefit of reducing stress. Ho- Earth. Therefore, devices experience low forces (10 –10 ), wever, secondary, non-trivial effects create much which may change rapidly due to the satellite's orbit and bigger problems in the design and development spacecraft orientation. On the Moon or Mars, the situation of mechatronic devices working in such envi- is more similar to Earth – gravity has a clear direction ronment. These effects are related to the follo- (although lower in amplitude) and is normal to the surface. wing phenomena: On small bodies such as comets the situation is very strange,

26 - Kinematics and dynamics of free body rotation. rbit, Observer, ORCO, NONHOLONOMIC). This is theoretically well-understood, although - Lower gravity on planets means that smaller not deeply explored by engineers due to both forces/torque or linear angular momentum are mathematical difficulties (no analytical solution needed to move an object. The effect can be both of the Euler equation) and the limitation of po- positive and negative; on the one hand it means tential applications to an on-orbit environment. that different (more effective) mobility principles The best technical example is seen in satellite can be implemented to move on the surface in- rotation, where, to actuate three degrees of stead of the typical, wheel-based mobile system. freedom, three single-axis cylindrical joints are On the other hand, even small pertur-bations, for used rather than one spherical joint. The (CBK example during sampling or drilling, can be PAN) contributed to the investigation of such a dangerous for the lander. This issue is being spherical wheel in the context of the ELSA FP7 investigated in the framework of PACK-MOON, project. REST, SAMPLER and WIERTNICA projects. - No fixation to a reference frame during on-orbit Testing such aspects is very challenging and, for operations. Most mechanical devices working on the past eight years, the CBK PAN has been wor- spacecraft need to be described as nonholonomic king on the development of an air-bearing facility. systems. Nonintegrable constraints are related to Currently, a complementary facility that can be the angular momentum conservation law. The used for underwater tests with neutral buoyancy best example is a LEMUR manipulator arm ope- vehicles is under development at Zielona Góra. rating on spacecraft, which is the topic of several (K. Seweryn, T. Rybus, F. Basmadji, P. Zagórski) CBK PAN projects (LIDER, RR-SPACE, e.Deo-

TECHNOLOGY DEVELOPMENT Landing on low-gravity bodies – tests of landing gear

The goal of the Robotically Enhanced Surface Touchdown (REST) project is to design, develop and test a scaled prototype of an actively-compliant landing gear for the Phobos mission. The Centrum Badań Kosmicznych PAN is responsible for: (i) the landing gear control system, (ii) upgrade of the air-bearing test facility for simulations of landing operations, and (iii) execution of the test campaign. Most of the CBK PAN's work was completed in 2017. The control system has been validated, and the air-bearing test facility has been upgraded. The test campaign started at the end of 2018 and is expected to end in February 2019.

Fig. 4. Air-bearing test set-up showing lander mock-up of the air- bearing cart approaching Phobos' surface. (T. Barciński, J. Musiał, A. Sikorski)

27 OTHER PROJECTS Participation in NASA projects Together with our American partners, the Solar Physics Department prepared a proposal for a new solar X-ray instrument, CubIXSS (the CubeSat Imaging X-ray So- lar Spectrometer). CubIXSS is designed to address the problem of coronal heating by filling a decades-long gap in soft X-ray observations of the solar corona during the next solar cycle, and seeks to answer the compelling question: How is plasma heated to millions of degrees throughout the solar corona? In particular, CubIXSS will measure the complete temperature distribution (from ~1 to ? 30 MK) and abundances of low and high first ionization potential elements, to explore two questions: Fig. 5. Simulated CubIXSS observations. 1. Are active and quiet Sun regions heated by nanoflares or waves? pact, inexpensive spacecraft. Simulated Cub-IXSS 2. How are hot plasmas formed in solar flares, and observations are shown in Figure 6. over what timescales? The proposal has been submitted and, if accep- CubIXSS will achieve this by combining spatially- ted, the Department will be responsible for came- integrated spectrometers with an innovative ra drive electronics, and the field program-mable spatially-resolved imaging spectrometer in a com- gate array core. (Sz. Gburek) The FOXSI project FOXSI (the Focusing Optics X-ray Solar Imager) is another project that is under development with American partners. The assessment phase ended in 2018 and we are awaiting a decision from NASA on further funding. This decision is expected in the second quarter of 2019. FO- XSI is the first solar instrument with direct hard X-ray imaging capabilities, and it addresses universal science is- sues regarding heating and particle acceleration in magne- tized plasmas. In particular, it seeks answers to three questions:

1) How are particles accelerated at the Sun? 2) How are solar plasmas heated to high tempera- tures? 3) How does magnetic energy released on the Sun produce flares and eruptions? The Solar Physics Department is also working on the Spectrometer for Temperature and Composi- tion (STC) instrument for the FOXSI project. The STC will extend FOXSI measurement capa- bilities to softer X-rays. Two of the CBK PAN scientists are Co-Investigators on the project. Fig. 6. Simulated FOXSI X-ray image of a solar flare. (Sz. Gburek, M. Stęślicki)

28 The IMAP GLOWS Experiment of interstellar matter near the Sun and its intera- ction with the solar wind. The Centrum Badań Kosmicznych PAN partici- Development of the GLOWS instrument will be pates in the NASA space mission, Interstellar carried out in collaboration between an engi- Mapping and Acceleration Probe (IMAP), sche- neering team from the CBK PAN, led by Dr Piotr duled for launch in 2024. The selection of the Orleański, and two German institutions. The winning proposal, submitted in response to the Centrum will be responsible for development of Announcement of Opportunity released in 2017, the power supply, the onboard computer and soft- was announced in Washington DC on 1 June, ware, and integration of the instrument. The 2018 (https://www.nasa.gov/press-release/ na- German partners will provide the instrument's sa-selects-mission-to-study-solar-wind-boun- detector and optical blocks. The Principal Inve- dary-of-outer-solar-system). The Centrum, in col- stigator in Germany is Professor Hans J. Fahr laboration with partners from Germany, will from Bonn University. Involvement in the IMAP supply a two-channel photometer called GLOWS project is very important for the CBK PAN and (GLObal solar Wind Structure). The objective of the program will be one of its most important re- the IMAP mission is to investigate the interaction search activities during the coming decade. The of the solar wind with the Sun's galactic environ- GLOWS experiment will result in a better under- ment and cosmic ray acceleration processes, as standing of the three-dimensional structure of presented in a paper by McComas et al. published the solar wind and its evolution during the cycle of in Space Science Reviews (https://link.springer. solar activity, and will include a pioneering study com/article/10.1007%2Fs11214-018-0550-1). of the temperature of solar wind electrons near The IMAP mission is being developed and will be the Sun. Based on planned observations, the carried out by an international science team led by GLOWS team will be able to investigate the Principal Investigator Dr David J. McComas from fundamental issue of energy transport in the solar Princeton University. The project is managed by wind close to its source region. Equally important the Applied Physics Laboratory of Johns Hop- are ongoing studies of interstellar neutral gas. kins University. IMAP will have ten science instru- The IMAP mission is a continuation of a multi- ments, including the GLOWS experiment and will year program of researching the heliosphere and operate near the libration point L1 between the its galactic environment, in the context of the Earth and the Sun, about 1.5 million km from the existing NASA mission Interstellar Boundary Ex- Earth. plorer (IBEX), as well as other projects. GLOWS A team of scientists and engineers from the CBK represents a quantum leap for the Centrum's PAN, led by Professor Maciej Bzowski from the research activities as it will be the first heliospheric LSSPA as the Principal Investigator, proposed an experiment to be conceived, developed, and ope- instrument to perform observations of the helio- rated by its scientists. The Centrum's role in the spheric resonant backscatter glows in the hydro- GLOWS instrument is a natural continuation of gen and helium spectral lines (121.6 nm and 58.4 work carried out by its FPGA Laboratory of Sa- nm, respectively). The team will use these remote- tellite Applications. It draws upon experience sensing observations to investigate variation of gained in the past from the many highly- the solar wind flux with heliolatitude and the successful space missions the Laboratory's temperature of solar wind electrons within a engineers have been involved in, including hundred solar radii from the Sun's surface. A Integral, MEX, Chandrayaan, Herschel, CaSSIS, second element of the CBK PAN involvement in ASIM, Solar Orbiter, and presently OpSat, the IMAP mission is the IMAP-Lo experiment, PROBA3 and JUICE. The high level of technical led by Dr Nathan Schwadron and Dr Eberhard readiness of the proposal, supported by a vast Moebius from the University of New Hampshire. heritage of space-proven solutions, was an Here, LSSPA scientists in collaboration with their important factor in the selection of the GLOWS US partners will investigate the neutral gas that instrument, which is a great opportunity for the enters the heliosphere from the solar galactic Centrum's engineering team to develop another environment. The results of these studies will specialization. A very important aspect, in this res- improve our understanding of the physical state

29 pect, is close collaboration between engi-neering Furthermore, the Centrum's engineers have a and scientific teams during the develop-ment of long record of successful collaboration with the experiment and its planned operation in space. international partners from Europe (the ESA), Studies of the heliosphere and its cosmic Russia, China, and India. GLOWS is the start of a environment are a very important part of the technical collaboration with NASA. Centrum's science mission. The development and Co-Investigators on the IMAP Science Team implementation of the GLOWS experiment is a include Dr Maciej Bzowski, Dr Justyna M. Sokół, natural continuation of a long-standing colla- Marzena A. Kubiak MSc (from the LSSPA) and boration between the Centrum's scientists and Dr Paweł Swaczyna, currently a post-doctoral German partners, as well as US colleagues: Dr researcher at Princeton University. The engi- David McComas from Princeton University, and neering team is led by Dr Piotr Orleański. Dr Eberhard Moebius and Dr Nathan Schwadron (M. Bzowski) from the University of New Hampshire. NAVISP A GNSS RECEIVER FOR MICRO-LAUNCHERS AND MICRO-SATELLITES The main aim of this project is to develop advan- versions will be developed: ced software for a Global Navigation Satellite • a small launcher version – a single L1/E1 System (GNSS) receiver, based on registering and band GNSS receiver processing GNSS signals (the so-called SDR tech- • a small satellite version – a dual band L1/E1 nique). The project is funded by the European and L5/E5 receiver Space Agency within the framework of the Similar activities were launched last year within NAVISP (NAVigation Innovation Support) Pro- the framework of another contract. Under this gramme, and the consortium is made up of GMV contract, a breadboard version of the Front-end Innovating Solutions Sp. z o.o. (leader), Hertz Sys- Electronics (FE) for the single band (L1/E1) re- tems and the Centrum Badań Kosmicznych PAN. ceiver has been developed (Fig. 7). The final FE The CBK is responsible for the design and deve- version is in preparation and work is expected to lopment of hardware and preparations for testing be completed in early 2019. Heritage from this the experimental micro-launcher, MURIA-1. work is a base for activities of current project with In 2018, activities focused on requirements' speci- respect to FE activities. Second part of the project fications, the initial definition of design concepts assumes utilization of one of OBCs solution and analyses of potential hardware solutions. Two which are studied in CBK PAN.

Fig. 7. Breadboard model of the Front-end Electronics for the single band GNSS receiver.

(R. Wawrzaszek and the Team)

30 RENESANS An Attitude and Orbital Control System for the HyperCube platform

The purpose of the AOCS project is to design and Research and Development (Narodowe Centrum develop a positioning and orientation control Badań i Rozwoju). Depending on the results of system (Attitude and Orbital Control System) for ongoing analyses, appropriate components will be a new, modular and scalable satellite platform bought or developed, control software will be proposed by the company Creotech Instruments designed, and a testing system will be developed. SA. The project is the result of a contract with In 2018, initial work began and activities were Creotech Instruments, which obtained financial focused on requirements' specifications and the support from the Polish National Centre for early definition of design concepts.

Fig. 8. Mock-up of Astro-Sat: concept of the satellite which base on HyperCube platform (Credits: Creotech Instruments SA).

(R. Wawrzaszek and the Team)

31 DATA ACQUISITION Astrogeodynamical Observatory of the Centrum Badań Kosmicznych PAN in Borowiec A second caesium fountain for Poland

At the beginning of November 2017, a second caesium CBK PAN's fountain was installed at the Poznań Super- computing and Networking Centre. This fountain joins the exclusive club of the most accurate atomic clocks in the world, and is the second such clock in Poland.

The most stable local timescales consist of a fly- wheel clock, usually a hydrogen maser, the fre- quency of which is controlled using corrections provided by an atomic fountain frequency stan- dard. The microwave source, used in the fountain to interrogate the atomic absorbers (the local oscillator, LO), is usually weakly phase-locked (i.e. with a time constant of up to tens of seconds) to the maser clock. While it is possible to stabilize the LO using the fountain's data directly, the solution is not practical as the atomic resonance frequency is usually intentionally varied during both the characterization phase and regular operation, in order to measure or control systematic frequency shifts. The maser acts therefore as a flywheel oscillator. A cold-atom fountain primary fre- Fig. 1. An example of the new fountain systems, showing the physics package. quency standard consists of a physics package (a vacuum vessel with cooling, detection and flight implemented in the NPL-CsF3 fountain. Free chambers, and microwave cavities), an optical precession occurs while atoms travel within a assembly producing light for atom cooling and waveguide, below a cut-off to eliminate the detection, microwave sources, and an electronic influence of stray microwaves. control system. The physics package, shown in The entire cavity and free precession regions are figure 1, is largely based on an approach initially temperature-controlled to prevent cavity pulling developed for theNPL-CsF2; namely, a single- effects and uncontrolled blackbody radiation stage magneto-optical trap as the cold atom shifts. source, optical pumping into the mF=0 clock state, The 10 MHz reference signal for the microwave and cancellation of the collisional shift to enable synthesizer is transferred via a dedicated optical high accuracy. fibre link with an electronically- stabilized time Improvements to the NPL-CsF2 include the delay. We ran two fountains with quartz-based reduction of the overall size of the structure, rigid local oscillators, one co-located with a referencing fixing of the vacuum vessel to a supporting frame, maser, and the second linked to it by 34 km of and pre-aligned optics for cooling and detection, buried optical fibre forming part of telecom- which are attached directly to the vessel. Ramsey munication infrastructure. interrogation is performed in a state-of-the-art A key technical challenge in developing optical microwave cavity that minimises the distributed fibre time and frequency transfer technology is cavity phase frequency shift, using a design first stabilising the delay (phase) of the signal trans-

32 mitted through the fibre. One technique developed to address this problem is electronic stabilization (ELSTAB) technology developed at AGH University. The solution is based on sensing and cancelling round-trip delay fluctuations by means of a pair of precisely-matched variable delay lines placed in forward (local-to-remote) and backward (remote-to-local) signal paths. Our work shows that the addition of the delay- stabilized fibre link, delivering the remote 10 MHz reference, does not degrade the short-term stabi- lity of the standard fountain—as long as the bandwidth of a servo locking the local oscillator to the maser reference is optimized. Relative to the stability of the fountain, the ELSTAB noise contribution becomes negligible for averaging times longer than 1000 s. This is far superior to alternative methods, such as satellite-based com- parisons, which require several weeks of integra- tion to reach the same statistical uncertainty as a caesium fountain. Fig. 2. The fountain co-located with a maser reference, and a remote fountain operating at Poznań. (J. Nawrocki) The GNSS BOR 1 station Data streams from the BOR1 station have been In 2018, the long-term provision of Global Navigation made available through IGS-IP and EUREF-IP Satellite System (GNSS) data from the BOR1 station, for projects. High-quality data files make a valuable national and worldwide scientific and surveying, was contribution to the global geodesy and related secured. This permanent GNSS station is located at the research within the IGS framework. Data Centrum Badań Kosmicznych PAN Borowiec Observa- provided by BOR1 are used for precise orbit tory and, since 1996, it has been integrated into Interna- calculations by many international institutions, tional GNSS Service (IGS) and EUREF networks. such as CODE (Central Orbit Determination Europe) at Bern Switzerland, the GFZ-IGS

Fig. 3. The Trimble GNSS antenna installed at the BOR1 station since 5 October, 2016.

33 Processing Centre in Germany, the JPL-IGS/ FLYNN Processing Centre at Pasadena, USA, the Massachusetts Institute of Technology in the USA, the Scripts Institution of Oceanography in the USA, and the National Geodetic Survey in Canada. The BOR1 station is one of the reference stations within the multifunctional, precise satelli- te positioning system established by the Head Office of Geodesy and Cartography in Poland. All of the station's data are provided in two formats: RINEX 2.11 and RINEX 3.02. All data are gathered by a Trimble Dorne Margolin with choke ring antenna (Fig. 3), which collects signals from GPS, GLONASS, GALILEO, BEIDOU, QZSS and SBAS systems (Fig. 4).

Fig. 4. Satellites observed by the GNSS BOR1 station. Since 5 February, 2015 the BOR1 station has been receiver is capable of gathering signals simulta- equipped with a multisystem Trimble NetR9 neously from GPS, GLONASS, GALILEO, receiver (Fig. 5). This multichannel (440 channel) BEIDOU, QZSS and SBAS constellations.

Fig. 5. The Trimble NetR9 receiver installed at the BOR1 station.

( P. Lejba, P. Michałek)

34 The BORL satellite laser ranging station From an observational point of view, 2018 was a record 483 space debris passes were performed. Infor- year for the CBK PAN's laser ranging station (BORL). mation about the position and behaviour of space For the first time in the long history of laser measurements debris such as defunct satellites is very important in Poland, the BORL station recorded more than 1100 from the point of view of future debris removal passes of tracked objects. Only two times in its history has missions (e.g. ENVISAT). We need to know not the number of passes exceeded 1000: in 1999 (1060) and only where it is, but also precise information about 2003 (1092). its rotation/tumbling and orientation in space. Laser measurements recorded by the BORL In 2018, the BORL station tracked 53 different station support global research on the determina- objects, satellites and pieces of space debris (co- tion of space debris spin dynamics (ENVISAT, operative and uncooperative targets), with a total ERS-1, ERS-2, OICETS, SEASAT-1, TOPEX/ of 1857 full passes (Fig. 6). Forty-three were Poseidon and others), which is essential to impro- satellites, 29 were Low Earth Orbit (LEO), and 14 ve theories of the movement of artificial satellites. were Medium Earth Orbit objects. Ten objects All results were sent to the Crustal Dynamics Data were typical space debris, in particular, inactive Information System and Eurolas Data Center (defunct) satellites from the LEO regime. These databanks and all satellite recordings from the targets were observed within the framework of BORL station in 2018 are available to the public at the Space Debris Study Group run by the Interna- http://www.cbk.poznan.pl/stacja_laserowa/lista tional Laser Ranging Service (ILRS). A total of _obserwacji.php.

Fig. 6. Observational statistics recorded by the BORL station in 2018. In 2018, staff at Borowiec worked on a second 8'' guiding telescope equipped with two fast independent optical-laser system, dedicated to the dedicated optical CMOS cameras. The whole Space Surveillance and Tracking (SST) program- system is controlled by multiplatform steering/ me, developed by European Space Agency (ESA) tracking software (Fig. 8) supporting space and European Commission (EC). The new sys- debris/satellite prediction, real-time laser obser- tem is based on an azimuth-elevation mount with vations, system calibration, ADSB monitoring a 65 cm Cassegrain telescope (Fig. 7) equipped (Fig. 9), data post-processing and other functions. with servo drives. These provide very fast trac- When fully implemented, the system will operate king, with accuracy better than 1 arcsec and a RC 24 hours a day, 7 days a week.

35 Fig. 7. The second independent satellite laser system developed by the CBK PAN (main telescope).

Fig. 8. The second independent satellite laser system developed by the CBK PAN (operator room).

Fig. 9. Screenshot of the ADSB system with a second optical-laser setup developed by the CBK PAN.

36 Fig. 10. Optical tracking of the CRYOSAT-2 satellite Fig. 11. Optical tracking of the ASTRA constellation (LEO regime) by the second BORL setup. (GEO regime) by the second BORL setup. ?Optical measurements will be used to chara- This project will start in the middle of January cterise space missions and SST activity. In the test 2019 and will run for 18 months. phase, a special spectroscopic module was dedi- • “MOST – Mobile Optical Tracking Station” is cated to recording the physical characteristics of a three-year project funded by the National tracked targets. The first results of these tests (for Centre for Research and Development. The the JASON-3 satellite) were presented during the CBK PAN is an approved subcontractor, and is 21st International Workshop on Laser Ranging responsible for the analysis of the laser com- (International Workshop on Space Debris Mana- ponent of the station's equipment. gement and Mitigation) in Canberra (Australia). In 2018, the BORL station focused on the SST The next step in the development of the new programme, which constitutes one of the pillars BORL setup, planned for 2019, is the integration of the Space Situational Awareness (SSA) pro- of the whole system with a laser module. gramme implemented by the ESA and the EC. In 2018, staff at the BORL station were involved The SST programme is dedicated to monitoring in the following projects: (observation and detection) of active and inactive • The ILRS project, Special Mission Support, satellites, discarded launch stages and fragmen- which is an observational campaign dedicated tation debris orbiting Earth. The BORL station is to SENTINEL-3A and SENTINEL-3B responsible for research and development in satel- satellites. The CBK PAN was an approved sub- lite laser ranging. At the end of 2018, Poland beca- contractor and the project is onoging. In 2018, me an official member of the EU SST Consor- the BORL station collected 56 passes of tium, and the CBK PAN is one of the members of SENTINEL-3A with 898 normal points, and the Polish SST consortium. 31 passes of SENTINEL-3B with 445 normal In 2018, several events took place on the subject points. of laser/timing techniques, and the SSA/ SST In 2018 the BORL station secured funding for programme, which BORL staff participated in. three projects: The most important were: • The ESA project “WebPlan”, within the • 23 February, 2018 – Users' workshop on SSA, framework of the Polish Industry Intensive at the Albert Borschette Conference Centre, Scheme. The CBK PAN is an approved sub- Brussels, Belgium. contractor. This project started at the begin- • 3–4 July, 2018 – bilateral meeting at Borowiec ning of December 2018 and will run for 12 with representatives of the DLR Institute of months, plus 6 months' support. Technical Physics. The main topic of the • The ESA project “SST Sensor Data Acqui- meeting was related to Space Surveillance and sition”. The CBK PAN is an approved subcon- Tracking activity. tractor. The BORL station is responsible for • 5–9 November, 2018 – 21st International laser measurements of uncooperative targets.

37 Workshop on Laser Ranging (International a presentation (Mission characterisation of Workshop on Space Debris Management and LEO targets) was given by Dr Pawel Lejba, Mitigation), Canberra, Australia, where a manager of the Borowiec Observatory, and poster (Laser activity of the Borowiec laser Head of the BORL station. station in years 2017-2018) was presented, and (P. Lejba) The Global Navigation Satellite System (GNSS) Observatory in Warsaw

The observatory is involved in the following projects: - monitoring the quality of EGNOS corre- - the GALILEO global navigation system, ctions under the European GNSS Agency - positioning measurements and defining the (GSA) grant - EGNOS Service Perfor- national reference frame with GNSS techno- mance Monitoring Support (SPMS), logy, - Galileo performance monitoring.

GALILEO In 2009, a new GESS+ (Galileo Experimental Sensor of testing observed data quality, the station was included in Station) was installed at the CBK PAN. After few months the global monitoring network of GIOVE satellites.

Fig. 12. The new GALILEO GESS+ station (GWAR) at the CBK PAN, Warsaw. Each week, ESA-ESTEC generates reports of the toring the Galileo system, the CBK PAN is parti- status of stations and observation data quality for cipating in the GSA project Galileo Reference GPS and Galileo signals. In the context of moni- Centre – Member States. (L. Jaworski, A Świątek) GNSS PERMANENT STATION Since February 2003, a permanent GPS station has ope- 2007, that station has been included in the ASG– rated in Warsaw, as part of the pilot project Active Geo- EUPOS project. In 2015 at the station a new GNSS detic Network for Poland (ASG-PL). From December Trimble NetR9 receiver was installed. (L. Jaworski, A Świątek) The European Geostationary Navigation Overlay Service (EGNOS) CBK PAN in Warsaw is the location for a Ranging and designed to broadcast correction signals in Europe for Integrity Monitoring Station - the RIMS WRS station. improving GPS performance (Fig. 13). This station is part of the EGNOS System, which is

38 Fig. 13. EGNOS Ground Segment.

In addition to the RIMS station, the CBK PAN is is participating in the EGNOS Service Moni- cooperating with European institutions on rese- toring Support project. arch based on the EGNOS System. Specifically, it (L. Jaworski, A Świątek)

39 INTERPRETATION AND MODELLING SPACE PHYSICS Our new calculations provide an exceptional de- scription of the relative intensities formed in va- Solar Physics rious calcium lines. The updated line formation theory was successfully applied to earlier flaring (Wrocław Solar Physics Division) plasma spectra observed by the NRL SOLFLEX A new analysis of Diogeness data experiment aboard P78-1, and ALCATOR C- Mod tokamak laboratory spectra. Diogeness is an X-ray spectrometer that operated aboard the Russian CORONAS-F satellite in 2001. The in- strument collected hundreds of high-resolution spectra from a period of high solar activity including, on 25 August 2001, an X5.3 flare. This flare (see Fig 1) was also obser- ved by the American Geostationary Operational Environ- mental Satellite (GOES) and the Japanese/NASA Yoh- koh satellite. In 2018, we continued work on a compre- hensive re-analysis of the instrument's spectra recorded during the flare; our results were published in The Astro- physical Journal (https://doi.org/10. 3847/1538-43 57/aace5b).

Fig. 2. Plot of DIOGENESS spectra during the 25 August 2001 solar flare averaged over five temperatures (vertical axis) beginning at 12.8 MK.

Fig. 1. The 25 August 2001 X5 flare. Upper panel: Photon count rates for the DIOGENESS channel 1 (red dots), channel 4 (blue dots) and Yohkoh (green curve). DIOGENESS peaks are due to calcium lines as the crystals are repeatedly scanned. The data gap between 16:42 UT and 16:49 UT is due to telemetry loss. Lower panel: Temperatures derived from the intensity ratio of the two GOES channels. Our dataset consisted of flare spectra averaged over five temperatures (see Fig. 2), and we identi- fied dozens of lines in the astrophysical plasma, many of them for the first time. These lines mainly correspond to helium and lithium-like calcium ions. Our theoretical calculations of line Fig. 3. Synthetic spectra for temperatures ranging from 4 intensities were based on Cowan's atomic code MK (bottom) to 30 MK (top). Different colours (blue, orange, red, yellow) indicate increasing intensities. The and Hartree–Fock wavefunctions for hundreds most interesting lines are shown at the top of the figure at of transitions in the observed spectral range. a temperature equal to 13.8 MK.

40 Fig. 4. DIOGENESS spectra for temperatures of 13.4 MK, 15.1 MK, 16.8 MK, and 20.7 MK. The solid red line shows best-fit theoretical spectra, and the blue line shows an argon spectrum.

(B. Sylwester, J. Sylwester) An analysis of RESIK differential emission measure distributions In 2018, we continued our analysis of differential emission CORONAS-F satellite in 2001. Preliminary results measure distributions for the complex flare observed by the were presented at the Second VarSITI General RESIK X-ray spectrometer flown onboard the Russian Symposium in Irkutsk in 2017. In 2018, we recalculated

Fig. 5. Left: An example of the decomposition of the RESIK light curve for the 9 January, 2003 flare showing four elementary flare profiles. The purple line indicates the summed profile. Right: Differential Emission Measure (DEM) distributions of the four flares integrated over the entire time range, obtained by the decomposition of RESIK light curves into four elementary flare profiles. Colours correspond to the profiles shown in the left panel.

41 our dependences and carried out an in-depth analysis of RESIK and GOES data. A detailed description of our work was published in The Journal of Atmospheric and Solar-Terrestrial Physics (doi: 10.1016/j.jastp.2018. 09.004). In particular, we applied the elementary flare pro- file (EFP, proposed by Gryciuk et al. 2017) model to RESIK spectra interpretation. The EFP model makes it possible to distinguish individual flare components based on observed light curves in se- lected spectral bands, and therefore study diffe- rential emission measure distributions for indi- vidual components of the complex event. This new approach has not previously been described in the literature. The subject of the analysis was the flare on 9 January, 2003. This flare lasted about 40 minutes and consisted of four overlapping events with intensities ranging from 30–80% of maximum flare intensity and durations of ~10– Fig. 6. Change in temperature (red line), emission measure (blue line) and thermodynamic measure (black line) 30 minutes. calculated from GOES data for an isothermal We also performed a complex analysis of the approximation using the flux-ratio technique for pre-flare long-duration event observed on 15 April 2002. signal subtracted fluxes. Here, we studied the morphology and physical pa- rameters that characterized conditions in flaring tion of this flare was very complicated, and that it plasma. Images from the SOHO Extreme ultra- was still visible a few hours after the event maxi- violet Imaging Telescope show that the configura- mum.

Fig. 7. Left: Distributions obtained for a selected time interval. Differential emission measure distributions were determined using two methods: Withbroe-Sylwester (WS) and differential evolution (DE) in the temperature range 3–30 MK. Right: observed (in black) and synthetic (in green) spectra calculated from the corresponding differential emission measure distribution. (A. Kępa)

42 RESIK–RHESSI cross-calibration In the last years, new calibration data became available, and we revisited the problem of comparing X-ray fluxes measured by two instruments: the Centrum Badań Kosmi- cznych PAN's RESIK spectrometer (flown aboard the Coronas-F satellite) and the Reuven Ramaty High Ener- gy Solar Spectroscopic Imager, known as RHESSI, which was a NASA Small Explorer Mission. The analysis was based on solar flare spectra observations in 2002 and 2003. Our results are summarised in Figure 8. This figure shows that for the dataset of 360 cases, RHESSI mea- surements are higher than RESIK measurements for fluxes in the range 3.00–3.67 keV (3.38– 4.13 Å). The difference may be due to uncertainties in RHESSI calcu- lations in this energy range. This result will be used to com- Fig. 8. RESIK and RHESSI cross-calibration. RHESSI fluxes (y-axis) are generally higher then RESIK fluxes (x- pare observed RESIK spectra with spectra calculated from axis). Solid and dashed black lines represent the y=x flaring loop models derived from RHESSI data. function and the correlation obtained in 2006, respectively. (A. Kępa, M. Siarkowski) Is there hot plasma in the Sun's corona even when it's quiet? Using spectra collected by the Polish spectrophotometer Our paper, published in 2012, reports the results SphinX, aboard the CORONAS-Photon we addressed of that work. We selected 27 time intervals, lasting the intriguing question of whether hot (~10 MK) plasma from one to several hours, when the photon count exists in parts of the Sun's corona even when there are no rate was at its lowest (~100 counts/s). Spectra in active regions (AR). SphinX observed the Sun's X-ray these intervals were analysed, and the average radiation throughout most of 2009, including periods of corona temperature and emission measure were exceptionally low activity when not even the smallest ARs determined. Temperature was obtained by fitting could be detected in X-ray and extreme ultraviolet images, the observed spectrum to the theoretical one, in and no sunspots were reported. At that time, SphinX was the range 1.2–2.7 keV. In a subsequent step, we the most sensitive instrument opera-ting in the spectral deepened the analysis by dividing the 27 selected range >1.2 keV, and spectra were recorded over numerous intervals into 141 shorter, sub-intervals. The no-AR periods lasting up to a few days. results are presented in Figure 9.

Fig. 9. Obtained isothermal temperatures for the 141 sub-intervals.

Our analysis found in these very quiet conditions, statistically-important changes (so-called brigh- tening) is sometimes observed. An example is shown in Figure 10.

43 Fig. 10. An example of brightening. Black dots correspond to the original data smoothed with 51 points; blue dots are smoothed with 11 points. The red line denotes the pedestal (the level for points with lowest count rates), the yellow line represents points with more than 1000 counts. Green dots correspond to count rate levels 4σ above the general trend (i.e. brightening). We found 20 brightenings in the 141 sub-inter- (>5MK) component. The proportions of these vals. To check whether our approximation did low- and high-temperature plasma components describe the temperature of the non-flaring coro- are shown in the right panel of Figure 11. na, we analysed SphinX spectra using multiple Our initial analysis indicated that most plasma is at temperatures (1–15 MK). The multi-temperature a temperature of ? 2 MK. However, more detailed model used a Bayesian differential emission mea- calculations revealed that the source plasma is sure (DEM) deconvolution algorithm that was actually made up of two components: in addition tested on artificially-generated sample spectra. An to the main plasma (at a temperature of <2 MK) example of the results for sub-interval 33 is there is a smaller (by orders of magnitude) amo- presented in the left panel of Figure 3. This shows unt of higher-temperature (2–10 MK) material. that the main emitting plasma component is at a This analysis leads us to conclude that there is a temperature of ~1.8 MK, which is close to that hot component of plasma present all the times in found using our isothermal approach. However, the corona, even when solar activity is at its lowest. there is also a smaller, higher temperature

Fig. 11. Left: An example of DEM for the sub-interval 33. Right: The proportion of lower- (<2MK; black) and higher- (2–10MK; red) temperature amounts of plasma for all 141 sub-intervals. (B. Sylwester, J. Sylwester)

44 Comparing SphinX and RHESSI data In 2018, our analysis of solar microflare observations continued. The SphinX instrument was developed by the Centrum Badań Kosmicznych PAN's Solar Physics Divi- sion, and was used to observe the Sun in 2009. At that time, it was the most sensitive instrument in the 1.2–15 keV spectral range and, as such, offered an excellent oppor- tunity to compare its observations with spectra from the Ra- maty High Energy Solar Spectroscopic Imager (RHE- SSI), as both instruments record measurements in the range where most flare energy is found. We selected four, conse- cutive small solar events observed on 4 July 2009 (13:43 Fig. 12. Example of SphinX (black error bars) and UT, 13:48 UT, 13:52 UT, and 13:55 UT) and used RHESSI (red error bars) spectra for the maximum of the them to compare data and results from the two instruments. strongest analysed flares (13:55–13:56 UT). We extended the analysis to include Geostationary Ope- differences in obtained emission measures, rational Environmental Satellite (GOES) records. In while derived plasma component temperatures practice, the comparison was limited to ~3–6 keV. are similar. The RHESSI hot component agrees Our results were published in Solar Physics (https: well with GOES, while its hotter component //doi.org/10.1007/s11207-018-1319-0) and can fits well with the SphinX flaring component, be summarized as follows: and variability is consistent. • In the 4–6 keV range we observe a systematic • Due to differences in the respective spectral shift between spectral irradiances for SphinX irradiance levels, there are (smaller) uncer- and RHESSI data. In particular, SphinX values tainties in derived values of total thermal ener- are about three times higher. gy content in the four microflares. There is high • We compared SphinX fluxes with RHESSI me- agreement for derived values and variability of asurements calculated for separate detectors. the so-called 'thermodynamic measure' for Measurements were consistent in the 3–4 keV SphinX, GOES and RHESSI instruments. range, and for RHESSI detectors 1, 4 and 9. • The SphinX instrument is a very sensitive • The shift in spectral irradiance contributes to complement to RHESSI and GOES.

Fig. 13. Correlation plots of RHESSI and SphinX ? uxes for three energy bands. The dashed line represents the linear ? t to 4–6 keV data. (T. Mrozek)

45 Basic research on coronal and photospheric activity In 2018, we carried out an initial comparison of solar SOHO/MDI Debrecen Sunspot Data. Our preliminary photospheric and coronal activity. The dataset was com- results indicate that higher coronal activity can develop posed of images from the X-ray telescope operating on the without increased activity in the photosphere. Hinode satellite, X-ray measurements from the SphinX (Sz. Gburek) instrument, the Debrecen Photoheliographic Data, and Dynamics of the outer radiation belt during geomagnetic substorms The SphinX instrument and the STEP-F satellite substorms in May 2009. This highlighted the belt's double- telescope are located close to each other on the external pla- peak, L-shell profile, and an increase in electron fluxes that tform of the CORONAS-Photon satellite. Both instru- were recorded simultaneously by STEP-F and SphinX ments collected data on energetic charged particles during instruments during the recovery phase. An interesting the deep solar activity minimum in 2009. In 2018, we observation is that particle fluxes increased by 2–4 orders investigated the phenomena of Van Allen electron outer at both an altitude of ~ 550 km and at the level of the radiation belt splitting (Fig. 14) during geomagnetic geostationary GOES satellite orbit (Fig. 15).

Fig. 14. Van Allen outer radiation belt splitting as seen by the STEP-F instrument.

Fig. 15. Splitting of outer belt and increasing of particle fluxes at both an altitude of ~ 550 km by the SphinX/CORONAS-Photon measurements and at the level of the geostationary GOES satellite orbit.

(P. Podgórski, J. Sylwester, O.V. Dudnik)

46 Investigating the impact of cosmic X-rays and solar energetic particles on STIX The European Space Agency's Solar Orbiter satellite will be launched in 2020. Its mission is to observe the Sun. The STIX (Spectrometer/Telescope for Imaging X-rays) in- strument will be onboard, and will operate in a heliocentric orbit very close to the Sun (0.3 au). Such a close approach is expected to expose the instrument to Solar Energetic Particles (SEP) associated with solar flares. We therefore carried out a Monte Carlo simulation of the expected effect of background X-ray radiation from SEP and cosmic X- rays (CXB) on STIX's detectors.

Fig. 17. The response of the STIX instrument to SEP.

Fig. 16. The response of the STIX instrument to CXB. The left panel shows whole energy range; the right panel shows the energy range registered by the STIX instrument. The results are shown in Figures 16, 17 and 18. The first shows background CXB radiation. The Fig. 18. The response of the STIX instrument to SEP left panel presents the entire spectrum. As ener- protons. The left panel shows whole energy range; the gies above 150 keV will be not measured, we ex- right panel shows the energy range registered by the STIX panded the spectrum in the 0–200 keV energy instrument. range (right panel). This shows that the visible Background flux from SEP is a more important continuum falls slightly with increasing energy. issue. However, SEP arrive occasionally and the However, the number of counts is very low, and flux is variable over time. Figure 17 shows the therefore we do not expect CXB background simulated spectral response of the instrument radiation to have a major effect on measured solar illuminated with a stream of electrons based on spectra. maximum measurements from the Helios space-

47 craft. Detected counts are significant and strongly ring an SEP event. However, they produce much dependent on energy, with a peak around 100 keV. lower levels of background flux (see Figure 18). This indicates that an SEP event such as a solar As this is very often correlated with electron flux, flare could significantly distort measurements of it is not thought to play a significant role in data the solar spectrum. Protons are also present du- analysis. (J. Barylak) Estimating fluxes observed by STIX during periods of low solar activity In 2018, our work focused on estimating flux during pe- riods of low solar activity. The initial dataset consisted of observations recorded by the SphinX instrument during the last solar activity minimum. Our estimation focused on overlapping energy ranges (4–15 keV) that are expected to be observed by the STIX instrument during periods of low solar activity (Fig. 19). The results suggest that a single STIX detector will be able to register about 11 counts per second for B1 GOES class level emission. We then re- peated the process for higher activity – B4 class solar flare. In this case, the estimated output count rate increases to about 550 counts per second. Our results indicate that the Fig. 19. Expected STIX spectrum for low intensity solar STIX instrument will be able to provide efficient imaging flux (B1 GOES class) at 0.28 au from the Sun. of solar emissions even during periods of low-level activity. (M. Gryciuk, P. Podgórski) An image reconstruction algorithm for STIX In 2018, we continued development and testing of a STIX • (Very) good photometry: source brightness is image reconstruction method. This method is based on a restored with 2% accuracy using our algorithm. vector of count rates recorded by all of the instrument's sub- Other algorithms do not perform that well. pixel detectors. The algorithm is based on the Richardson- • The algorithm is stable, irrespective of source Lucy maximum likelihood method. As our initial results morphology, location and brightness. were promising, we addressed the problem of multi-source The main problem that remains to be addressed is structures and defined two, artificial source distributions. to optimise the code to speed up execution. Cur- Our initial results were compared with existing image rently, we are working with several European insti- reconstruction algorithms and can be summarized as tutes to develop a STIX data analysis software pa- follows: ckage. Our algorithm can be used as a reference • All simulated sources have been reconstructed for other methods implemented for STIX. It will by our algorithm. Comparable results were also help to significantly improve the Solar obtained for the vis-CLEAN method for typi- Orbiter's software, in preparation for its launch in cal flare morphologies. 2020. (M. Siarkowski, T. Mrozek) The SolpeX instrument The Bragg POLarimeter Figure 20 shows an example of a spectrum to be measured relative to the normal crystal surface. B-POL will record and highlights a number of strong emission lines. The ob- spectra not only for ongoing flares, but also for more active served spectral range is recorded for Bragg incidence angles regions. This will enable us to study thermal plasma pro- close to the Brewster angle; consequently, their reflected in- perties such as turbulence, directed motion, the differential tensities will depend on the degree of linear polarization emission measure distribution and the elemental com- and the respective orientation of the polarization vector position for argon and sulphur.

48 Fig. 20. a). The B-POL crystal detector geometry. C1 and C2 indicate the location of the crystal's edges, D1 and D2 indicate the detector. “p” is the projected distance from the lower edge of the crystal to the detector (20 mm). b). Spectrum recorded during one rotation of the detector. The Rotating Drum Spectrometer The Rotating Drum X-ray Spectrometer (RDS) will allow us to investigate very rapid changes in solar spectra, and enable the creation of an atlas of contiguous spectra in the entire soft X-ray ran- ge for various plasma temperatures. Figure 22 shows the instrument's confi- guration. Flat mono-crystals are attached to an octagonal drum rotating at a high rate or in slow rocking mode. The geome- try is such that, for most of the time, solar X-rays illuminate a pair of the rotating crystals. Bragg-reflected photons are recorded by two pairs of detectors and, over time, each detector records spectra at a slightly different Bragg angle. The res- pective incidence angles can easily be de- termined and converted to corresponding incoming photon wavelengths (or equi- valent energies) with a pin-hole soft X-ray imager-spectrophotometer (see below). Fig. 21. Expected spectra recorded by the four RDS detectors. The x-axis plots the rotation angle. The y-axis plots the log of the count rate per drum revolution. To improve statistical reliability for weaker events, count rates from many rotations are collected. Red lines correspond to expected background fluorescence; for most channels this level is below the “real” X-ray continuum.

49 Fig. 22. The RDS's main components. Eight flat crystals are fixed to the rotating or rocking drum. Bragg- reflected spectra are recorded by four detectors. During each full rotation, each of the eight crystals illuminates each of the four detectors over a short time interval.

The results of laboratory tests of the instrument's detectors are shown in Figure 23.

Fig. 23. Histograms of energy spectrum taken in laboratory conditions. The pin-hole soft X-ray imager-spectrophotometer The CMOS that will be used performs well, of the solar illumination profile and the provided that single X-ray photons strike the instrument's response function. Local variations pixel. This is the usual scenario; the exception will in the crystal's shape change the direction of X- be the most powerful flares, when double strikes ray diffraction. Our calculations were designed to are expected. An amplitude analysis will be used to evaluate the real response function, compared to a discriminate between solar X-ray photons and perfect crystal shape. This showed that shifted those due to secondary fluorescence or energetic column summation can be used instead of strictly particles. Specifically, a brightness profile can be selected columns just by compensating for wave- created for selected energies that are represen- length shifts caused by the imperfect crystal shape tative of individual spectral bands. The signal (Fig. 26). measured by X-ray spectrometers is a convolution

50 Fig. 24. a) The pin-hole: a cylindrical opening ? =0.7mm in lead foil 0.4mm thick. This diameter was selected to obtain sufficient statistics. The pin-hole is covered by a ~15 µm-thick thermal filter and the X-ray image is projected on the CMOS. At a pin-hole–CMOS distance of 578 mm, the projected diameter of the solar disc corresponds to ~215 detector pixels. b) Simulated solar images for four characteristic coronal observations projected on the pin-hole camera's CMOS. The imager can find the location of the solar limb (from the limb brightening ring), the position of the solar centre in the CMOS coordinate system, and determine the location, sizes and intensities of ARs, as well as positions of flares and their intensities.

Fig. 25. Histogram of the energy spectrum in laboratory conditions. X-rays are reflected from a multi-metal foil system consisting of titanium, iron, copper and molybdenum. The foil was illuminated by an X-ray lamp at 35 keV and the CMOS matrix was shielded from direct illumination coming from the lamp itself.

Fig. 26. Real wavelengths recorded by the spectrometer detector (continuous line). Wavelengths recorded by column with shifted pixels (dotted line). Wavelengths recorded by the perfect spectrometer (dashed line).

(J. Sylwester, M. Stęślicki, J. Bąkała, S. Płocieniak, A detailed description of our work on the SolpeX Ż. Szaforz, M. Kowaliński, D. Ścisłowski, instrument can be found in our article, 'The soft P. Podgórski, T. Mrozek, J. Barylak, A. Makowski, X-ray spectrometer polarimeter SolpeX', to be M. Siarkowski, Z. Kordylewski, B. Sylwester, published in Experimental Astronomy (https:// S. Kuzin, A. Kirichenko, A. Pertsov, S. Bogachev) doi.org/10.1007/s10686-018-09618-4) 2019. The SolpeX Team

51 Optimising ChemiX sured its spectrometric characteristics in the range The solar X-ray spectrophotometer ChemiX is part of the 482–1048 keV. Interhelioprobe interplanetary space mission. The instru- As a result of the laboratory measurements, we ment contains a Background Particle Monitor (BPM). found that scintillation detector manufactured BPM measurements of particle fluxes help to determine from lightweight organic scintillator and 57,600 the level of X-ray spectra contamination due to high-energy pixel's MPPC is capable to register the characte- interplanetary particles. Its detector head comprises an ristic linear X-ray emission and electron fluxes in a organic scintillator, which is built on a p-terphenyl single wide energy range from E = 32 keV up to E = crystal, optically coupled with a multi-pixel photon counter. 1048 keV provided that the temperature of the Although organic scintillators are lightweight, their light photodetector is constant. The largest technical outputs are usually moderate compared to inorganic light yield of such type scintillator is registered scintillators such as CsI(Tl) or NaI(Tl). We therefore exa- when the light splashes propagate along axis b of mined how to optimise technical light yields from these sample crystalline array. Taking into account small small, p-terphenyl single crystals. values of effective charge and density of this type of organic single crystal scintillator the proba- We measured the relation between technical light bility for registration of bremsstrahlung in space yield and the direction of the crystalline axis. The 3 is almost negligible, that allow us to detect, count sample's dimensions (6 mm ) are very close to the and register energy spectra of primary electrons, geometric parameters of the BPM's bottom anti- protons and other nucleons in the magnetosphere coincidence detector. Its sides were oriented using and interplanetary space with high efficiency. a laser beam in the red spectral region and we mea-

Fig. 27. Energetic spectra of β- particles and characteristic X-ray emissions from 137Cs and 207Bi.

(M. Kowaliński, O. Dudnik)

52 Heliospheric physics (Laboratory for solar system physics and astrophysics - LSSPA) The hypersonic, ionized solar wind carves out a cavity in the tes the solar wind and interstellar plasmas. While the inter- interstellar matter, called the heliosphere. The size of the stellar plasma is deflected and flows past the heliopause, the heliosphere is determined by a balance between the pres- neutral component of interstellar matter, mainly hydrogen sures of the solar wind and the interstellar gas, both of and helium, penetrates freely into the heliosphere, where it which are magnetized. The heliosphere is bounded by a con- can be directly observed. An artist's impression of the he- tact discontinuity layer called the heliopause, which separa- liosphere is shown in Figure 28.

Fig, 28. Artist's impression of the heliosphere and its nearest Galactic neighbourhood as it emerges based on the analysis of recent IBEX observations and several years of research carried out in the Laboratory for Solar System Physics and Astrophysics. The figure shows the Sun embedded in the local plasma. Subjected to the ram pressure of the cloud of interstellar matter composed of ionized ambient interstellar matter, the solar wind slows and neutral atoms and dust grains of various sizes. down through a shock wave—the solar wind This cloud is one of many similar clouds within termination shock—and eventually flows down- the Local Interstellar Medium—an astrophysical stream, forming a contact discontinuity surface object spanning approximately 200 pc across that called the heliopause, which separates the solar and is a remnant of a series of Supernova explosions interstellar plasmas, and an elongated heliotail that happened a few million years ago. The Sun (bottom-left corner of Figure 28). The helio- moves through the Local Interstellar Cloud from pause, impenetrable for charged particles except right to left in Figure 28, emitting the solar for cosmic rays, is transparent for neutral atoms, wind—an ever-evolving, omnidirectional, latitu- which thus freely enter the heliosphere. Inside the dinally-structured, hypersonic outflow of solar heliosphere, the interstellar atoms become the

53 seed population for energetic neutral atoms being products of this reaction also enter the (ENAs). ENAs are formed everywhere in the heliosphere and are detected as the so-called heliosphere due to the charge exchange reaction secondary population of neutral interstellar gas. Together between the ions from local plasma and the neu- with all the other populations of neutral atoms, tral interstellar atoms. Once created, they travel they provide an important means for analysing the without being ionized or absorbed at large distan- physical state of the distant regions that they ces, comparable to the size of the heliosphere. originated from. The charge exchange process operates both in the During recent years, a very important insight into supersonic solar wind and in the inner heliosheath the heliosphere, Local Interstellar Medium, and (centre-left in Figure 28), i.e., in the region processes responsible for the coupling of these between the termination shock and the helio- astrophysical objects was obtained based on ob- pause. Some of the ENAs created in these regions servations by the NASA space probe Interstellar freely escape from the heliosphere and, due to Boundary Explorer (IBEX). This mission was eventual collisions, slightly modify the inflowing developed and is being led by the Southwest interstellar gas. Others run in the opposite direc- Research Institute in San Antonio, Texas under tion and reach detectors located in the Earth's the NASA Small Explorers program. It is orbit (in Figure 28, schematically drawn close to managed by the Goddard Space Flight Center for the Sun). the NASA Science Mission Directorate in Neutral atoms from the interstellar matter (whose Washington, DC. The research facilitated by streamlines are marked by the short arrows in IBEX is carried out by the IBEX Science Team of Figure 28) typically have energies of between a researchers from the United States, Poland, few dozen and about 150 eV. Due to interaction Switzerland, Germany, and Russia. The Centrum between the heliosphere and the interstellar Badań Kosmicznych PAN has participated in the medium, a disturbed region called the outer IBEX effort since the planning phase, at the Co- heliosheath (the green haze in the figure) is formed Investigator level. in front of the heliosphere. In this region, the During 2018, scientists from Laboratory for Solar flows of interstellar plasma and interstellar neutral System Physics and Astrophysics (LSSPA) carried gas decouple from each other. This leads to the out studies of various aspects of the heliosphere formation of another population of neutral and the surrounding interstellar medium. All rese- atoms through charge exchange reactions arch results obtained in 2018 by LSSPA scientists between ions from the perturbed plasma flow past were published in sixteen scientific papers in the heliopause and the hardly perturbed international, peer-reviewed scientific journals. interstellar neutral atoms. Some of the atoms Some of these results are presented below. The heliosphere is not round! The solar wind expansion stops at a certain distance to the The laws of physics suggest that the shape of the Sun. This happens in the locations where the solar wind heliosphere depends on the speed of the Sun's pressure becomes equal to the pressure of the interstellar motion through the interstellar gas, the density of matter. The solar wind matter cannot accumulate infinitely this cloud, the intensity and direction of the inside the heliosphere and must find an exit path to the interstellar magnetic field, as well as the spatial interstellar space. But where exactly is this path located? distribution of the total pressure of the solar And is there just one evacuation path or more? These wind. The key factor is the pressure balance bet- questions cannot be answered directly because up to now ween the solar wind and interstellar matter. The there have been just two active space probes – Voyager 1 interstellar magnetic field exerts a certain stress and 2 – to reach the boundary regions of the heliosphere, force on the heliosphere, which can be conven- and this happened in the regions least suspect of being iently represented as an additional pressure term anywhere close to the solar wind evacuation path. Therefore, known as the magnetic pressure. The magnitude the question of solar wind exhaust location can only be of this pressure is proportional to the square of answered by means of remote-sensing measurements and the strength of the component of the magnetic theoretical modelling. field vector perpendicular to the heliopause.

54 The ram pressure of the ionized component of ENAs must be very similar for all directions. Con- interstellar matter is proportional to the total den- sequently, the heliosphere must be approximately sity of the interstellar plasma and to the square of round and, if so, then it must be shaped by a Sun's speed relative to the surrounding interstellar strong interstellar magnetic field. plasma. If the interstellar magnetic field is so This hypothesis is at odds with previous views on strong that the magnetic pressure is much larger the shape of the heliosphere because the strength than the ram pressure of the interstellar plasma, of the interstellar magnetic field, the plasma den- then the heliosphere is expected to be approxi- sity, and the speed of Sun's motion through the mately spherical in shape, and the solar wind is Local Interstellar Medium have been measured evacuated via two channels parallel to the direc- with a sufficiently good accuracy and suggest that tion of the local interstellar magnetic field. If, ho- interstellar magnetic pressure is lower than the wever, the ram pressure is much larger than the plasma ram pressure. However, the INCA obser- magnetic pressure, then the heliosphere will take vations used by the aforementioned team of an elongated, comet-like shape (somewhat disto- scientists are an enigma that must not be ignored. rted from axial symmetry by the magnetic pressu- Professor Nathan Schwadron from the University re), and the solar wind will be evacuated via one of New Hampshire and Professor Maciej Bzow- channel directed 'back-wards', i.e., along a long tail ski from the LSSPA suggested that the INCA pointing approximately opposite to the Sun's observations can be understood based on the con- motion. An extensive study on the shape of the ventional, comet-like paradigm of the heliosphe- heliosphere for various combinations of the ram re. In a paper published in The Astrophysical Journal and magnetic pressures was published in 2018 by (http://iopscience.iop.org/ article/10.3847/15 two scientists from LSSPA team: Professor An- 38-4357/aacbcf) they suggested some reasons for drzej Czechowski and Jolanta Grygorczuk Msc. the correlation between observed fluctuations of Based on available extensive insights from INCA ENAs, fluctuations of the charged parti- experimental and modelling studies using various cles observed by Voyager, and the phase of solar measurement techniques, it had been concluded activity. that most likely, the interstellar dynamic pressure Schwadron and Bzowski pointed out that the is much larger than the magnetic pressure, and ENA fluctuations are related to the ENA produ- consequently the heliosphere has a comet-like ction rate, which is strongly dependent on fluctu- form. However, in 2017, a team of US scientists ations in the temperature and density of the solar published a hypothesis that the heliosphere is wind plasma penetrating the solar wind termi- round in shape (in Nature Astronomy). They consi- nation shock. This is a quasi-stationary shock dered measurements of the flux of energetic neu- wave structure that separates the hypersonic and tral atoms (ENAs) with energies of several dozen subsonic regimes of the solar wind outflow. When keV (an order of magnitude larger than typical a portion of plasma with an increased density and energies of solar wind protons), performed by the speed crosses the termination shock, the plasma INCA instrument onboard the Cassini space just downstream of the termination shock is hea- probe. They found that: (1) variations in time of ted and, before cooling, for some time propagates the flux are unexpectedly rapid; (2) they are with the plasma flow in the inner heliosheath. The strongly correlated with each other, with the temperature of such plasma flow is much larger phase of the 11-year cycle of solar activity, and than that of the shock-processed 'regular' solar with time variations of in situ point measurements wind plasma. Therefore, the charge exchange rate of energetic ions in the outer heliosheath (the between protons in the heated plasma and the parent population for ENAs observed by INCA); ambient interstellar neutral H atoms increases and (3) the fluxes of these ENAs from the upwind rapidly and, consequently, an enhanced flux of and downwind sides of the heliosphere have ENAs is produced for a certain time before the similar magnitudes, and their variations are heat dissipates. Since the occurrence of fast and correlated in time. On this basis, the team of US dense gusts of the solar wind increases during researchers concluded that the distances to, and high solar activity and, on the one hand, the dimensions of, the source region of these thesegusts have a global range and, on the other

55 hand, the difference in arrival times between and the ENA fluxes from the heliosheath, measu- various locations along the shock is relatively red (with a well-understood time delay) by INCA. small (a few months) a strong spatial correlation Consequently, the seemingly strange observations eventually appears between time fluctuations of reported by the team of US researchers can be the ENA flux from various regions of the ter- explained on the basis of the conventional mination shock, and a time correlation between heliospheric paradigm and the heliosphere, which, the charged energetic particles processed by the as the title of Schwadron and Bzowski's paper termination shock, measured by the Voyagers, claims, is not round!

Conclusions from ENA observations from the HSTOF: The heliosphere has a tail and is asymmetrical Since the speed and direction of motion of heliospheric by INCA and IBEX. The correlation of the ENA ENAs reflect the speed and direction of motion of their flux with the solar wind flux supports the hypo- parent ions, ENA observations offer a good insight into the thesis that observed ENAs originate from the energy distribution of cosmic plasma located far away from aforementioned charge exchange reactions bet- the observation site. ween protons from the shocked solar wind plasma The High energy Suprathermal Time Of Flight and interstellar hydrogen atoms in the boundary sensor (HSTOF) instrument onboard the Solar regions of the heliosphere. and Heliospheric Observatory (SOHO) space Furthermore, these observations corroborate the probe has been carrying out ENA observations hypothesis that the heliosphere's axial symmetry is since 1996. The instrument is sensitive to ENAs distorted due to the action of the interstellar ma- with energies from 55 to 88 kiloelectronvolts gnetic field. This is because the observed ENA (keV), i.e., to atoms traveling at 3250 to 4100 flux in the “starboard flank” (ecliptic longitudes km/s. Other instruments observing ENAs (in from 120° to 210°) is larger than the flux from the different energy bands) include INCA, onboard “portside flank” (ecliptic longitudes from 300° to the Cassini Saturn probe (observations between 30°). The observed asymmetry is in agreement 2005–2013), the ASPERA instruments onboard with recent estimates of the direction of interstel- the planetary probes Mars Express and Venus lar magnetic field. Express (also presently inactive), and the IBEX Finally, HSTOF observations lend strong support satellite (carrying out observations from 2009 to the existence of the heliospheric tail: the flux until present). observed from the upwind region of the helio- The implications of HSTOF observations carried sphere, i.e., from the direction of Sun's motion out from 1996 to 2010 were studied by a team of through the local interstellar matter, is much lower scientists from LSSPA: Professors Andrzej than the flux from the opposite direction. This Czechowski, Maciej Bzowski, and Stanisław behavior is expected if the heliosphere has a long Grzędzielski, Dr Justyna M. Sokół and Jolanta tail. The upwind to downwind ratio of the ENA Grygorczuk MSc., in collaboration with Professor fluxes observed by HSTOF differs from the ratios K.C. Hsieh from the University of Alabama, who observed by INCA and IBEX. Researchers from formulated the concept of the HSTOF experi- the demonstrated that this difference is a natural ment and Dr M. Hilchenbach from the Max- consequence of the larger energies observed by Planck-Institut für Sonnensystemforschung in IBEX: 55 to 88 keV in comparison with 5 to 55 Göttingen, Germany, who processed the data. keV observed by INCA and 0.7 to 4.3 keV obser- The researchers found a clear downward trend in ved by IBEX, and the resultant difference in reac- observed ENA intensities, which seems to be tion cross sections. This result is another confir- correlated with the secular systematic decrease in mation that “The heliosphere is not round!”. the solar wind flux observed in situ at the Earth's In addition to the data from the HSTOF, the rese- orbit, but not with periodic variation in the solar arch team used results of earlier determinations wind related to the solar activity cycle. A similar of the densities of interstellar hydrogen and downward trend in ENA observations was found helium at the termination shock of the solar wind,

56 based on data from the Voyager and Ulysses spa- The results and conclusions were presented by the cecraft, with an important contribution from team led by Professor A. Czechowski in a paper scientists from LSSPA as well as the Warsaw Test published in Astronomy & Astrophysics (https:// Particle Model of the density distribution of www.aanda.org/articles/aa/abs/2018/10/aa324 interstellar H and He in the heliosphere developed 32-17/aa32432-17.html). in LSSPA, and the Warsaw MHD model of the heliosphere. Interstellar neutral helium atoms observed in three IBEX-Lo energy channels Interstellar neutral atoms of helium from the Local Inter-stellar Medium are observed by the Interstellar Boundary Explorer (IBEX) spacecraft in the Earth orbit. Researchers from LSSPA, Dr Paweł Swaczyna, Professor M. Bzowski, Marzena A. Kubiak MSc, Dr Justyna M. Sokół, and their international collaborators analysed these observations to determine the Sun's motion with respect to the Local Interstellar Medium and the temperature of this medium. From a broader perspective, the results of these analyses provide an important insight into how the heliosphere interacts with its surroundings. In a paper published in The Astrophysical Journal (https://doi.org/10. 3847/1538-4357/aaabbf), they analysed data from two energy channels of the IBEX- Lo detector previously not used, in addition to the data from the channel previously used, and obtained a better assessment of these quantities.

Fig. 29. Sky maps of counting rates of interstellar neutral atoms observed by IBEX in the analysed energy channels. The maps are centered at the direction of the Sun's motion with respect to the interstellar medium. Atoms are deflected by the Sun's gravity and thus observed predominantly away from this direction. Differences between observed counting rates in these energy channels are caused by the contribution of hydrogen atoms (not considered in this analysis) and the different energy-dependent sensitivities of the IBEX-Lo detector in these channels.

The structure of the interstellar medium at scales the absorption lines towards the closest stars show of tens and hundreds of parsecs around the Sun is that the Sun is located either in one of two clouds not homogeneous. The Sun is within a system of known as the Local Interstellar Cloud and G multiple, partially-ionized, warm (5000–8000 K) Cloud, or - more likely - in a boundary region and dense (~0.2 cm-3) clouds, embedded in a very between them. However, the ultimate determina- hot (~106 K), completely ionized and rarefied tion is not possible from telescopic observations. (~0.005 cm-3) region. Telescopic observations of The results of the IBEX mission may make it

57 possible to resolve this enigma and answer the the IBEX-Lo detector in which interstellar neutral question of how conditions in the interstellar helium is visible, and abandoned the assumption medium along the Sun's path will change during of uniform energy sensitivity. The analysis aimed forthcoming millennia. to determine the temperature and velocity vector Previously, only data from one of the energy of interstellar neutral helium simultaneously with channels of the IBEX-Lo detector had been used the determination of the velocity-dependent in the analysis of the local interstellar gas. This sensitivity. Researchers found that the previously- was due to limited knowledge of the sensitivity of obtained parameters of the interstellar medium the detector to incoming atoms with various did not need revision. This is important because velocities (i.e., with various kinetic energies). As a this analysis lends more credence to earlier analy- first approximation, the energy channel that had ses of interstellar neutral gas and its secondary been used in previous analyses was assumed to component, the so-called Warm Breeze, and to have a sensitivity independent of the atom energy. conclusions stemming from these analyses con- In this study, scientists from LSSPA analysed cerning the orientation of the interstellar magne- observations from the three energy channels of tic field. Evolution of the solar Lyman-α profile line and radiation pressure for interstellar hydrogen

Fig, 30. Schematic illustration of building-blocks of the model of the profile of the solar Lyman-α spectral line. The blue line represents the main Gaussian-like shape, the red line the central self-reversal, and the green line the spectral background of the line. The actual profile is a superposition of these building-blocks; it is represented by the black line.

The Lyman-α line is one of the most prominent features in Previous models of the Lyman-α line profile were the UV part of the solar spectrum. It is responsible for the based on just a few observations, and therefore resonance radiation pressure acting on hydrogen atoms in they were not able to reproduce the evolution the heliosphere, i.e., for an effective anti-solar force that is related to variations in solar activity with sufficient exerted on these atoms by photons from the Sun. Next to accuracy. A team of scientists from LSSPA: Dr the solar gravity force, radiation pressure is the main factor Izabela Kowalska-Leszczyńska, Professor Maciej that determines the trajectories of neutral hydrogen and Bzowski, Marzena A. Kubiak MSc, and Dr Justyna deuterium atoms inside the heliosphere. Accurate know- M. Sokół developed a new model of the evolution ledge of the dynamics of these atoms is necessary to calcu- of the solar Lyman-α line profile based on new late the density of interstellar neutral hydrogen inside the observations from the SOHO satellite that have heliosphere and, consequently, to investigate derivative po- been available since 2015. Based on these observa- pulations of H atoms important for heliospheric physics, tions, the researchers proposed an analytical including pickup ions and energetic neutral atoms. To that formula composed of three parts. Each describes end, one needs a model of the spectral shape of the solar a different feature of the line profile, shown in Lyman-α line and its evolution during the cycle of solar Figure 30 (the main line – blue line, the self- activity. reversal in the centre – red line, and a slight slope

58 of the whole line with respect to the vertical axis – green line). It turned out that by using the propo- sed formula, the team could reproduce solar line profile observations collected over several years (covering almost a full cycle of solar activity) with very good accuracy. An example is shown in Figure 31, where two observed profiles (dots) are compared with fitted functions (lines). Further- more, the team of researchers found that the pa- rameters of the proposed function (e.g., the wid- ths of component functions, the depth of the self-reversal, and the shifts of the profile compo- nent relative to each other) can be expressed as li- near functions of total solar irradiance in the Lyman-α line. The evolution of the latter quantity is closely related to the level of solar activity. The results of this analysis were presented in a paper published in The Astrophysical Journal (http:// io- pscience.iop.org/article/10.3847/1538-4357/ aa9f2a). Subsequently, the team from LSSPA examined Fig. 31. Example solar Lyman-α line profiles obtained how the new radiation pressure model affects the from the newly-developed model for the solar maximum (orange) and solar minimum epochs (purple). The bottom interstellar neutral hydrogen distribution in the panel presents relative differences between model heliosphere, and distributions of its derivative predictions and actually-measured profiles. populations of particles. The analysis started with a comparison of the densities of interstellar scientists from the USA and Russia discovered hydrogen inside the heliosphere predicted by the that the ratios of fluxes of hydrogen atoms obser- old and new models. It turned out that during ved by IBEX-Lo in different energy channels are periods of low solar activity the new model pre- inconsistent with models. They had suggested dicts more hydrogen close to Earth's orbit than that the reason for this may be an insufficient the old one, but during high solar activity, the new understanding of the radiation pressure acting on model predicts less gas. The largest differences hydrogen atoms in the heliosphere. Simulations between the two considered models are in a performed by scientists from LSSPA showed that region located opposite to the direction of inflow indeed, expected fluxes of hydrogen atoms are of the interstellar gas to the heliosphere, i.e., in the very sensitive to details in the radiation pressure downwind region. model, but even using the newly-developed model does not remove the observed discrepancy. Another aspect considered by the research team was the value of the density of interstellar neutral Therefore, researchers from LSSPA challenged hydrogen at the termination shock. In 2008, the existing paradigm regarding how the radiation scientists from the carried out estimates using the pressure in the heliosphere actually works. It had old model of radiation pressure and the flux of been assumed that if the flux of photons from the pickup ions observed by the Ulysses mission. The Sun decreases with the square of solar distance, new value of hydrogen density calculated using then the force due to the radiation pressure the new model of radiation pressure turned out to should behave in the same way. This is because the be statistically consistent with the old one due to gravity force also decreases with the square of the large measurement uncertainty, which was solar distance. Consequently, the ratio of the 25% of the measured value. gravity and radiation pressure forces acting on hydrogen atoms should be constant, regardless of Another question was the influence of the new ra- where it is measured. But is that assumption true, diation pressure model on the hydrogen atom flux if some of the solar photons are scattered by seen by the IBEX-Lo detector. Several years ago, hydrogen atoms? Scientists from LSSPA calcula-

59 ted how many of the original photons emitted by The modification of the radiation pressure force the Sun are scattered from the beam of hydrogen due to the absorption effect is larger than the dif- atoms located between the Sun and a given loca- ferences between the two radiation pressure mo- tion in the heliosphere. They found that even at dels. Therefore, a new radiation pressure model in relatively small distances (within approximately 10 the heliosphere is needed, which should take ab- astronomical units – around Saturn's orbit) scatte- sorption processes into account. However, this ring losses can reach 30% of the original Lyman-α new model must also include the distribution of photons emitted by the Sun within the spectral interstellar neutral hydrogen in the heliosphere as sensitivity band of hydrogen. Thus, the force the two phenomena are closely related to each caused by radiation pressure decreases much other. faster with distance than previously thought.

Fig. 32. Evolution of effective radiation pressure (expressed in units of solar gravity force) acting on hydrogen atoms in the heliosphere with distance from the Sun. Absorption of solar photons that are responsible for radiation pressure results in a gradual decrease of the effective spectral flux from the Sun in the frequency range corresponding (due to the Doppler effect) to radial velocities of interstellar neutral atoms in the heliosphere. As a result, the magnitude of radiation pressure effective for interstellar hydrogen atoms is closely related to the column density of interstellar hydrogen between a given location in space and the Sun. Hence, the approximation in which radiation pressure is just a factor that is scaled with the square of the distance to the Sun (represented by black profiles) is unlikely to be valid. The four panels present the evolution of spectral profiles of the solar Lyman-α line along upwind, downwind, crosswind and north-pole lines in the heliosphere at selected distances from the Sun. The results of this analysis were presented by the team lead by Dr Izabela Kowalska-Leszczyńska in a paper published The Astrophysical Journal (http://iopscience.iop.org/article/10.3847/1538-4357/ aae70b).

60 Magnetic waves excited by newborn interstellar pickup ions measured by the Voyager spacecraft up to Pluto's orbit New ions in the solar wind are created by ionization of astronomical units from the Sun. They were de- interstellar atoms that penetrate inside the heliosphere. tected by instruments on the ACE (at 1 au) and They are called pickup ions because immediately after Ulysses missions (from 1 to 5 au). Very important creation they are “picked up” by the Lorentz force from the data were gathered by the Voyager spacecraft be- magnetic field “frozen” in the solar wind and advected with tween 1 and 45 au. A team of researchers from the the solar wind into the interplanetary space. Pickup ions University of New Hampshire studied magnetic gyrate in the magnetic field, producing characteristic magne- field data from Voyager 1 and Voyager 2 missions tic waves. These waves can be detected via careful analysis collected in the period from 1997 to 1990, and of time series of the intensity and direction of the magnetic identified more than 600 events associated with field, observed by the interplanetary probes. magnetic waves excited by newly-born interstellar pickup ions, both helium and hydrogen. Magnetic waves produced by ion pickup have Scientists from LSSPA (Dr Justyna M. Sokół, characteristic signatures in observed time series Professor Maciej Bzowski, and Marzena A. of interplanetary magnetic field, and are different Kubiak MSc) studied pickup ion production rates for each of the pickup ion species. However, these for interstellar hydrogen and helium using the signatures can be detected only when the growth Warsaw Test Particle Model simulation code, rate of the wave is greater than the turbulence models of the solar wind evolution in time and level of the solar wind. Searching for wave- heliographic latitude, and solar wind extreme growth events is challenging, but very important, ultraviolet ionizing radiation. These research because it enables models of the distribution of tools, developed by the team from LSSPA, were neutral gas in the heliosphere, and the pickup ion employed to calculate the distribution of inter- creation processes in the solar wind magnetic field stellar neutral hydrogen and helium gas inside the to be verified. The growth rate of magnetic waves heliosphere and production rates for pickup ions depends, among other things, on the production along Voyager 1 & 2 trajectories. The results of rate of pickup ions. This rate is directly pro- these studies were applied by the team at the portional to the density of the interstellar neutral University of New Hampshire in their research on gas in the interplanetary space, and ionization magnetic wave creation. The study showed that rates, which vary both temporally and spatially magnetic waves due to pickup ions can be excited with heliographic latitude. The spatial distribution as far from the Sun as Pluto's orbit and beyond, of interstellar neutral hydrogen and helium i.e., up to 45 au from the Sun. Both teams of rese- densities, and the rates of their ionization are archers found good agreement between the mo- totally different and, consequently, the resulting del's predictions and observed rates of magnetic pickup ion production rates are significantly waves due to pickup ion creation. different. For solar distances smaller than three astronomical units, the production rate for helium The results of the study were published in a series pickup ions is much greater than that for hydro- of three articles by Hollick et al. in The Astro- gen ions. Consequently, we can expect to find physical Journal and The Astrophysical Journal more magnetic wave events characteristic of the Supplement. The articles are available at: http:// creation of helium than hydrogen pickup ions. iopscience.iop.org/article/10.3847/1538-4357/ Beyond 3 au, more hydrogen pickup ions are aac83b, produced. http://iopscience.iop.org/article/10.3847/1538- 4357/aac839, Magnetic waves excited by newborn interstellar http://iopscience.iop.org/article/10.3847/1538- pickup ions are observed within the supersonic 4365/aac83a. solar wind from a few tenths to several dozens of

61 A corridor to the Sun for select nanodust particles The smallest dust grains in the circumsolar dust cloud are its speed may be comparable to that of the solar nanodust particles, i.e., dust grains with sizes of a few, to a wind, but in the opposite direction. Therefore, it is few ten millionth parts of a millimeter. They are so small expected that the orbital dynamics of these they only include a few dozens of thousands of atoms. Like nanodust particles are different to those of colli- all dust grains in the Solar System, they are electrically sional nanodust grains. This topic was investi- charged, and their high charge to mass ratio makes the gated by Professor Andrzej Czechowski from Lorentz force from the magnetic field in the solar wind LSSPA and Professor Ingrid Mann from the similar in strength to the solar gravity force, or even larger. Arctic University of Norway in Tromsø, Norway, Therefore, the motion of nanodust grains significantly dif- who created a particle motion model. fers from the motion of typical dust grains, which resembles Based on numerical simulations of the forces ac- the motion of asteroids. ting on nanodust particles, Czechowski and Mann Nanodust is predominantly produced by colli- concluded that unlike “regular” nanodust parti- sional fragmentation of larger dust particles. Ini- cles, particles from sungrazing comets cannot be tial velocities of particles produced by this mecha- trapped close to the Sun, even those released very nism are close to the orbital velocities of their close to the Sun. Therefore, sungrazing comets parent dust grains. The newly-created dust grains are unlikely to be an additional source of the quickly become electrically charged, are picked up trapped nanodust population. However, the two by the solar magnetic field, frozen in the solar researchers identified an interesting phe- wind, accelerated to velocities comparable to that nomenon that they called a “corridor to the Sun”. of solar wind, and move away from the Sun. Ho- Some nanodust grains, released in the inbound leg wever, particles that are created sufficiently close of the comet orbit, can enter peculiar trajectories to the Sun become “trapped” in bound orbits leading them deep into the solar corona, i.e., the around it, due to an interplay between solar gra- upper, hot part of the solar atmosphere, visible vity and magnetic forces. Therefore, it is likely that from Earth during solar eclipses. Due to electro- a population of trapped nanodust particles is magnetic forces, these grains approach the Sun at present in the vicinity of the Sun. a distance much closer than the perihelion of the Another hypothetical source of nanodust is co- parent comet, which may lead to destruction of mets and, in particular, sungrazing comets. Such nanodust grains by sublimation or collisions with comets have perihelia deep inside Mercury's orbit ions. Most nanodust grains are, however, picked and aphelia somewhere between the orbits of up by the solar wind and ultimately escape the Sun. Mars and Jupiter. The initial velocities of nano- The results of this study were presented in a paper dust particles released by these comets shortly published by Czechowski & Mann in Astronomy & before perihelion are much larger than those of Astrophysics, available at https://www.aanda.org/ collisional nanodust particles. If the release of a articles/aa/abs/2018/09/aa32922-18/aa32922- nanodust particle occurs inside the Mercury orbit, 18.html. Exact solutions and singularities of an X-point collapse in Hall magnetohydrodynamics Magnetic reconnection is a topological rearrange- most fundamental questions have remained ment of the global magnetic field. It is believed to poorly understood, and magnetic reconnection be responsible for fast conversions of magnetic continues to be one of the most challenging pro- field energy into other energy forms, like kinetic blems in plasma physics. energy of the plasma flow, as well as thermal and One of the many challenging aspects of magnetic radiation energies. Despite multiple, decades-long reconnection is the question of its onset. Long attempts to fully understand how some basic ago, Dungey argued that neutral X-points in the concepts can explain the overall picture of plasma magnetic field are unstable and collapse into thin, dynamics in various environments, like the solar elongated regions of significantly-increased resis- corona, the Earth's magnetosphere, relativistic tivity, called current sheets. In principle, the for- astrophysical plasmas, or tokamak physics, the mation of current sheets requires a kinetic descri-

62 ption of the process. Nonetheless, an acceptable superalfvenic plasma flow. An exact formula, ba- understanding has been obtained using an appro- sed on initial conditions at the time when singula- priate magnetohydrodynamical approach. Vario- rities form, was found. These results were publis- us plasma fluid approximations have facilitated hed in a paper by Janda in the Journal of Mathemati- our understanding of the specific physical pheno- cal Physics (https://doi.org/10.1063/ 1.5026876). mena involved in the formation of current sheets. Exact solutions within Hall MHD are very rare. One of them is Hall magnetohydrodynamics The solution obtained by Artur Janda seems to be (MHD), which is a monofluid approximation of a the only one in the literature that is singular. It is two-fluid description of plasmas that is much very important to identify its physical meaning. more detailed than more frequently-exploited Although self-similarity has to break down at a ideal or resistive magnetohydrodynamics. In Hall certain point, shock waves accompanying the magnetohydrodynamics, unlike classical magne- current sheet are expected to appear. Moreover, tohydrodynamics, resistivity is non-zero; the ma- intuitively, from the physical point of view, the gnetic field becomes fro-zen in the electron fluid, emerging resistivity is unlikely to be homo- rather than the bulk plasma flow, and dispersive geneous, and it can be expected that the recon- whistler waves appear due to the Hall effect. Such nection rate will explosively increase. This picture a theory is useful in the solar corona as well as in seems to be complementary to the well-known the Earth's magnetosphere. secondary tearing instability of elongated current To reduce the complexity of the global dynamics sheets, the so-called plasmoid instability that leads of magnetic collapse, Artur Janda MSc from to the acceleration of magnetic reconnection. LSSPA hypothesised a specific, self-similar stru- The exact solutions found by Artur Janda are a cture for the magnetic field and incompressible convenient tool to derive appropriate initial plasma flow. Having reduced the Hall MHD conditions, leading generically to the formation of equations for the case of an X-point collapse, and singularities, which in general is a challenging using an appropriate ansatz, he obtained a mathematical task. Another interesting task would definition of a dynamic system that could be be to extend this class of solutions to nonlinear solved in terms of elliptic functions. He found magnetosonic waves forming singularities. Such that there are two possible classes of solutions. solutions would clarify the outstanding problem One consists of periodic regular solutions, and of the heating of the solar corona. the other includes singular solutions. Surprisingly, (M. Bzowski, A. Czechowski, A. Janda, it turned out that singular solutions are more I. Kowalska-Leszczyńska, J. M. Sokół, P. Swaczyna) physically relevant, because regular ones exhibit a

Ionospheric and magnetospheric group (Plasma Physics Group) Swarm The Swarm consists of three, identical satellites (A, B and C) that were launched on 22 November 2013 into a near-polar orbit. Satellites A and C fly side-by-side and form a lower pair (1.4° longitude separation) at an altitude of about 470 km and an inclination angle equal to 87.30°. Satellite B has a higher orbit, about 520 km, and an inclination

Fig. 33. Configuration of three satellites a Swarm mission (courtesy of the European Space Agency).

63 angle equal to 87.75°. All three satellites are and areas of seismic activity, the analysis exami- equipped with a set of six, identical instruments. ned a concentration of thunderstorms over Afri- We used data from a vector field magnetometer to ca (Figures 34 and 35) and an area that had exper- study magnetic field variations and a Langmuir ienced a strong earthquake (Figures 36 and 37). probe (an electric field measurement instrument) Figure 35 shows dynamic spectra of the magnetic to study electron concentration and temperature. field and electron density variations on 26 March The magnetometers installed on-board the Swa- 2016. These data were recorded during flight over rm measure the main magnetic field at a sampling the centre of a thunderstorm in Africa. Diamonds rate of 50Hz. As the goal of the study was to com- indicate key moments. pare ionospheric disturbance over thunderstorms

Fig. 34. Location of lightning associated with a thunderstorm over Africa on 26 March, 2016.

Fig. 35. Dynamic spectrograms (δB: top panel, δNe: bottom panel) for selected passes of Swarm A over the centre of an active African thunderstorm.

64 Figure 36 shows dynamic spectra of magnetic field variations over an earthquake area. The ma- gnitude 7.9 epicentre is located at 56.03N, 149. 03W, at a depth 30km below the ocean floor. The main quake was registered on 23 January 2018, 09:31:44UT. The left and centre images in Figure 4 show recordings from two days before earth- quake, while right-hand image is from three days before the event. The yellow star indicates the clo- sest approach of the satellite to the epicentre. The analysis shows that the effects are seen not exactly over the epicentre, but are shifted by a few tens of kilometres. This suggests a mechanism on gravity waves. The spectra of magnetic field varia- tion over thunderstorms and earthquakes are very similar, which makes distinguishing them pretty much impossible.

Fig. 36. Spectra of magnetic field variations and electron density registered by Swarms A (left) and C (centre) two days before earthquake, and Swarm B (right) three days before the earthquake.

(J. Błęcki, J. Słomiński, R. Wronowski, E. Słomińska, R. Haagm)

Analysis of Auroral Kilometric Radiation bursts In 2018, working in the frame of a SOC concept, Lefeuvre, M. Parrot) experiments, in the frame- we concluded analysis of the Auroral Kilometric work of the Interball-2 mission. Our preliminary Radiation (AKR) bursts occurrence as a function results were reported in our paper "Is The Akr Cy- of their intensity. We used data collected by the clotron Maser Instability A Self–Organized Criti- Polish POLRAD and the French MEMO (F. cality System?" and presented at the 8th Interna-

Fig. 37. Normalized single AKR bursts growth rates estimated via the self- organized criticality (SOC) logistic growth model from the MEMO AKR waveforms.

65 tional Workshop on Planetary, Solar and Helio- bandwidth. MEMO data are very scarce, but we spheric Radio Emissions in Graz, Austria and has were still able to show, that the characteristics of been published in the Proceedings of the con- single AKR bursts determined from the logistic ference. Self-organized criticality is a rather gene- growth model agree well with the Electron Cy- ral concept and we initially decided to fit the AKR clotron Maser mechanism producing AKR, in bursts data to a simple analytical model, the particular, with expected growth rates for the logistic–growth model (Aschwanden, [2011]). We AKR bursts. Our result is a strong argument in used AKR waveform data from the MEMO expe- favor of the AKR as a SOC system. riment. We determined both shapes and durations (M. Marek and R. Schreiber) of single AKR bursts filtered within a 4 kHz Lofar scintillation measurements As a part of the Low Frequency Array (LOFAR) which influences, for example, low frequency network, the Polish station PL610 in Borówiec radioastronomy and radio communication. provides observational data useful for studying Data used in this research come from the sixth distant radio sources in the frequency range 10– cycle of LOFAR core observations the 6th obser- 270 MHz. These data can also be used to investi- ving cycle. Data presents measured amplitudes in gate weak scintillation regimes commonly found resolution of about 10Hz in a 100 frequency in the mid-latitude ionosphere. Strong radio sour- subbands between 75.97 and 21.87 MHz, 38 ces (such as Cassiopea A and Cygnus A) and bri- stations (core and remote station) has been con- ght quasars have been observed in the local mode sidered. We used three datasets: L547449, L547 of the station to study ionospheric and interpla- 785 and L552177 (respectively quiet, disturbed netary scintillations. As an electromagnetic wave and stormy conditions). In each case, the source propagates through a medium where electron de- of observations was CasA, as it has the best cross- nsity fluctuations are present, variations in the re- correlation function. We have transform the spa- fractive index occur. Since observations carried tial coordinates so that all the stations (antennas) out in low frequency range are more sensitive to are placed on the same surface. Further we have ionospheric disturbances than those recorded in selected subband 70 (out of 100). For this data higher frequency ranges, they can provide infor- cross-correlation function has been calculated. mation on the irregular structure of this layer,

Fig. 38. Top row: amplitude time series; Bottom row: amplitude power spectrum density. Left column: quiet conditions (set L547449); Centre column: disturbed conditions (set L547785); Right column: stormy conditions (set L552177) Special thanks to Richard Fallows for providing LOFAR core data.

66 Each column of Figure 38 shows in upper panel amplitude time series and on bottom panel its (1) power spectral density (PSD) for three considered cases. One can see that with increasing distur- Above formula gives time lag for maximum of bance level amplitude scintillates stronger and temporal correlation between two stations PSD broadens. Having established by correlation separated by vector ξ. The quantity Q is the matrix analysis that the studied amplitude of LOFAR of quadratic form which describes anisotropy of interferometry agrees well with the picture of the random field (and can be estimated – see [3]) ionosphere modifying interstellar radioemission and v is the drift velocity. One can see that the τ we can try to estimate drift velocity of diffraction max is linear function of separation and depends pattern observed on the ground. We used the me- both on drift velocity and geometry of irregu- thod of relating characteristic features on auto- larities. and cross-correlation function described in va- riety of papers [4, 5].

Fig. 39. Left: top - correlation function evaluated at available positions for null time lag, bottom - time lag for the maximum correlation evaluated at available positions (as above) for quiet conditions (set L547449); center: correlation function evaluated at available positions for null time lag, bottom - time lag for the maximum correlation evaluated at available positions (as above) for disturbed conditions (set L547785); left: correlation function evaluated at available positions for null time lag, bottom - time lag for the maximum correlation evaluated at available positions (as above) for stormy conditions (set L552177).

In Figure 39 (similarly to Figure 38) correlation 7449 and L547785) the correlation function is ani- function evaluated at available positions for null sotropic while for stormy conditions (set L55 time lag in top panel and in bottom panel time lag 2177) it tends to isotropy. On the other hand, time for the maximum correlation evaluated at avai- lag for the maximum correlation behaves accor- lable positions (as above) is shown for each data- dingly to Equation 1 linearly what confirms hypo- set. For weak and moderate scintillation (sets L54 thesis on the drifting irregularities. (M. Grzesiak, M. Pożoga, B. Matyjasiak)

67 Formation of Dusty Plasma Clouds at Meteoroid Impact on the Surface of the Moon We have presented a mechanism explaining the appearance of two dusty plasma clouds because of the meteoroid impact on the surface of the Moon observed on February 26, 2015. The main characteristics of these clouds have been calcu- lated. It has been shown that the shock wave from the meteoroid impact ejects lunar regolith parti- cles (or fragments) and melt from the surface of the Moon into free space. Rising over the surface of the Moon, both regolith particles (or frag- ments) and melt droplets become electrically cha- rged because of the interaction, in particular, with electrons of the solar wind and with solar radia- tion. As a result, two dusty plasma clouds appear. The first cloud is formed regolith by particles (or fragments) and the second cloud is formed by solidified melt droplets. These clouds have dif- ferent characteristics (cloud expansion velocity, total mass of the particles in a cloud, characteristic sizes of the particles in the cloud, number den- sities and charges of the particles, etc.). Consequ- Fig. 40. Photographs of the region where the meteoroid ently, the clouds can be observed separately. collides at the point (0, 0) with the surface of the Moon taken at 0.25 s before the collision and at 4, 8, 12, 16, and Qualitative agreement has been achieved between 20 s after the collision. The axes present distances in the calculated expansion velocities of clouds and kilometers. Arrows 1 and 2 indicate the fast large and slow observational data. It has been shown that the small dust clouds, respectively. event observed on February 26, 2015, was most February 26, 2015, significantly change the pro- likely induced by a fairly large fast meteoroid with perties of the dusty plasma system over the Mo- the parameters corresponding to the upper part on. In particular, a noticeable amount of dust lu- of the range of possible kinetic energies of me- nar regolith particles (or fragments) with sizes of teoroids, which was obtained by calculating the ki- about 10–100 µm, whose amount in the exo- netic energy of the impactor from the maximum sphere is usually small, is ejected into the exo- brightness of the flash. Events similar to that on sphere of the Moon. Fig. 41. Dynamics of layers of the dusty plasma cloud formed by solidified melt droplets at the altitudes h = (a) 0.1-0.11, (b) 1-1.1 (c) 10-11, and (d) 100-110 km. Time dependences of (R) the radius characterizing the size of the layer in the direction parallel to the surface subjected to the meteoroid impact, (M) the total mass of dust particles in the layer, and (n) the volume-average dust particle density. Published: JETP Letters, 2018, Vol. 108, No. 6, pp. 356–363, ISSN 0021-3640. (S. I. Popel, A. P. Golub', A. V. Zakharov, L. M. Zelenyi, A. A. Berezhnoy, E. S. Zubko, M. Iten, R. Lena, S. Sposettih, Yu. I. Velikodsky, A. A. Tereshchenko, and B. Atamaniuk)

68 An Analysis of Processes in the Solar Wind in a Thin Layer Adjacent to the Front of the Shock Wave A two-dimensional stationary system of nonli- sis of the solution of the MHD equations are con- near magnetohydrodynamics (MHD) equations sistent with the conclusions based on the inve- in a thin layer adjoining the front of the interpla- stigation of the particle velocity distribution func- netary shock wave has been solved. Previously, tions. This makes it possible to confirm the pre- any available publications relied on linear tran- viously established fraction of particles excited to sport equations. But the presence of high-energy energies above 1 MeV. Before this paper, publi- particles in the solar wind (SW) requires taking cations in this field of inquiry were based on the into account the processes of self-interaction. linear transport equation. The presence of parti- Our analysis examines the nonlinear terms in the cles with high energies in the SW requires taking MHD equations. A solution has been constructed into account the processes of self-interaction. for three cases: (1) in the absence of magnetic re- Further development of particle acceleration the- connections; (2) for magnetic reconnections; and ory in the SW should be based on the nonlinear (3) with the simultaneous action of reconnections velocity distribution function of accelerated parti- and junction of magnetic islands. In all three cles. cases, expressions were found for the main para- Published : The Astrophysical Journal, 859:39 meters of the SW. The results obtained on the ba- (5pp), 2018 May 20 (A. Molotkov and B. Atamaniuk)

69 PHYSICAL AND GEODETIC STUDIES OF SOLAR SYSTEM BODIES AND EARTH Planetology and Solar System parts: one part was on the Philae lander on the co- met's surface, while the other was on the Rosetta Dynamics spacecraft. Comet 67P/Churyumov-Gerasimenko CONSERT operated for 9 hours after the Philae from Rosetta mission landing and made measurements through the small lobe (head) of 67P/C-G. Measurements we- What lies inside comet 67P/C-G? re taken of the propagation time of the signal The internal properties of cometary nuclei are the through the comet and the shape of the received best clues to the size distribution and properties signals. 3D propagation models were developed of planetesimals that formed the planets during from this data, which, together with the early Solar System nebula processes. To find out propagation time, made it possible to derive the more, the CONSERT radar (part of the Rosetta bulk permittivity value (= 1.27) of the cometary mission) was designed to probe the interior of co- interior. Permittivity values for porous mixtures met 67P/Ch-G at a wavelength of about 3 meters. of ices and dusts were compared with experi- It operated successfully during the First Science mental, laboratory values in order to determine Sequence, when CONSERT's wave propagated possible constituents of the comet's nucleus (ices, through part of the comet's small lobe. The shape silicates and organics) and its porosity (70–85%). of the received signals offers some insight into its As the minimum content of carbonaceous mate- internal structure. Our study compared the limi- rial is 75% in volume, it appears that the comet ted broadening that was observed to simulations contains a massive carbon reservoir. performed on a series of non-homogeneous nu- Furthermore, as the shape of the signal is very cleus models, in an attempt to identify potential close to the calibration signal, there is no evidence structures at the wavelength scale. Consequently, of scattering by inhomogeneities in the medium. we were able to exclude structures with permit- This indicates that the interior is homogenous at tivity contrast above 0.25 inside the tested part of the scale of few wavelengths. 3D simulations of the nucleus. signal propagation in non-homogeneous media The results of our work were published in Monthly were run to define the sensitivity of CONSERT Notices of the Royal Astronomical Society in December to inhomogeneities, and to identify constraints on 2017, however they were not included in the 2017 internal structures in terms of size and compo- Annual Report. sition, at a scale commensurate with the 3-meters wavelength. Given the high bulk porosity (~75%) (V. Ciarletti, A. Herique, J. Lasue, A.-Ch. Levasseur- of the sounded part of the nucleus, a likely model Regourd, D. Plettemeier, L. Florentin, G. Christophe, is a mixture of voids (vacuum) and blobs, made up P. Pierre, W. Kofman) of ices and dust with a porosity above 60%. The CONSERT probing of the 67P/C-G nucleus absence of spreading due to scattering means that during the Rosetta mission: operations and we can exclude heterogeneity with higher results. dielectric contrast (0.25) and at a much larger scale Our work focuses on the structure and composi- (although larger scales can be responsible for tion of cometary nuclei, which is one of the major multipath propagation). unknowns in cometary science. Such knowledge The properties of meter-scale inhomogeneities is important in understanding the formation and found inside the comet are essential to understan- evolution of comets and this was one of the ding its formation. In September 2016, the precise scientific objectives of the Comet Nucleus Soun- position of the Philae lander was established; this ding Experiment by Radiowave Transmission made it possible to improve the determination of (CONSERT) instrument flown aboard the Euro- propagation paths inside the comet and therefore pean Space Agency spacecraft Rosetta. CON- to better describe its interior. The influence of the SERT was a bi-static radar composed of two immediate environment on antennas lobes and

70 polarization was calculated using the Digital Ter- catalogue of 57 exposed, bright features observed rain Model of the landing site and used to study by OSIRIS on the comet nucleus. All are attri- the received signal power. buted to the presence of H2O ice. Some are thou- Our work is ongoing, and we will soon be able to ght to be frost deposits from the outward branch present measurements of the interior of the co- at the previous perihelion. Others, originating in met, and discuss and interpret our findings in cometary outbursts, represent consolidated, ori- terms of its internal structure and composition. ginal comet material and tend to have higher albe- Our results so far were presented at the 42nd CO- do. The paper by Auger et al. (2018) examined a SPAR Scientific Assembly (July 2018, Pasadena, small-scale morphological feature referred to as California, USA). polygons. Over 6300 of these were studied; they (W. Kofman, A. Herique, V. Ciarletti, J. Lasue, A-C. cover ~1.5% of the nucleus's surface with a mean Levasseur-Regourd, Y. Rogez, S. Zine, D. Plettemeier) size of ~3 meters and are thought to be due to thermal contraction of a near surface hard and Imaging 67P/C-G consolidated H2O ice layer. In 2018, we published several papers reporting re- Two of our articles were published in Astronomy sults from the OSIRIS camera system. The study and Astrophysics, and one each in Monthly Notices of by Gerig et al. (2018) describes dust in the inner- the Royal Astronomical Society and Icarus. most coma region, less than 50 km from the nu- (H. Rickman together with the OSIRIS-Rosetta Team) cleus surface. Profiles of azimuthally-averaged dust brightness, derived from the images, were Erratum: Comet 67p outbursts and quiescent fitted and used for analysis. It was found that free coma at 1.3 AU from the Sun: dust properties radial outflow provides a good fit beyond 12 km. from Rosetta/VIRTIS-H observations. Inside this, effects of grain acceleration and non- point source geometry were seen. The paper by The original paper on this topic was published in Attree et al. (2018) reports estimates of the mini- MNRAS 469, S443 (2017). While performing a mum tensile strength needed to support twenty follow-up investigation, we discovered a numeri- overhanging cliffs on the nucleus surface against cal error in the algorithms that were developed to collapse, under the comet's gravity. This found model the infrared continuum emission from a values of only ~1 Pa. From the presence of ero- population of dust particles. The results of scatte- ded material at the cliff base, and observed or im- ring models for compact or moderately porous plied cliff collapse, we inferred a true average grains (Mie theory) and fluffy grains (Rayleigh- strength of a few Pa for comet material. The Gans-Debye theory, RGD) were affected. Altho- paper by Fulle et al. (2018) considered the phase ugh the general conclusions of the paper are un- function and density of dust particles released changed, there are slight differences in quanti- from the comet. Dust bursts observed close to tative constraints obtained for dust size distri- Rosetta were interpreted as due to the fragmen- bution in the quiescent coma. tation of parent particles upon impact with the This erratum was published in Monthly Notices of spacecraft. Theor bulk density was inferred from the Royal Astronomical Society (July 2018). their measured antisunward accelerations caused (D. Bockelee-Morvan, G. Rinaldi, S. Erard, by solar radiation pressure. This is consistent with C. Leyrat, F. Capaccioni, P. Drossart, G. Filacchione, GIADA dust mass fractions of ~40% hydro- A. Migliorini, E. Quirico, S. Mottola, G. Tozzi, carbons and ~60% sulphides and silicates. G. Arnold, N. Biver, M. Combes, J. Crovisier, The paper by Deshapriya et al. (2018) presented a A. Longobardo, M. I. Błęcka, And M.-T. Capria) Long-period comets – dynamics and statistics Dynamical evolution of C/2017 K2 PAN- will approach its perihelion in December 2022, STARRS and the question of its past dynamics is an impor- C/2017 K2 PANSTARRS attracted attention at tant issue. the time of its discovery in May 2017, when it was A key question is whether C/2017 K2 is a dynami- about 16 AU from the Sun. This Oort spike comet cally old or new comet? To answer this, it is neces-

71 sary to obtain its precise osculating orbit, its origi- ficant, non-gravitational perturbation during its nal orbit, and propagate its motion backwards in upcoming perihelion in 2022. time to the previous perihelion. Knowledge of The results of our work were published in the previous perihelion distance is necessary to Astronomy & Astrophysics (August 2018). distin-guish between the two groups of Oort (M. Królikowska and P. A. Dybczyński) spike co-mets. We therefore studied the dynamic evolution of C/2017 K2 back in time to the How the modified method of orbit quality as- previous perihelion (backward calculations for sesment works for Oort spike comets? about 3–4 Myr) and in the future (forward In 2018, we present a brief overview of the effec- calculations for about 0.033 Myr). This was based tiveness of our modified method to estimate orbit on a virtual comet swarm constructed from the quality, which we initially proposed a few years comet's nominal osculating orbit, which was ago. As we now have a complete sample of 100 determined using all available positional measu- Oort spike comets with large perihelion distances, rements. Outside the planetary system, both we were able to introduce more restrictive condi- Galactic and stellar perturbations were taken into tions. In particular, we can now separate individual account. We derive that C/2017 K2 is a dynami- quality classes, and have introduced a new class cally-old Oort spike comet (1/aprev = (48.7±7.9) containing excellent quality orbits (which we label- ×10-6 AU-1, see Figure 42) with a previous peri- led 1a+). helion distance below 10 AU for 97% of virtual To enrich the study, we compiled a complete visual comets (nominal qprev = 3.77 AU). Current data collection of time distributions of the positional suggest that it will be perturbed into a more datasets we used for orbit determination. We fo- tightly-bound orbit after passing the planetary und that modern measurements of large-perihe- -6 -1 lion Oort spike comets should be carried out for at zone (1/afut = (1140.4 ± 8.0) ×10 AU , qfut = 1.79336 ± 0.00006 AU) provided that non- least 3 years around perihelion (3–4 oppositions) gravitational effects do not significantly change to be as certain as possible that the derived orbit is this orbit. of the highest quality (see Figure 42). Our results C/2017 K2 visited our planetary zone during its strongly support our hope that, in the near future, it will be possible to study the shape of the 1/a - previous perihelion. Thus, it is almost certainly a ori dynamically old oort spike comet. Although the distribution of Oort spike comets in great detail, based only on the highest-quality orbits (i.e. 1/aori- future formal orbital solution is very precise, it is -6 -1 not particularly reliable as the analysis is based on uncertainties well below 5 × 10 AU ). The results pre-perihelion data collected at very large helio- of our work were published in Monthly Notices of centric distances (23.7–14.6 AU from the Sun). the Royal Astronomical Society (June 2018). Furthermore, the comet may experience signi- (M. Królikowska and P. A. Dybczyński)

Fig. 42. Projection of the swarm of orbital elements (5001 virtual comets including nominal orbit) in the previous perihelion of C/2017 K2 onto the 1/a-q plane for the basic solution, augmented with two, marginal distributions of these parameters. Black points indicate the evolved swarm of virtual comets, green cross marks the evolved nominal orbit while full green dots show a Gaussian fitting to 1/a and q marginal

distributions. It is clear that qprev (the red histogram) does not follow a Gaussian distribution.

72 Did we miss an interstellar comet four years to small-perihelion LPCs as a function of 1/a- ago? original, and to construct the precise distribution of an 1/a-original). To minimize the influence of In 2018, we obtained a new orbit for C/2014 W10 PANSTARRS. Its high original eccentricity (e = parabolic comets on these distributions, we deter- 1.65) suggests that the comet has an interstellar mined definitive orbits (which included eccen- origin. In a paper published in arXiv .org (October tricities) for more than 20 LPCs previously classi- 2018), we examined reasons why this potentially fied as parabolic comets. important event was missed, and noted the need We found that the percentage of large-perihelion for an archival search for other observations that comets is significantly higher within Oort spike may have been overlooked. comets than in a group of LPCs with a<10 000 (P. A. Dybczyński and M. Królikowska) AU, and that the ratio of large-perihelion to small- perihelion comets for both groups has grown sys- tematically since 1970 (see Figure 44). Different shape of the Oort spike for small-perihelion and large-perihelion LPCs is also discussed. Addi- tionally, we observed a spectacular decrease in the ratio of large-perihelion to small-perihelion LPCs as the semimajor axis shortens to within a range of 5000–100 AU. Analysing discovery circum- stances, we found that in statistical terms, Oort spike comets are discovered at larger geocentric and heliocentric distances than other LPCs. This difference in the percentage of large-perihelion comets in both groups of LPCs is probably a direct consequence of a well-known comet fading process that is due to ageing of their surface during consecutive perihelion passages and/ or reflects different actual q-distributions. A paper Fig. 43. Distributions of 1/a-uncertainties in a function reporting our work was submitted to Monthly of a period of observations of long-period comets Notices of the Royal Astronomical Society, and was (q>3.1 AU) with pure gravitational orbits (solid triangles accepted at the end of 2018. and dots) and comets with non-gravitational orbital solutions (open triangles and circles). For readability, we (M. Królikowska and P. A. Dybczyński) excluded comet C/2006 S2 due to its exceptionally long observational arc (16.60 years). Objects discovered before 2000 are represent by triangles, while modern comets are shown using dots and circles. Comets with orbits of 1a+ quality are shown in red, 1a quality are shown in magenta, and 1b quality are shown in blue. Comets with second- quality orbits (2a and 2b) are marked by gold points. Background colours are used to distinguish areas corresponding to different quality classes. Discovery statistics and 1/a distribution of long-period comets detected during 1801- 2017 The past two decades have seen a huge increase in discoveries of long-period comets (LPCs), es- Fig. 44. Ratio of large-perihelion (q>3.1 AU) to small- pecially those with large perihelion distances. To perihelion comets (q<3.1 AU) as a function of the discovery period. The red curve shows statistics for Oort find out more, we collected a full dataset of LPCs spike comets, while the green curve describes LPCs discovered in the period 1801–2017, including outside the Oort spike. The overall ratio for the whole their osculating orbits, discovery moments (to sample of LPCs is plotted in black (parabolic comets not included) and cyan (including parabolic comets). These study discovery distances), and original semi- ratios were calculated for 10 year bins, except for the last major axes (to study the ratio of large-perihelion bin which covers a 7-year period (from 2011 to 2017).

73 The internal structure of comets from Rosetta mission observations, primarily pro- Modelling comet 67P/C-G in preparation for vided by the CONSERT 90-MHz radar investi- 2021 gation and the OSIRIS optical imager. Our results suggest that any observed changes in the comet's In November 2021, comet 67P/Ch-G will make radar backscatter reflectivity will be the result of its next closest approach to Earth – at a distance changes in the nucleus' structure, such as surface of 0.418 AU – and the Arecibo Observatory in smoothening associated with increased coverage Puerto Rico plans to take full advantage of this by fine-grained material, or, potentially, nucleus radar detection opportunity. breakup. Our findings were published in EPSC In 2018, our work focused on developing the Abstracts (September 2018). most up-to-date 3D dielectric model of the (E. Heggy, E. Palmer, A. Hérique, W. Kofman) comet's surface and interior. It is based on data Model of a cometary atmosphere Modelling molecular line transfer in come- tion. The excitation of the water rotational and ro- tary atmospheres vibrational lines is influenced by radiative intera- In 2018, I examined opacity effects on Sun ction between regions. This research is ongoing. exciting radiation (via ro-vibrational transitions) (S. Szutowicz) using the updated HITRAN molecular database for vibrational bands of water. A key problem lies Investigating the dynamical history of in calculating radiative transfer at any point of the interstellar object 'Oumuamua cometary coma given optical depth effects. The Our work was described in the 2017 Annual model implements an anisotropic distribution of Report, and a paper was published in February water density in the cometary atmosphere. 2018 in Astronomy & Astrophysics Letters. Molecular excitation processes include collisional (P. A. Dybczyński and M. Królikowska) excitation and infrared pumping by solar radia- From Missions to Asteroids A radar package for asteroid subsurface inve- science, exploration and planetary defence. This stigations: Implications of implementing suite consists of a monostatic high frequency and integration into the MASCOT nanoscale radar to investigate the stratigraphy of surface landing platform from science requirements regolith, and a bistatic low frequency radar (LFR) to baseline design to characterize the deep interior. The MASCOT The internal structure of asteroids is still poorly nanolander will deliver the surface unit of the LFR known and has never been directly measured. Our and other instruments for a close-up study of the knowledge relies entirely on inferences from re- target asteroid. MASCOT already flies on Haya- mote sensing observations of the surface, and busa2 (HY2) in a mineralogy scout configuration. theoretical modelling. Direct measurements are We have published details of the chosen instru- crucial in order to characterize an asteroid's inter- mentation for radar science, baseline mission nal structure from the sub-metric to the global requirements and the initial design for integration scale. into the lander platform, including any special To address this problem, in 2018, we developed a requirements and constraints. The results of our radar package within the framework of the work so far are available in Acta Astronautica. Asteroid Impact Mission (AIM), itself part of the (A. Herique, D. Plettemeier, C. Lange, larger Asteroid Impact & Deflection Assessment J. T. Grundmann, V. Ciarletti, T-M Ho, W. Kofman, (AIDA) mission. The radar is a mature instrument B. Agnus, J. D. Wenzhe, O. Gassot, R.Granados- suite that is designed to improve our ability to Alfaro, J. Grygorczuk, R. Hahnel, C. Hoarau, understand and model the mechanisms driving M. Tokarz, P. Schaffer, A.-J. Vieau, J. Biele, C. Buck, Near Earth Asteroids. It is of key interest for J. G. Fernandez, C. Krause, R. R. Suquet, S. Ulamec)

74 Jupiter Trojan's shallow subsurface: direct ANOS/ JAXA mission. The monostatic radar observations by radar onboard OKEANOS onboard OKEANOS is a unique opportunity to mission directly access the shallow subsurface of these What are the Jupiter Trojans? Are they rocky aste- bodies and image their internal structures and will roids accreted in the vicinity of Jupiter? Captured be the focus of our work (EPSC Abstracts, Sep- icy bodies? Something else? Understanding the tember 2018). genetics of the Trojans is the goal of the OKE- (A. Herique, P. Beck, P. Michel, W. Kofman, A. Kumamoto, T. Okada, D. Plettemeier) Exploring exoplanets with ARIEL A chemical survey of exoplanets with ARIEL capable of observing a large and well-defined pla- Thousands of exoplanets have now been discove- net sample during its 4-year mission lifetime. Tra- red, with a huge range of masses, sizes and orbits: nsit, eclipse and phase-curve spectroscopy me- from rocky Earth-like planets to large gas giants thods will be used. These techniques differentiate grazing the surface of their host star. However, signals from the star and planet using knowledge their essential nature remains largely mysterious: of planetary ephemerides. They will allow us to there is no known, discernible pattern linking the measure atmospheric signals at levels of 10–100 presence, size, or orbital parameters of a planet to parts per million (ppm) relative to the star. At the its parent star. We have little idea whether the che- same time, given the bright nature of targets, more mistry of a planet is linked to its formation envi- sophisticated techniques such as eclipse mapping ronment, or whether the type of host star drives will offer a deeper insight into the nature of the the physics and chemistry of its birth and evolu- atmosphere. tion. Such observations require a stable payload and a ARIEL was conceived to observe a large number satellite platform with broad, instantaneous wave- (1000) of transiting planets. The aim is to develop length coverage that is able to detect multiple a statistical understanding of these exoplanets, molecular species, probe the thermal structure, including gas giants, Neptunes, super-Earths and identify clouds and monitor stellar activity. The Earth-size planets around a range of host star proposed wavelength range covers all of the types, using transit spectroscopy in the 1.25–7.8 expected major atmospheric gases (e.g. H2O, CO2,

µm spectral range and multiple, narrow-band CH4 NH3, HCN, H2S) through to more exotic photometry in the optical range. ARIEL will fo- metallic compounds (such as TiO, VO and con- cus on warm and hot planets; the idea is to take densed species). We have already run simulations advantage of their well-mixed atmospheres, of ARIEL's performance in conducting exopla- which are expected to show minimal conden- net surveys. These experiments were based on sation and sequestration of high-Z materials conservative estimates of mission performance compared to their colder Solar System siblings. and incorporated a full model of all significant Specifically, these warm and hot atmospheres are noise sources in the measurement (taken from a expected to be more representative of the list of potential ARIEL targets that includes the composition of the planetary bulk. latest-available exoplanet statistics). Our conclu- Our observations, in particular, of their elemental sion, at the end of this Phase A study, is that AR- composition (especially C, O, N, S, Si), will pro- IEL will be able to meet stated mission objectives. vide an understanding of the early stages of pla- In particular, it will be able to observe about 1000 netary and atmospheric formation during the exoplanets (depending on the details of the ado- nebular phase and the following few million years. pted survey strategy), which confirms the feasi- ARIEL will provide a representative picture of bility of the main science objectives. Details of the chemical nature of exoplanets, and relate this our work were published in Experimental Astro- directly to the type and chemical environment of nomy (November 2018). the host star. This dedicated survey mission is (G. Tinetti, P. Drossart, P. Eccleston and 241 designed for combined-light spectroscopy, and is co-authors including M. I. Błęcka)

75 The formation of habitable planets mic transfer of icy planetesimals inward, across Closely related to the Centrum Badań Kosmicz- the snow line, by gravitational scattering due to nych PAN's involvement in the ARIEL mission, giant planets forming in the presence of nebular another major new research initiative is planned. gas drag. Here again, the Solar System will be The ultimate goal is to clarify various aspects of taken as the baseline case, due to observational the formation and survivability of Earth-like constraints. planets around solar-type stars in the Galaxy. Two, In 2018, preliminary discussions began with seve- parallel projects are being developed. The first ral international scientists working in the United will focus on dynamic effects of stellar birth clu- States, Sweden, France and Japan, as well as Polish sters on planetary systems, aiming to nail down colleagues. Work has started on the application of the criteria that these clusters must meet in order Aarseth's N-body code to the modelling of the for stable planets to remain in the habitable zone. Sun's birth cluster and the simulation of planetary It will begin with a dedicated study of the Solar scattering of icy planetesimals. This work is System, from which the role of the Sun's birth ongoing. cluster will be characterized. The second will fo- (H. Rickman with the international team including cus on the delivery of water to Earth-like planets P. Wajer and M. Banaszkiewicz from CBK PAN) in different environments: in particular, the dyna- Mars Water in the history of Mars: An assessment High resolution thermal inertia mapping of This paper presents a review of recent literature sloping terrain on Mars: an Apparent Ther- concerning issues related to the origin of water on mal Inertia-based method Mars and its role in the geologic evolution of the Thermal inertia, which represents resistance to planet. The baseline case of our discussion is the change in temperature in the upper few centi- Grand Tack model of planetary migration in the metres of a surface, helps to understand surficial solar nebula, and early planetary orbital instability geology and recent processes that may still be acti- according to the Nice Model. This discussion also ve. Thermal inertia cannot be directly measured benefits from a comparison with the Earth's ac- on Mars and is most often modelled. However, cretional history. Recent observations are used to these models are complex and difficult for the check the results of planetary accretion models, broader community of scientists to apply. leading to a new picture of the early history of We therefore developed a new method, based on water on Mars. The embryo forming the basis of Apparent Thermal Inertia (ATI). This is an ap- the planet was found to have been very deficient proximation of thermal inertia that can be directly in water. During the following period, predating calculated from surface albedo, diurnal tempe- the formation of the Earth's Moon, accreted rature difference, terrain slope and aspects, as well water may have been as high as ~5 km Global as solar geometry. Our method is entirely based Equivalent Layer (GEL), while the amount on available data and does not require additional accreted at later times may have been as low as modelling. Furthermore, it can be used on sloping ~10 m GEL according to recent studies. In parti- terrain, which makes THEMIS thermal mapping cular, the trans-planetary source was found to be possible in nearly any area of Mars, independent insignificant, whatever the time it was active. The of local topography. proposed resurfacing event that created the Bore- We tested our method in an area located in Valles alis basin could have played an important role in Marineris, and it revealed surface properties that the loss of a significant part of the early Martian usefully complement geological information ob- water inventory. The results of our work were pu- tained from other data sources. A comparison wi- blished in Planetary and Space Science (August th results obtained by other approaches based on 2018). modelled data highlighted similarities in flat areas, (H. Rickman, M. I. Błęcka, J. Gurgurewicz, U. G. and illustrated the significant influence of slope Jørgensen, E. Słaby, S. Szutowicz and N. Zalewska) and aspect on albedo and diurnal temperature dif-

76 ferences (Figure 45). Our method increases op- cessible input data: temperature, incidence angle, portunities to use THEMIS thermal data for geo- visible dust opacity, and a digital elevation model. morphologic and geologic mapping. The ap- The results of our work have been submitted to proach can calculate ATI values automatically for Icarus. most of the Mars surface based on a few, easily ac- (M. Ciążela, J. Gurgurewicz, J. Ciążela and D. Mège)

Fig. 45. (a) ATI map; (b) Thermal inertia (TI) map based on the Fergason et al. (2006) mosaic released to the public in 2014; (c) Fuzzy numerical comparison algorithm calculated for ATIc and TI with a Fuzzy Kappa value of 0.85. The scales of maps (a) and (b) are unified for easier comparison; true ranges are 142–750 tiu for the ATIc map (a), and 88–736 tiu for the TI map (b). White zones, excluded from calculations are related to an incidence angle above 79° (maps a and c). Black lines indicate image borders (maps a and b). How does the Martian surface affect the In general, trace gas production depends on the visibility of atmospheric trace gases in mid- structure and composition of the soil and the phy- infrared spectra? sical state of the atmosphere. In 2018, our analysis Our work is connected with the measurements focused on the influence of optical spectral fea- taken by the stereoscopic camera CASSiS (the Co- tures on the surface and in the atmosphere con- lour and Stereo Surface Imaging System), which is taining trace gases on radiance spectra. The mo- part of the payload of the ExoMars Trace Gas dels we developed provide estimates of spectral Orbiter (TGO), a of the European Space Agency reflectance/emittance and total radiance from the mission. Martian surface and atmosphere in the mid-infra- The CASSiS camera offers an opportunity to red spectral range. Examples of diverse surface analyse the structure and locations, on the surface shapes and subtle soil structures were selected of Mars, of possible sources of trace gases (e.g. from the pictures taken by the HIRISE instru- methane). Identification and monitoring of mi- ment. These surfaces were spectrally described in nor species in the atmosphere are performed terms of presumed reflectance and emissivity of from the orbiter by spectrometric instruments minerals and rocks (e.g. serpentinized rocks) at se- (e.g. NOMAD, ACS). Various features on the lected locations. Spectral reflectance and emis- Martian surface could release trace gases: exam- sivity were calculated from n,k with Mie and Hap- ples include volcanos in Utopia, the Gusev Crater, ke theories, or measured in the lab. The atmo- Arabia Terra and Valles Marineris. It is likely that sphere was characterized in terms of its thermo- different processes led to methane emission inclu- dynamic parameters, and absorbing or scattering ding, among others, serpentinized rocks. properties. We also analysed mid-infrared spectral

77 signatures of the surface and atmospheric trace Role of solar-induced thermal stress on Mar- gases in various physical conditions. Our preli- tian rocks minary conclusions (Figure 46) concerned the vi- Mapping of recent rockfalls (<100 ka) in relatively sibility of spectral features of trace gases (metha- fresh impact craters on Mars indicates that they ne) in radiance spectra. Reflectance measure- tend to occur on slopes that have a certain orienta- ments (Figure 47) were performed at the Military tion and latitude. Specifically, rockfalls are more University of Technology (by Dr Mirosława Ka- numerous in mid-latitude craters with equator- szczuk) and the Institute of Aviation (by Dr Nata- facing slopes than pole-facing slopes or other lia Zalewska) in Warsaw, where the composition orientations. At equatorial latitudes, there are mo- of the sample was also analysed. This analysis re rockfalls on N–S oriented slopes than E–W confirmed that the measured sample is good ones. Rockfall events triggered by phase changes analogue for Martian conditions of the surface . (as on Earth) seem to occur where water ice can Our work is ongoing, and a paper presenting our condense and/or be preserved from previous ice findings is planned for 2019. The results of our ages (i.e. on pole-facing slopes at mid to high- numerical modelling were presented at the 42nd latitudes and not at the equator). This suggests

COSPAR Scientific Assembly (July 2018, Pasa- that H2O or CO2 phase changes do not play a role dena, California, United States) and our analyses in present-day rockfall activity. Instead, our results were published at EPCS 2018 in Berlin, Germany. show that it is more likely to be related to insola- tion. Numerical simulation of solar flux on Mar- tian slopes (~45°) at equatorial and mid-latitudes indicates a correlation between high rockfall activity and high energy received on the surface. This finding highlights the role of solar-induced thermoelastic stress in the weathering of Martian rocks. Our preliminary results were published in EPSC Abstracts (September 2018). (P-A. Tesson, S. J. Conway, N. Mangold, S. Lewis, J. Ciążela) Investigating the fate of trace gases: a photo- Fig. 46. Results of numerical simulations of nadir chemical model of the Martian atmosphere measurements of the surface and atmosphere of Mars All constituents of the Martian atmosphere are showing radiance at the top of the atmosphere in the spectral region of methane absorption. Calculations subject to solar radiation and react with each other include: the reflectance of dark regions of Mars, in the presence of atmospheric aerosols. This identified in the literature as containing intrusions of leads to several hundred reactions that change the serpentinite; typical concentrations of gases in the atmosphere; and maximum concentrations of CH . abundance of all species. In 2018, we developed a 4 model of Martian atmospheric photochemistry, chemistry and transport to simulate these chan- ges. The main, single-column chemical and pho- tochemical model is coupled with model of tran- sport and reactions in the subsurface to simulate the release, transport and loss of trace gases. Mo- lecules can react with each other, be exchanged between layers of the atmosphere, be lost to reac- tions with aerosols and the surface, or escape into space. The specific aim of our model is to analyse data Fig. 47. The reflectance of serpentinite measured in the laboratory (IA): horizontal axis – wavelength [in microns]; from the European–Russian ExoMars Trace Gas vertical axis – reflectance. Orbiter (TGO), which is currently performing (M. I. Błęcka) scientific observations. The CaSSIS camera is re-

78 cording colour and stereo images of the surface that we intend to use to characterize sources and sinks of trace species, notably methane (CH4), which shows great and unexplained variability. High-precision measurements of the abundance of trace gases will be taken by the NOMAD and ACS instruments. The mission is expected to de- termine the detailed composition of the atmo- sphere and detect hitherto unobserved species that are predicted to exist on Mars (e.g. So2). The results of our work so far have been publi- shed in EPSC Abstracts (September 2018) and Fig. 48. Location of the main shear zone exposures and our research is ongoing. extrapolated trends. The base map is the HRSC digital elevation model of Valles Marineris. (P. Witek, P. Wajer, M. Banaszkiewicz, W. Kofman, L. Czechowski and A. Pommerol) High resolution thermal inertia mapping of sloping terrain on Mars: a Differential Appa- Brittle-plastic and brittle shear tectonics in rent Thermal Inertia-based method Valles Marineris As direct measurement of thermal inertia (P) is Hebes Chasma and Ophir Chasma are the two not possible on Mars, thermal inertia models and deepest troughs of the Valles Marineris. Dextral, deductive methods (Apparent Thermal Inertia: brittle-plastic shear zones several kilometres wide ATI and Differential Apparent Thermal Inertia: run NE–SW and ENE–WSW on the chasma DATI) are used to estimate it. ATI is computed as floors. Structural maps of these areas were (1-A) / (T – T ), where ∆T is the temperature prepared. Mapping suggest that the northern part day night difference, and A is albedo. Due to the lack of of Valles Marineris is probably composed of thermal daytime images with maximum land sur- large, sheared tectonic blocks that moved relative face temperature (LST) and nighttime images with to each other while, overall, Valles Marineris was minimum LST, the ATI method is difficult to ap- being stretched perpendicular to its main, ESE ply. To overcome this problem, we explored the trend (Figure 48). DATI technique. Deformation takes the form of wide, S-C struc- DATI is calculated based on shorter time (t) tures, indicative of brittle-plastic shearing. These intervals with a high |∆T/∆t| gradient (in the structures are the first observed evidence of deep morning or afternoon); it is proportional to the tectonics on Mars. It appears that block bounda- day/night temperature difference (ATI) and, hen- ries have played a role in guiding the tectonic and ce, P. Mars, which exhibits exceptionally high geomorphologic evolution of Valles Marineris. |∆T/∆t| gradients due to the lack of vegetation As shear structures do not follow the lava flows and thin atmosphere, is especially suitable for the that cap the surrounding plateaus, shearing pro- DATI approach. Our method takes local topogra- bably predates the deposition of these flows. Ho- phy (slopes and aspects) into account and is based wever, our analysis of Hydrae Cavus, a shallow on existing datasets, rather than modelled values. pull-apart graben next to Candor Chasma that has The method is especially useful in three, petrolo- never been studied before, suggests that these gical applications. structures were reactivated. Firstly, exposure of harder rocks (ATI > 520 Jm- Our work will continue in 2019 and 2020, with the 2 -1 -1/2 incorporation of mineralogical information and K s called also tiu) can be distinguished from continued tectonic analyses of Valles Marineris, loose sedimentary material (ATI < 400 tiu). while our preliminary results were published in Secondly, sediment grain size can be estimated. EPSC Abstracts (September 2018, 2 abstracts). For example, dusts (silt fraction) show an ATI < ~200 tiu, and sands an ATI of 260–400. Thirdly, (D. Mège, J. Gurgurewicz and P. A. Tesson) major types of Martian hard rocks such as basalts (1630–2200 tiu) and serpentinites (~2500 tiu) can

79 be distinguished from each other. Despite the province in Early Noachian (~4.3 Ga), small different approach, we found that DATI values in magma reservoirs stopped working at an early flat areas are in the same range as those obtained stage and yielded smaller volcanoes, while larger by Fergason et al. (2006). However, they provide magma reservoirs marked by the largest volcanoes more accurate information for geological inter- lasted longer and may be still active. Based on the pretations of hilly or mountainous terrains. assumption that the growth rate of a single vol- Our preliminary results were published in cano is non-linear, and decreases exponentially Mineralogia Special Papers (October 2018). over time at a rate similar to the rate of crustal (M. Ciążela, D. Mège, J. Ciążela, growth, we used the 12 volcano volumes and ages J. Gurgurewicz and P-A.Tesson) as a dataset of 24 constraints to model average magma flux since Tharsis magmatic activity began Large Tharsis volcanoes keep growing mar- ~4.3 billion years ago. Our results indicate that the king >4 Ga-lasting Martian hot spots flux has decreased exponentially over time – from Due to lack of plate tectonics and magnetic field, >2000 km3/myr in Noachian to ~92 km3/myr the Martian core was traditionally interpreted as today (Figure 49). In this light, the >4-Ga-lasting entirely solid. However, this has been recently Tharsis volcanism is dormant, rather than extinct. questioned by many researchers, who have sug- Potential CH4, H2S, SO2, and HCl emissions asso- gested the presence of a liquid outer layer sur- ciated with hydrothermal venting and volcanism rounding the Martian core: a theory that is cur- tracked by the ExoMars Trace Gas Orbiter may be rently being tested by the ongoing InSight mis- found at the calderas of Olympus Mons and, sion. potentially, the Tharsis Montes. These preliminary At the same time, the growing body of evidence results were published in Mineralogia Special indicates recent volcanism (2-250 Ma) on Mars. Papers (October 2018). We took advantage of the lack of plate tectonics (J. Ciążela, D. Mège, M. Ciążela, J. Gurgurewicz, and limited erosion on Mars to investigate the P-A. Tesson, B. Pieterek and A. Muszyński) intensity of volcanism in the Tharsis province from Early Noachian to Late Amazonian. Tharsis is the planet's largest volcanic province of Mars with well-known 21-km-high Olympus Mons and at least 302 other large, medium and small volcanoes (>1 km diameter). We estimated the ages of last activity and volumes of the 12 largest Tharsis volcanoes. Our results indicate a distinct inverse correlation 2 (R = 0.75) between volcano volumes and their Fig. 49. Modelled magma flux vs. age in Tharsis province. youngest summit caldera ages. Importantly, we The 12 diamonds represent the largest Tharsis volcanoes. did not find such an inverse correlation in other The ages of diamonds indicate when a volcano became dormant, and corresponding magma fluxes indicate yield volcanic provinces. For example, no dependence from the remaining active volcanoes. Red diamonds on age was found for the three large volcanoes in represent the Olympus Mons and Arsia Mons, and are not the Elysium province (R2 = 0.03). This province is, consistent with the other volcanoes; in fact, model fit would improve if their age was negative. Thus, Olympus however, characterized by a relatively thin crust Mons and Arsia Mons might be still active. Indeed, the (40–50 km) and short-lasting volcanism is mostly fitted curve predicts a present-day magma flux (x=0, 3 limited to Noachian and Hesperian. Tharsis, on where x is age) of 91.8 km /myr in the Tharsis area, which is consistent with the current global Martian flux the other hand, features a thick crust (70–90 km) of 8–400 km3/myr estimated by Kiefer (2003, in and there has been prolonged tectonic activity Meteoritics & Planetary Science). with nearly constant intensity throughout Martian Hydrothermal evolution of Ladon Valles, the history. first study site of the ExoMars Trace Gas Or- Our new results support this indicating prolonged biter CaSSIS Science Team magmatic activity in Tharsis. After a coeval The CaSSIS instrument, flown onboard the Exo- beginning of volcanic activity in the entire Tharsis Mars Trace Gas Orbiter has been acquiring scien-

80 tific datasets since May 2018. The CaSSIS Science simulated Martian soil samples Phyllosilicatic Team selected an image of the Ladon Valles area Mars Regolith Simulant and Sulfatic Mars for investigation, and used it to study the geology Regolith Simulant to model Hellas Planitia, which of the site based on colour filtered data, and a Di- showed that the composition of the selected area gital Terrain Model generated by stereophoto- is high in sulphates.Linear spectral combination grammetric and photoclinometric analyses of modelling was chosen, and was performed using MRO/CTX images. We also conducted a detailed PFSLook software developed by the CBK PAN. analysis of hyperspectral MRO/CRISM data that Additional measurements were collected using an constrains the composition of the site. In par- infrared spectrometer with thermal infrared spec- ticular, we verified the permittivity of the site aga- troscopy, for comparison with PFS and TES mea- inst the permittivity map presented in the 2017 surements. Our work seeks to match the minera- Annual Report in order to constrain the depth of logical composition to the measured spectrum the first dielectric interface. These results, toge- from the surface of Mars and the method is useful ther with complementary results from other gro- in areas where sample collection is not yet possi- ups in the CaSSIS team (notably the National ble. Areas were chosen based on data availability. Institute of Astrophysics at Padova) are currently Martian infrared spectra were modelled by apply- embargoed, and the publication policy is in the ing the linear combination of spectra of selected hands of the CaSSIS Principal Investigator. Me- minerals, which were normalized against the anwhile, our research is ongoing. measured surface area with a previously-separated (D. Mège and J. Gurgurewicz) atmosphere. Minerals were selected based on the expected composition of Martian rock (e.g. ba- New explorations of the mineral composition salt). of the surface of Mars Modelling of surface The software program was named PFSLook; it spectra with and without dust from Martian was written in C11 at the CBK PAN. It is based on infrared data: new aspects adding spectra of minerals at the relevant per- In 2018, work continued on characterizing the mi- centage, resulting in a final spectrum containing neral composition of Martian surfaces based on 100% of the minerals. data collected by the Thermal Emission Spec- The results of our work confirm that there is a trometer (TES; Mars Global Surveyor), measured relationship between the modelled, altered and in the infrared thermal range. We were able to pre- unaltered basaltic surface, and the spectrum sent a model and interpretation of TES spectral measured by Martian instruments. Spectral data from selected Martian regions, from which deconvolution makes it possible to interpret mea- atmospheric influences had been removed using a sured spectra from areas that are difficult to explo- radiative transfer algorithm and a deconvolution re, or to choose interesting sites. Software deve- algorithm. Spectra from the dark area of Cim- lopment means that the method is only described meria Terra and the bright area of Isidis Planitia for mid-infrared, but it can also be applied to were presented in studies led by Philip Chris- shortwave spectra in the near-infrared band for tensen and Joshua Bandfield; they were subjected data from operational Martian spectroscopes. to spectra deconvolution to estimate the mineral composition of the Martian surface. Our work is the only attempt to model the spectra of the surface of Mars with a separated atmo- The results of these analyses were used to model sphere, and to determine its mineralogical compo- dusty and non-dusty surfaces of Mars. Additional sition. Our findings were published in Aircraft data was drawn from the mineral composition of Engineering and Aerospace Technology (Novem- Polish basalts and mafic rocks for modelling Mar- ber 2018). tian meteorites Shergottites, Nakhlites and Chas- signites. Finally, spectra for modelling the Hellas (N. Zalewska, M. Mroczkowska-Szerszen, region were obtained from the Planetary Fourier J. Fritz, M. I. Błęcka) Spectrometer (PFS) onboard Mars Express, and The Isidis Planitia volcanic system the mineralogical composition of basalts from the The focus of our work is to develop a spatial di- southern part of Poland. The analysis also used stribution algorithm to address the issue of arched

81 cone structures found on the Isidis Planitia plain on Mars (Fig. 50), with the aim of distinguishing them from other structures in the area. Our goal is to find out how they were originally formed. In its final form, the algorithm will facilitate the pre- processing of image data and the analysis of stru- ctures of interest. In particular, it will be able to determine linear structures on the surface in ques- tion (linear and conical forms, arched ridges) and classify designated structures in terms of their spatial characteristics. This work is ongoing. Fig. 50. Cone fields on Isidis Planitia showing (N. Zalewska, M. Jenerowicz) characteristic furrows through the centre, forming arched structures. Courtesy of Google Mars, image width 60 km (10 cm=60 km). Comparative planetology SOlar SYstem analogues database POLand range and 10 nm in the infrared (instrument of (SOSYPOL) Laboratoire de Planétologie et Géodynamique at The SOSYPOL database is a part of the SSHA- Nantes, France). Tholin spectra were collected DE (Solid Spectroscopy Hosting Architecture of using a Fourier Transform Infrared spectrometer Databases and Expertise, https://www.sshade. (Nicolet, NEXUS 670) with a drift reflectance eu), an interoperable solid spectroscopy database accessory (Harrick, Praying Mantis DRP) moun- infrastructure, which contains a set of specialized ted inside the instrument's compartment (instru- databases from various European research gro- ment of NASA Ames Research Center). Tholin ups and is developed under the Europlanet 2020- experiments were conducted in the Andromeda RI programme (H2020). chamber at the Keck Laboratory of the Arkansas Our database contains spectra of analogue mate- Center for Space and Planetary Sciences. The rials of Solar System solid body surfaces, which database is available online at https:// www. have been collected to help in the interpretation sshade.eu/db/sosypol since February 2018. of spectra obtained by various space missions. (J. Gurgurewicz and D. Mège) The samples studied currently are various altered Constraining the magmatic plumbing system basalts, and mixtures of ice and organic matter in a zoned continental flood basalt province (tholins). The spectroscopic technique used is The Tharsis region of Mars contains the largest visible, near-infrared and mid-infrared reflec- flood basalt province in the Solar System. It is also tance. Spectra are collected in simulated environ- one of the most complex, featuring the migration mental conditions, ambient conditions, as well as of magma, the most significant being migration during field campaigns. Data currently ingested in from the Syria Planum area to the Tharsis shield the SOSYPOL database include: (1) Vis and NIR volcanoes. Some aspects of the migration of the reflectance spectra of basalts altered in cold magmatic plumbing system can be understood (Udokan, Siberia) and hot (Ogaden, Ethiopia) using Earth-based analogues. We therefore deve- arid environments, collected to help interpreting loped a methodology based on satellite image pro- the spectra of the surface of Mars; (2) NIR refle- cessing (similar to techniques used for Mars), but ctance spectra of several mixtures of ice and orga- with the addition of age dating and geochemistry nic matter (tholins) at various temperature and data, in order to shed further light on the migra- pressure conditions, to contribute interpreting the tion of plumbing systems. composition of the surface of Pluto and Charon. This dataset can be also used to determine the We examined the Oligocene Ethiopian Flood Ba- composition of aerosols in Titan's atmosphere. salts magma plumbing system (Figure 51). In this Basalt spectra were collected using the ASD province, domains are defined by the eruption of FieldSpec® 3 spectrometer in the range 0.35–2.5 low-Ti (LT) and high-Ti (HT) lavas. This requires µm, with 3 nm spectral resolution in the visible a magmatic plumbing system that facilitates the

82 transit of compositionally-distinct ma- gmas through the crust without mixing. Our geochemical and geochronological study examined a suite of 43 dykes from western Ethiopia. We found that most were emplaced contemporaneously with the Oligocene flood basalt phase of activity. Their composition is over- whelmingly LT, typified by an overall flat rare earth element pattern (median La/LuCN = 2.6), and a lack of enri- chment in in-compatible trace elements compared to HT lavas. These observa- tions confirm the western Ethiopian dyke swarm as a source for LT flood basalts in the Ethiopian Flood Basalts. We also found tentative evidence for an eastward migration of the LT dyke sy- stem. These observations are consistent with the terminal stages of LT magma- tism centred on the Simien shield vol- cano. This leads us to conclude that the apparent separation of ~400 km bet- ween LT and HT ma-gma plumbing systems enabled the development of a clearly geochemically-zoned continen- tal flood basalt province. Our findings were published in Geochemistry, Geo- Fig. 51. Satellite image mapping of dyke swarms in the north-western physics, Geosystems (September 2018). Ethiopian Flood Basalts, showing the location of the analysed samples (T. O. Rooney, S. R. Krans, (images source: Sentinel-2 and DigitalGlobe [WorldView 2-4, D. Mège, N. Arnaud, Quickbird]). Dyke swarms of different age and orientation are mapped in different colours. A principal component analysis revealed details of T. Korme, J. Kappelman and G. Yirgu) two ring dyke complexes (Angareb, Dangur), one of which has not previously been reported. Nanotopographic characterization of micro- such as Scanning Electron Microscopy (SEM), fractures in rocks by Atomic Force Micro- has huge potential in this field, with the possibility scopy to put fracture nanotopography into context. Not The study of microfractures is one of the keys to only can micro- or nanofractures be described understanding a variety of geological issues inclu- with a resolution of ~1 nm, and be compared to ding: microcrack initiation and propagation; pro- ~1 µm resolution obtained using other methods, cess zone characterisation and the evolution to- but also AFM can correct misleading SEM obser- ward large-scale fracturing; the characterisation vations. A paper reporting our work has been of reservoirs of geological fluids; and the identi- submitted to the Journal of Structural Geology. fication of microhabitats outside Earth. (J. Gurgurewicz, D. Mège, M. Skiścim and J. Pers) Atomic Force Microscopy (AFM) records nano- Investigation of friction weakening of terre- scale digital terrain models (nDTM), making it strial and Martian landslides using discrete possible to carry out quantitative, nanoscale struc- element models tural analyses of rocks (illustrated here with two Understanding what controls how far large land- basalt samples). AFM coupled with techniques slides travel has been a topic of considerable de- able to provide some mineralogical information, bate. Empirical work that combines observations

83 and experimental data with depth-averaged con- tains in Eastern Europe is investigated after their tinuum modelling of landslides and the seismic likely similar postglacial origin is established. De- waves they generate has found that lower effective formed Martian ridges are larger than their ter- friction must be taken into account in the models restrial equivalents by one to two orders, although in order to reproduce the dynamics and runout their height-to-width ratio is similar (~0.24). distance of larger landslides. Such simulation and Measured finite strain of the Valles Marineris observation results are compatible with the phe- ridges is three times higher than in the Tatra Mo- nomenon of frictional weakening with velocity, as untains, suggesting that although initial condi- observed in earthquake mechanics. tions were different , with steeper slopes in Valles We investigated whether a similar empirical redu- Marineris, the final ridge geometry is now similar. ced friction should be taken when using Discrete As DSGSD is now thought to be inactive in both Element Models (DEM) to reproduce observed regions, their comparison suggests that whatever runout of large landslides on Earth and on Mars. the initial ridge morphology, DSGSD proceeds First, we showed that, in the investigated parame- until a mature profile is attained. ter range and for a given volume, the runout On both planets, strain is distributed over the sa- distance simulated by 3D DEM is insensitive to me number (~5) of major scarps; fault displa- the number (i.e., size) of grains – once this num- cements are therefore much larger on Mars. The ber reaches ~8000. We then calibrated the model large offsets suggest the reactivation of DSGSD with laboratory experiments and simulated other fault scarps in Valles Marineris, while a single granular flow on inclined plane experiments ma- seismic event would have been enough in the Ta- king it possible, for the first time, to reproduce tra Mountains. The longer period of activity of observed effects of initial volume and aspect ratio Martian faults may be correlated with a long on runout distances. In particular, the normalized succession of climate cycles generated by the un- runout distance is a function of volume only abo- stable Mars obliquity. In sum, despite current ve a critical slope angle of >16–19°, as observed similarities in their global geometry, the studied experimentally. Finally, based on field data (volu- ridges on Mars and Earth affected by DSGSD did me, topography, deposit), we simulated a series of not start from similar initial conditions and did not landslides on simplified, inclined topography. The follow the same structural evolution. An article empirical friction coefficient, calibrated to repro- reporting these findings has been submitted to duce observed runout for each landslide, was sho- Earth Surface Dynamics. wn to decrease with increasing landslide volume (O. Kromuszczyńska, D. Mège, K. Dębniak, (or velocity), reaching values as low as 0.1–0.2. No J. Gurgurewicz, M. Makowska and A. Lucas) distinguishable differences were observed bet- ween the behaviour of terrestrial and Martian Discovery of a hydrothermal fissure in the landslides. A paper reporting these findings has Danakil depression been submitted to Landslides. Volcanic rift zones are among the most emble- (T. Borykov, D. Mège, A. Mangeney, P. Richard, matic features found on both Earth and Mars, and J. Gurgurewicz and A. Lucas) differences between them mainly result from different value of a single parameter: gravity. Rift Deep-seated gravitational slope deformation zones provide appropriate hydrothermal environ- scaling on Mars and Earth: same fate for dif- ments for the development of micro-organisms ferent initial conditions and structural evolu- in extreme conditions; this development initially tions depends on endogenic processes rather than the Some of the most spectacular instances of deep- planetary climate. seated gravitational slope deformation (DSGSD) On Earth, the Europlanet 2018 Danakil field are found in the Valles Marineris region on Mars. campaign identified a previously-unreported 4.5 They provide an excellent opportunity to study km-long hydrothermal fissure in the Ethiopian DSGSD phenomenology using a scaling ap- Lake Asale salt flats. This area forms the Erta proach. The topography of selected DSGSD Ale–Dallol segment of the southern Red Sea rift scarps in Valles Marineris and in the Tatra Moun- and is one of the best terrestrial geological analo-

84 gues of Martian rift zones. We conducted the first ject in the longer term. The next steps will be to geological analysis of this fissure, analysed the collect and analyse ground magnetic data in order geochemistry of its hydrothermal fluids, and to determine the sector's fissure nature (tectonic began to investigate its history through archived or magmatic) and geometry, and its effect on the high-resolution satellite images. alteration of surrounding rocks. Our preliminary A project proposal was submitted to the Digi- results were published in EPSC Abstracts (Sep- talGlobe Foundation in order to obtain additional tember 2018). high- resolution imagery that will be used in furt- (D. Mège, E. Hauber, M. De Craen, her work in 2019, as we plan to continue the pro- H. Moors and C. Minet)

Earth Rotation and Geodynamical Studies (Department of Planetary Geodesy) In the first part of our work, we used several com- binations of atmospheric and oceanic models in Geophysical interpretation of polar motion order to determine AAM and OAM. The resulting excitation AAM+OAM sums were compared with GAM Change in the orientation of the Earth's rota- calculations. The purpose was to determine to tional axis is known as polar motion. It is due to what extent determinations from AAM+OAM the constantly-changing mass distribution of the models corresponded to actual measurements. We Earth's geophysical fluids (atmosphere, oceans found that, for the non-seasonal part of the and land hydrosphere). The main method used to spectrum, the sum of AAM+OAM agrees well determine their influence is to compute so-called with GAM. A more detailed analysis found that Atmospheric Angular Momentum (AAM), Ocea- correlation coefficients between AAM+OAM nic Angular Momentum (OAM) and Hydrological and GAM are highest for the combination of Angular Momentum (HAM) functions. The sum ECMWF (atmosphere) and MPIOM (ocean), and of these functions is known as geophysical exci- NCEPP/NCAR (atmosphere) and ECCO080 tation, and its accuracy can be evaluated by a com- (ocean) models (Fig. 52). Best variance agreement parison with observed geodetic excitation func- is obtained for the combination of the ECMWF tion (Geodetic Angular Momentum, GAM), model and the MPIOM model. For seasonal computed from observations of pole coordinates components we found similar results for mass obtained using precise space geodesy techniques. terms (resulting from air pressure and ocean In 2018, we continued our research into: 1) the bottom pressure) of AAM and OAM obtained agreement between the sum of AAM, OAM and from different models. However, the motion HAM functions and GAM observations; and 2) terms (resulting from winds and ocean currents) the agreement between HAM functions calcu- are distinguished by various amplitudes and pha- lated from observations collected by the GRACE ses (Fig. 53). satellite mission and GAM functions.

Fig. 52. Comparison of χ1 and χ2 components of GAM with various AAM+OAM excitation functions.

85 a)

b)

c)

d)

e)

Fig. 53. Comparison of amplitudes and phases of annual, prograde and retrograde oscillations for GAM, AAM and OAM functions.

86 The second part of our work focused on the We found that although, in general, correlation comparison of land hydrosphere data from the coefficients between GAO and GRACE-based GRACE mission and GAM. First, GRACE data HAM are higher for GRACE RL06 series than were used to compute HAM functions. These RL05, especially for JPL-based series, these values were then compared with hydrological part of are not satisfactory, especially for χ1, where varian- GAM observations (called geodetic residuals – ce is negative in many cases. Best agreement for all GAO) at various scales: short-term, seasonal, spectral bands was found with the ITSG2018- non-seasonal, decadal, and interannual (Fig. 54). based HAM series.

Fig. 54. Comparison of χ1 and χ2 components of geodetic residuals (GAO) with HAM functions obtained from GRACE solutions and the LSDM model. (J. Nastula, M. Wińska, J. Śliwńska) Geophysical excitation of the Chandler be explained was at the level of 20%. wobble – research using the GRACE data In this study we took an advantage of the fact Chandler wobble (CW) is a free motion of the that the mass term of polar motion excitation

Earth's pole which is the largest component of components (χ1, χ2) is proportional to time va- polar motion. It has been observed on regular ba- riable gravity coefficients (C2,1, S2,1) which are esti- sis since the end of XIX century. The observa- mated from Gravity Recovery and Climate Expe- tions show that its amplitude is changing but there riment (GRACE) and the Satellite Laser Ranging is no clear decaying tendency. Therefore it must (SLR) observations. Our purpose was 1) to esti- exist a process or a combination of processes mate the Chandler wobble excitation by the mass which excite this oscillation against the energy dis- redistributions of the external geophysical fluids sipation. A search for the physical mechanism using GRACE and SLR gravity data, and 2) to which excites this free polar motion to the obser- consider also the role of the motion term in the ved level has been for decades one of the most Chandler wobble excitation balance by using the intriguing questions regarding global dynamics of data from geophysical models. Comparison of the the Earth. Several excitation mechanisms have geodetic and gravimetric excitations of polar mo- been proposed since the discovery of CW, but tion is shown in Fig. 55. Tab. 1 summarizes results only recent studies by, e.g. Brzeziński and Nastula of the cross-correlation analysis of the geodetic (2002), using improved models of the atmo- excitation of polar motion and combinations of spheric and oceanic circulation over 1985-1996 the gravimetric (GRACE-derived) excitations and could demonstrate that during that 11-year period motion term of the modeled atmospheric (A- the CW was mostly driven by irregular angular NCEP) and oceanic (O-ECCO) excitations. Ana- momentum exchanges between the coupled lysis has been done over the 11-year period 2003.0 system atmosphere-oceans and the solid Earth. In to 2014.0 with the highest quality GRACE data our estimation the remaining excitation power to (see Fig. 55). Results are shown only for the sele-

87 cted 3 GRACE solutions: CSR-RL05 – Center for high level – correlations 0.8, 0.9 and variance re-

Space Research, Austin, U.S.A; Tongji-RL02 – duction about 60%,80% for χ1, χ2; Tongji University, Shanghai, P.R. China; WHU- narrow-band correlation analysis at the Chandler RL01 – GNSS Research Center of Wuhan frequency: University, P.R. China. From this analysis we • we found a high coherence and a good agre- could conclude what follows: ement of power at the Chandler frequency bet- cross-correlation analysis of the de-seasoned and ween the geodetic excitation and the three sele- de-trended geodetic and geophysical excitations: cted GRACE-based functions representing the

• better agreement was found for χ2, corres- mass term of excitation;

ponding to S2,1, than for χ1 corresponding to C2,1; • adding the motion term of excitation impro- • the best result found – correlations 0.7, 0.8 ves slightly the coherence and the excitation

and variance reduction 50%,65%, for χ1, χ2, res- power becomes higher than expected from the pectively – was for the GRACE-derived series geodetic observations of polar motion. CSR, Tongji and WHU; We continue our research by using the recently re- • adding the motion term of excitation, estima- leased GRACE-RL06 series (Brzeziński and Na- ted from geophysical models, improves the agre- stula, in preparation). ement with geodetic series to the considerably

Fig. 55. Comparison of the geodetic and gravimetric excitations of polar motion, original curves (top) and the differences between geodetic and gravimetric excitations (bottom). Seasonal- polynomial model has been removed from each series prior to analysis.

88 Table 1. Cross-correlation analysis of the geodetic for the selected GRACE solutions: CSR-RL05, excitation of polar motion and combinations of Tongji-RL02, WHU-RL01. Complex correlation the gravimetric (GRACE-derived) excitations and and coherence coefficients are shown as magni- motion term of the atmospheric (A-NCEP) and tude and argument, PSD is expressed in mas2/ oceanic (O-ECCO) excitation. Analysis has been cpy. done over the 11-year period 2003.0 to 2014.0 and

Note: Our estimate of the coherence magnitude is not constrained to be less or equal 1. (A. Brzeziński, J. Nastula) Determining the position of Satellite Laser the stations. The results were compared with the Ranging stations results obtained from LAGEOS-1 and LAGE- In 2018, computations were performed to deter- OS-2 satellites. mine the positions of 15 selected Satellite Laser Also in 2018, computations were run to establish Ranging stations, operating in the period 2012- the coordinates of the Borowiec Satellite Laser 2016, from laser observations of the LARES sa- Ranging station for the period 2015-2018. Results tellite. These computations were performed with were compared with the results obtained for the the GEODYN-II orbital program in the ITRF- years 2006-2010 and no significant differences 2014 coordinate frame. The results of this work were found. These results were presented at the were presented at the 21st International Work- 21st International Workshop on Laser Ranging, shop on Laser Ranging, which took place in Can- and at the Satellite Position - Precise Navigation - berra (Australia) in November 2018. The purpose Mobile Monitoring conference which took place of the work was to check the suitability of the LA- in Dęblin, Poland in September 2018. RES satellite in determining the coordinates of (S. Schillak) GalAc The Cetrum Badań Kosmicznych PAN recently Technology Research programme, relating to the finalized the GalAc project. This project aimed to study and development of innovative GNSS me- analyse the feasibility and usefulness of equipping thodologies and technologies, especially algori- second-generation Galileo spacecraft with accele- thms, software and hardware. It is anticipated that rometers to improve the accuracy of the Precise GNSS positioning accuracy will reach the level of Orbit Determination and the Galileo Terrestrial millimetres, while ground infrastructures need to Reference Frame. The project addressed the obje- be simpler and more cost-effective. Accelerome- ctives of the Global Navigation Satellite System ter data can be used to directly measure the unmo- (GNSS) Evolution in Scientific and Innovative delled effects of nongravitational perturbations

89 (NGP) and spacecraft acceleration due to on- Using water tube tiltmeters and GPS vector to board activity. In parallel, the Inter-Satellite Link measure tectonic activity (ISL) was analysed, in an attempt to significantly Since 2003, the Geodynamic Laboratory at Książ enhance the orbital solution. The ISL provides (LGK) has been using its new tilting instruments precise range and range rate measurements (not to register observations of tectonic activity. Water affected by atmosphere) between satellites in a tube tiltmeters (WT) consist of two, long (65.24 specific constellation; this is one of the key requi- and 93.51 m) perpendicular pipes, half-filled with rements for improving the reliability of positio- water that are designed to record the tilting of ning and time transfer. It can also be a great con- foundations and vertical displacements of indi- tribution to on-board data processing and a step vidual sectors and their ends (Figure 57). The ana- towards autonomous GNSS constellations. lysis of observational data collected using WTs can indicate strong, non-periodic tectonic effects with an amplitude at least one order of magnitude larger than tidal effects (Figure 58). Topographical, geomorphological and geological analyses of the Książ massif and its environment suggest that the direct cause of tectonic activity recorded by the WT method are mutual displa- cements of its 'southern fault' wings, which are al- so monitored by the analysis of the vector bet- ween two GPS stations (KSIA and KSI1), located on opposite wings of this fault (Figure 59).

Fig. 56. Simulated Galileo constellation. Special attention was paid to the analysis of non- gravitational forces due to solar radiation, and the Earth's visual and thermal radiation. In particular, observed fluxes, taken from the Clouds and the Earth's Radiant Energy System database, were used to verify existing NGP models and identify areas of potential improvement. Fig. 57. Horizontal sliding of the southern fault is This research meets the objectives of the Euro- transformed into vertical movement and tilting of the pean Space Agency with respect to the proposed foundations of the mass blocks. evolution of Galileo. It has resulted in the deve- lopment of a bespoke software package that com- bines recent theory, models and data to perform realistic simulations of GNSS satellites in orbit. We expect to update the core features of this soft- ware in the future, paving the way for more advan- ced GNSS data processing – especially near real- time analyses of observation data and verification of modern techniques that can potentially be used in next-generation positioning and navigation sys- tems. Fig. 58. Strong, non-periodic tectonic signals recorded by WTs (raw observations from both WTs). (M. Kalarus, T. Kur, J. B. Zieliński)

90 Fig. 59. Geological situation of the surroundings, location of laboratory instruments and the KSIA & KSI1 GPS stations located on the opposite wings of the southern fault. Displacements of its wings are shown by the red, green, and grey arrows. The most likely cause of tilting effects and vertical time series, and after filtering for high-frequency movements of rock blocks within the Książ mas- effects (up to several tens of minutes). This func- sif are friction forces created by the difference in tion and it's derivative describes the change in travel speeds between the wings of the southern deformation of the Książ massif over time – in fault. These secondary displacements are several other words, its dynamics. orders of magnitude smaller than the relative Two GPS stations were set up near the Geody- displacements of the wings of the southern fault. namic Laboratory in Książ because the main force To investigate the phenomena in more detail, we driving kinematic activity in the Świebodzice De- defined a smooth curve, called the Tectonic Acti- pression is horizontal crustal movements (Figure vity Function (TAF), obtained after removing ti- 57) and the LGK is not equipped with instru- dal and water evaporator signals from the WT raw ments able to measure it. Instruments at both sta-

Fig. 60. The horizontal velocity vector between KSIA and KSI1 GPS stations represents the relative mean velocity of mutual displacement of the wings of the southern fault (based on 2013–2016 time series).

91 tions were applied to determine relative displa- vals in which arrows are pointing up represent cements of the wings of the southern fault, which periods when both wings of the fault are pressed are clearly seen in the morphological form of against each other, downward arrows indicate Pełcznica river valley (Figure 59). The analysis when they are 'disengaged'. Red arrows show assumes that horizontal displacements of the periods when the southern wing was ahead of the KSIA station are representative of movements of northern wing, while green arrows show the the northern wing of the southern fault, and dis- opposite. These results also show that the two placements of the KSI1 station reflect move- wings work as a scissor (alternating) system, with ments of its southern wing. clearly marked periods when they engage and Analyses of three-year observational series of the disengage. There are also some coincidences bet- KSIA–KSI1 vector indicate that mutual hori- ween GPS vector residuals and WT observations. zontal displacement of both wings is currently So far, the best results are obtained for differences around 0.2–0.3 mm/year (Figure 60), suggesting in the channels of each instrument (dotted blue that the southern fault is active. and red lines in Figure 61). By way of comparison, results obtained from WT Our work shows that the best coincidence is instruments and residuals of GPS solutions were observed for epochs in which GPS residuals transformed into the local reference frame of the change direction, and when their values are largest southern fault: in particular, its tangent and per- (Figure 61). The analysis seems to confirm the pendicular components. These residuals are sho- thesis that the direct cause of tectonic activity wn as red and green arrows in Figure 61. The hori- recorded by WTs are mutual displacements of the zontal axis in this figure represents both the wings of the southern fault. southern fault line and the time axis. Time inter-

Fig. 61. Comparison of GPS residuals with TAF for each WT instrument for 2013–2016 time series. (R. Zdunek, M. Kaczorowski, R. Wronowski, D. Kasza)

Examples of tectonic activity of the Świe- ments. The measurement system of the Geodyna- bodzice Depression orogen in the context of mic Laboratory in Książ, associated with instru- tragic events in the Lower and Upper Silesian ments situated on the rocky blocks separated by mining areas faults, is a natural detector of tectonic activity, As was previously presented in yearly reports, allowing to determine the temporal functions of changes in the stress field in Świebodzice Depres- tectonic activity (TAF) with sub-micrometric sion unit (ŚU) area are the reason of complex va- accuracy. Ten years long comparison of the TAF riations of the rock blocks kinematics consisted and their derivatives with seismic shocks in the of rotations and horizontal/vertical displace- Lower and Upper Silesia indicates that earth-

92 quakes occurred during special and repeatable conditions of the ŚU kinematic activity. The investigations of tectonic phenomena are de- dicated to increase security of mining works, exe- cuted in Upper and Lower Silesian mining areas. Determination of the temporal susceptibility of the orogeny to destruction defines periods of high risk of seismic events. The results of precise analysis of seismic events from years 2006-2018 confirmed existence of the time relation between function of derivative of the tectonic activity Fig. 63. Plots of derivatives of TAF and three tragic (TAF) i.e. susceptibility of the orogeny to destru- seismic events which occurred in the cuprum mines: the ction which is the reason of the earthquakes. OZG "Rudna Główna" 4.3 Mag., (17 September), "Lubin OZG " 3.1 Mag., (3 October) and OZG "Rudna Główna" On the Fig. 62, 63 and 64 there are presented three 4.4 Mag (29 October) (2 victims) in 2016. tragic seismic events in Upper and Lower Silesian As well as in the case of seismic event in the Wujek mining areas in the years 2015-2018. The figures mine (17 April 2015) the earthquakes occurred in contain fragments of plots of derivatives of tec- 2016 at the epoch when derivatives of TAF also tonic activity functions at the moments of tragic fulfilled necessary conditions before earthquake earthquakes. (see Fig. 63). On Fig. 63 are visible two interesting moments in 6 November and 17 November when necessary conditions for earthquake were also ful- filled but it did not result any seismic events in the Lower Silesian area. Otherwise, in the same time seismic events happened in the Czech and Upper Silesian mining areas (Fig. 63.). This fact strengt- hens the thesis about large-scale, homogeneous field of tectonic forces which, at the same time, covers the ŚU as well as the Lower and Upper Sile- sian areas. The credibility of this thesis is inde- Fig. 62. Plots of derivatives of TAF during very tragic pendently confirmed by the results of many years seismic event 4.0 Mag., in the KWK „Wujek” (17 April long measurements of the Earth crust motions, 2015) (2 victims). performed on hundreds of stations by the space The earthquake in the coal mine "Wujek" from 17 and satellite techniques i.e. GNSS, SLR, DORIS, April 2015, occurred at the moment of significant VLBA; which were used to develop the global decreasing of kinematic activity of the orogeny model of tectonic plate velocities, ITRF2008. of the Świebodzice Depression (Fig. 62.). In 5 May 2018 in the coal mine KWK „Borynia - At the same time the signs of derivatives of TAF Zofiówka-Jastrzębie” occurred very tragic seismic were changed on four measure channels less than event. Five miners were killed and two miners hundred hours before. were injured. This earthquake happened during Variations of the signs of derivatives as well as di- epoch of double and high symmetry between sappearance of the kinematic activity (small velo- derivatives of TAF (see Fig. 64). In short time city of deformations of orogen) define necessary before seismic event derivatives of TAF change conditions which must be fulfilled before earth- their signs for all measure channels. Results of the quake (CBK PAN Report 2017). In 29 November, comparative discussion between moments of 2016, occurred very tragic seismic event of ma- earthquakes and epochs of symmetry describe gnitude 4.4 in Richter scale in the depth 1 km in particular meaning of these states in the process the cuprum mine „Rudna” (Lower Silesia). Eight of triggering seismic event. About ten percent of miners were killed and twenty one were injured. seismic events took place during epoch of This earthquake was perceptible by habitants 40 symmetry of derivatives of TAF. km far from the epicenter.

93 Fig. 64. Plots of derivatives of tectonic activity functions (TAF) and tragic seismic event which occurred in the coal mine KWK „Borynia -Zofiówka-Jastrzębie” 4.1 Mag., (5 May, 2018) (5 victims). (M. Kaczorowski, M. Rudnicki, R. Zdunek, D. Kasza, R. Wronowski, M. Gadomski)

SPACE MECHATRONICS AND ROBOTICS (LMRS-Space Mechatronics and Robotics Laboratory) Formation of vesicles within the fusion crust of eucritic meteorites Cosmic objects entering a planetary atmosphere We are examining five eucritic meteorites: QUE reach a very high temperature, as a result of hy- 97014, EET 92003, BTN 00300, PCA 91007 and pervelocity collisions with air molecules. The GRA 98098. All samples have a preserved fusion outermost part of these objects completely melts crust, with numerous round vesicles (Fig. 65). The and, during cooling, is transformed into glassy process that is responsible for their formation is layer, usually 100–1000 mm thick, named the not fully understood and we tested a hypothesis fusion crust. Vesicles are a characteristic feature that variability in troilite content is the source of of the fusion crust. On microscopic images they variability in their number. look like round, empty objects with different sizes and densities. One hypothesis is that they are formed by “exsolution of volatile components from the silicate melts” due to high temperatures. The aim of our work is to explain the mechanism of vesicle formation within the fusion crust of eucritic meteorites (stony basalt meteorites, likely originating from asteroid Vesta-4) by means of microscopic observation, laboratory experiments and numerical modelling. The aim is to improve our understanding of the interaction of bolides with the atmosphere, and determine the amount of volatiles delivered to past and present atmo- spheres of terrestrial planets by cosmic particle flux. In order to determine the vesicle formation Fig. 65. Vesicles observed in the fusion crust of GRA 98098. mechanism, it is necessary to quantitatively deter- mine the level of vessicularity of the crust.

94 Table 2. Fusion crust parameters in studied meteorites. QUE EET BTN PCA GRA We characterized the fusion curst of 97014 92003 00300 91007 98098 percentage these meteorites in terms of the quan- 42.25 33 27 24 5 tity and size of their vesicles [Table 2]. of bubbles in FC / % Statistical parameters were determined average vesicles radius / µm 11.75 11 14 10 12 by custom-made Matlab code desig- vesicles radius 33.25 39 63 39 35 ned [Fig. 65]. The geochemical com- smaller than average / % position of bulk rock and the fusion vesicles radius 59.25 60 37 61 62 crust was determined by an electron bigger than average / % microprobe (CAMECA SX 100) at the the thickness of fusion crust / µm 138 157 152 170 255 Polish Geological Institute in Warsaw. This identified troilite crystals in the avg S content in bulk rock / wt.% 0.024 0.017 0.004 0.011 0.072 interior, and the percentage surface avg S content in fusion crust/wt.% 0.052 0.012 0.005 0.010 0.026 area covered by troilite was correlated Troilite area % 0.113 0.100 0.264 0 0.025 with specific fusion crust parameters. Sulphur is the most obvious volatile component, Our analysis suggests that troilite is not a main and this could have been exsoluted from silicate factor in the process of forming vesicles, as its melts at high temperature; however, we found content does not correlate with the percentage of that its presence was not correlated with vesicles the crust covered by vesicles. Interestingly, the either in bulk rock or the crust. Moreover, some amount of vesicles in the crust does correlate with areas near the crust contain much more sulphur the crust's thickness (orange dots in Figure 66). than surrounding grains. Although we do not fully understand the process, SEM analyses of all samples found differences in we suspect that thickness of the crust may be the location and size of troilite crystals. The per- related to the meteoroid's surface temperature du- centage of troilite was used to estimate the amo- ring its passage through the atmosphere. Dif- unt of troilite present in the crust before it melted. ferences in temperature might have led to slight This found no correlation with areas covered by variations in the viscosity of melted material, vesicles (blue dots in Figure 66). Furthermore, which had an impact on expanding and escaping vesicles are distributed uniformly across the curst volatile elements. This could potentially explain and are very close to each other, unlike troilite cry- the smaller volume of vesicles in thicker crusts. stals, which are located some distance from each Our work is ongoing: the project started in 2016 other with an irregular distribution. and funding was provided for three years by the Polish National Science Academy. (A. Nicolau-Kuklińska) Mathematical model of a landing on Phobos – the LOOP project In 2017, the Centrum Badań Kosmicznych PAN and AGH submitted a project proposal to develop a mathematical model of a landing process under the PIIS program. The proposal was accepted and, at the end of 2017, the LOOP project was launched. In 2018, the LOOP team conducted an in-depth review of the literature in order to define requirements for future modelling and testing. In the next step, two testbeds (the FBT; Falling Box Testbed and the FCT; Falling Cone Testbed) were Fig. 66. Relation between the percentage of the crust covered by vesicles and: 1) the percentage of troilite in the designed, manufactured and tested. At the begin- unmelted part of the meteorite (blue); and 2) the ning of 2019, commissioning of both devices will thickness of the crust (orange). be completed and the test campaign will start.

95 Efficient landing algorithms and robust lander purposes – the first is the creation of a simplified mechanical designs will be an important part of engineering model that should be easy to imple- any successful future endeavours. Past, ongoing ment in control systems, and the other will take the and proposed landing missions have made it clear form of ready-to-use simulation tool in the that the landing process itself is crucial for the MATLAB/Simulink environment. entire project to succeed. There is no doubt that Project members are drawn from two leaders in missions such as Phootprint will gain a lot from their scientific fields. The CBK PAN has broad the outcomes of our project, which we call LO- experience in laboratory microgravity simulations OP (Landing Once On Phobos). The origin of and mathematical modelling. The AGH is a the name lies in the fact that, during our work on pioneer in the field of geology, mining, geophy- the REST project (Robotically Enhanced Surface sics and engineering in general. We believe that the Touchdown) the team realized that an empirically- synergy between these two entities will be the key valid mathematical model of the contact would be to the success of the proposed project. a valuable tool in various projects. Such a model should, in our opinion, be developed hand-in- hand with its counterpart in the form of a full la- boratory model. As the idea emerged from a pro- ject to land on Phobos, this tiny celestial body ga- ve its name to our activity. The project is directly concerned with Phobos, but the results will be generalizable to landing on other celestial bodies. The mathematical model will be adapted to serve two engineering Fig. 67. The LOOP project logo. (T. Barciński, J. Baran)

96 APPLICATIONS

(The Earth Observation Group) The Department of Earth Observation specialises in remote sensing and geographic information systems. The group has been active in European projects, notably the 7th Framework Programme, H2020, pre-accession European Space Agency PECS programs, together with domestic research programs. The Department has developed innovative applications, software and algorithms. Sentinel-2 Global Land Cover classifi- improved when training data were extracted from cation multiple databases. The project has generated several important Duration: 1 February 2016 findings, notably: – 31 January 2018 • algorithms for the automatic production of GLC maps based on Sentinel-2 data; • software tools for classification, including The European Space Agency's Sentinel-2 Global batch processing; and Land Cover (S2GLC) project provides tools and a • land cover maps for prototype sites that de- roadmap leading to the automatic development monstrate the capabilities of the developed and update of a GLC database based on Sentinel- tools. 2 data. Five prototype sites, on four continents, The project consortium included research insti- have been defined. They include two European tutions and companies with experience in global, 2 countries: Germany (360 000 km ) and Italy (300 pan-European and regional land cover (LC) clas- 000 km2); a 200 000 km2 area in China (Asia); an sification. It was headed by the Centrum Badań area covering 200 000 km2 in Colombia (South Kosmicznych PAN, and included IABG mbH, America); and an area of 220 000 km2 in Namibia Friedrich Schiller University Jena and EOXPLO- (Africa). RE UG. Given the spatial resolution of Sentinel-2 data (10 × 10m), and the need to automate the classifi- cation process, one of the most important and challenging parts of the project was the genera- tion of a reference database to serve as a founda- tion. The most detailed and reliable open access GLC databases are only available at a maximum spatial resolution of 300 × 300m. The project ad- dressed this problem by departing from the com- mon assumption that highly-accurate results can only be obtained from highly-accurate reference data. Our investigations showed that even with moderately imperfect reference data (provided by lower-resolution GLC databases) it is still possible to obtain results with high overall accuracy. Con- sequently, existing databases were used as the primary source of training data for the Sentinel-2 classification methodology. A supervised pixel-based classification method was selected due to its accuracy, preservation of detail and efficiency. Among the various methods used to analyse multi-temporal data, aggregating the results of multiple classifications of single- date images was found to be the most reliable, due to changing cloud conditions in different parts of the globe. A second finding was that results were Fig. 1. S2 Land Cover Maps of the project test sides.

97 Project website: http://s2glc.cbk.waw.pl/ In order to fully automate the process, the pro- The initial project has been extended and the prietary, cloud-based distributed computing ma- CBK PAN plans to classify the whole of Europe nagement system CalcManager was created. This using the CreoDias infrastructure. In 2018, the system makes it possible to manage work both in classification strategy was modified to use Corine the cloud and on workstations. LC and HR layers as reference databases. Clas- (St. Lewiński, R. Malinowski, M. Rybicki, sification is planned for 2019. E. Gromny, M. Krupiński, M. Jenerowicz, C. Wojtkowski)

BAMS-Mazovia – Built-up Area Monitoring Service for Mazovia Duration: 18 September 2018 – 17 September automating the identification of areas that may 2020 have changed. The goal is to accelerate the pro- The main goal of the BAMS-Mazovia project is to cess of updating existing databases and reducing develop a platform that can provide reliable infor- maintaining costs. mation on changes occurring in built-up areas. The current study area is Mazovia Province – the The service will be based on Sentinel-2 imagery largest and most populated of the Polish provin- and information provision will be fully automa- ces. In the longer term, the aim is to develop a ted, using image classification algorithms. A high methodology and tools that can be easily applied level of detail is required, and this will ensured by in other provinces of Poland. the application of multi-temporal observations The project consortium consists of GEOSYS- from the Sentinel-2 constellation, and the use of a TEMS Polska Sp. z o.o. (project leader) and the dedicated classification workflow developed by Department of Earth Observation of the Cen- the CBK PAN. trum Badań Kosmicznych PAN (research part- The platform will be used to compare image ner). classification results with existing databases, such (R. Malinowski, S. Aleksandrowicz, M. Jenerowicz, as the Database of Topographic Objects (Baza M. Rybicki, St. Lewiński, C. Wojtkowski) Danych Obiektów Topograficznych), with the aim of

Remote Sensing Analysis of Landforms in Isidis Planitia, Mars Duration: 1 January 2018 – 31 December 2019 dataset, the semi-automatic extraction of structu- In 2018, the project's goal and scope were deter- res of interest based on the use of mathematical mined, namely: to develop a semi-automatic algo- morphology operators and, finally, creating libra- rithm to analyse characteristic landforms in Isidis ries of spatial parameters for extracted structures. Planitia on Mars. The current scope is preliminary These studies will help us to understand the ori- processing of imaged data and the analysis of gins of Isidis' characteristic cones. Understanding structures of interest, i.e. the detection of arcuate their spatial distribution will enable us to determi- ridges and aligned cones, and the classification of ne the pattern governing their arrangement. No- detected landforms as a function of their spatial tably, a characteristic feature is their linearity and features. arcuateity, which is a geological scientific problem. Preliminary activities consist of the selection of This study is being carried out in cooperation with the input dataset. For analysis purposes, a set of the Centre's Dynamics of the Solar System and high- resolution optical data (2m spatial resolu- Planetology Department (Zakład Dynamiki tion) acquired by a stereoscopic camera on the Układu Słonecznego i Planetologii) under the Mi- European Space Agency Mars Express mission nistry of Science and Higher Education's grant (the High/Super Resolution Stereo Colour Ima- for the development of young researchers and ger) was selected. doctoral programme participants. Participants are The planned next steps are as follows: the chara- selected via an internal competition. cterisation of structures of interest from a limited (M. Jenerowicz, N. Andrzejewska)

98 Evaluation of the usefulness of multifractal formalism in the processing and analysis of optical remote sensing images Duration: 20 July 2017 – 19 July 2020 describing remote sensing data; The scientific goal of this study is to analyse opti- - verification of whether multifractal scaling is cal remote sensing images using an advanced mul- found in high-resolution data recorded in dif- tifractal formalism. Consequently, in 2018, a series ferent wavelength ranges; of systematic and comprehensive analyses of - a comparative analysis of the methodology ba- multifractal characteristics of different kinds of sed on local multifractal features and mathema- optical remote sensing images were carried out. tical morphology operators. The main research milestones achieved last year This study is being carried out under Opus project were: no. 2016/23/B/ST10/01151, funded by the Na- - the implementation and ongoing development tional Science Centre. of multifractal analysis methods, in the context of (M. Jenerowicz, A. Wawrzaszek) Vertical distribution of cloud amount over Poland Historically, climatologists have found it difficult profiles was almost equal: 548 profiles (day), vs. to access reliable information on vertical cloud 535 profiles (night). structure. This is because both surface-based ob- The study found that the sky over Poland is domi- servers and imaging/ sounding satellite sensors nated by low-level cloud (33–35% at an altitude of have limited capability to report superposed clo- 1–3 km), while cloud amounts at 5–10 km altitude ud. However, lidar–radar cloud profiles have ope- are relatively constant (20%). Low-level cloud is ned up new research opportunities. found to have the greatest seasonal (20% in July, Lidar and radar active sensors offer an alternative 50% in January) and diurnal (30% daytime, 40% to imaging and visual techniques. This instru- night-time) variability. Uncertainty in the estimate mentation emits radiation pulses that can pene- of mean cloud amounts is shown to vary as a fun- trate cloud. The strength and time of arrival of the ction of the number of profiles analysed, notably returning (backscattered) signal provides a vertical the time-window used for data averaging. Uncer- cloud profile – hence the name: profiling lidar and tainty (measured as the width of the 95% confi- profiling radar. dence interval) ranged from a minimum of ±2% Cloud climatologists are particularly interested in for the annual mean, to a maximum of ±10% for spaceborne active instruments, as these tools are monthly means. able to probe the Earth's cloud regimes. In 2006, The analysis demonstrated that uncertainty of CloudSat and Cloud–Aerosol Lidar and Infrared below ±1% for the annual mean was only achie- Pathfinder Satellite Observations (CALIPSO) vable if data was averaged over an area of 1300 satellites were launched into a common orbit. This km2. A further finding was that surface-based ob- dataset was explored to provide the very first servers in Poland are usually unable to determine analysis of vertical cloud structure over Poland. whether there are high-level clouds (up to 64% of A vertical cloud amount profile was calculated for the time), as these clouds are obscured by clouds at each CloudSat–CALIPSO pass/ transect over lower levels. Similarly, middle-level clouds cannot Poland. A total of 1083 joint CloudSat– CALI- be observed 55% of the time. These findings lead PSO profiles (transects) were analysed, covering to the conclusion that CloudSat–CALIPSO ob- the period June 2006 to April 2011. The availa- servations remain the most reliable source of data bility of monthly data varied, with a total of 110 on cloud vertical structure for Poland. profiles for the five October months, compared to For details see: Kotarba A.Z. (2018). Vertical profile a total of only 60 profiles for the five August of cloud amount over Poland: variability and uncertainty months. Similarly, within a particular year, the based on CloudSat-CALIPSO observations. Interna- monthly availability of data varied widely (e.g. tional Journal of Climatology, 38, 4142–4154, from 6 to 27 profiles in 2008 and 2009). On the doi:10.1002/joc.5558. other hand, the number of day and night-time

99 Fig. 2. Change in mean cloud amount at different altitudes. Values are calculated as running averages applying a time window of ±15 days (a), ±30 days (b), and ±45 days (c). (A. Z. Kotarba)

THE CRISIS INFORMATION CENTRE The mission of the Crisis Information Centre (CIK) is to vices and crisis management institutions regar- make rescue operations and crisis management activities ding the use of geoinformation and satellite ap- more efficient through the effective use of existing geospatial plications; information technologies and the development of new me- • providing geoinformation support to the State thods and tools – in particular, satellite-based applications Fire Service, Polish crisis management insti- and the organisation of demonstrations and training focu- tutions and non-governmental organisations; sed on new solutions. • organising training and simulations focused on The CIK combines scientific expertise in the field the effective use of new technologies; and • of satellite applications with an end-user pers- demonstrating and testing the usefulness of pective. The CIK's operational activities include: pre-operational technical solutions via table top • providing expert advice to Polish rescue ser- and field exercises.

100 Earth Observation for Sustainable Development – Eastern European Partnership namely Armenia, Georgia, Poland and Moldova. Duration: 1 July 2016 – The project's activities resulted in the develop- 3 October 2018 ment of six products and services in the field of agriculture and water management, including The project forms part of the European Space flood protection. End-users in Armenia and Agency's Earth Observation for Sustainable De- Georgia were provided with an agriculture produ- velopment initiative aimed at the Eastern Euro- ctivity monitoring service and a statistical crop pean Region. The Crisis Information Centre mapping service. Four products concerned (CIK) led the consortium, which consisted of the Poland: a river ice monitoring service, seasonal following Polish and Czech organisations: Astri biomass change monitoring, land cover maps and Polska Sp z o.o., Geosystems Polska Sp. z o.o., the production of elevation data. The final out- GeoPulse Sp. z o.o., Gisat s.r.o. and the Polish comes were presented and handed over to end- Centre for International Aid. users at dedicated meetings in each country. The main aim was to achieve a step increase in the Furthermore, in spring 2018, the CIK organised a uptake of Earth Observation-based environmen- study visit for Moldavian stakeholders, who were tal information in development programs im- able to familiarise themselves with the disaster risk plemented by the World Bank and European management system in Poland with a particular Investment Bank in Eastern Europe; in particular focus on flood protection practices. it sought to support collaboration and knowledge More information is available on the project's exchange among Eastern Partnership countries, website: http://eo4sd-eastern.eu/.

Fig. 3. River ice monitoring service. Credit: Astri Polska for the ESA/World Bank. (M. Milczarek, J. Ryzenko) DRIVER+ Duration: 1 May 2014 – - create a pan-European testbed for crisis manage- 30 April 2020 ment stakeholders, in the form of virtually-con- nected facilities and labs for crisis exercises and The main aims of the DRIVER+ (DRiving Inno- simulations; Vation in crisis management for European Resi- - launch a portfolio of solutions, including a data- lience +) project are to:

101 base-driven website to record all available soft- During the project, four trials will be organised to ware and hardware tools, operational concepts evaluate new crisis management solutions in va- and other resources used in crisis management si- rious European countries, each with a different tuations; focus on the needs of crisis management stake- - create a shared, European understanding of cri- holders. sis management, through the enhancement of the In 2018, the methodology for the preparation, cooperation framework. execution and evaluation of these trials was deve- DRIVER+, funded under the European Union's loped and then implemented. It was subsequently 7th Framework Programme, is the largest colla- tested in two initial trials held on 21–25 May in the borative crisis management project in the security Main School of the Warsaw Fire Service, and domain. It brings together 31 partners from 14 22–26 October in the European Centre for Risk countries. Stakeholders who have already com- Simulation located at L'Entente pour la forêt mitted to the project, or plan to join include end- Méditerranéenne (Valabre) in France. users, solution providers, researchers, policyma- More information is available on the project's kers, practitioners and NGOs. website: http://www.driver-project.eu/ (A. Foks-Ryznar, J. Ryzenko, K. Trzebińska, J. Tymińska, E. Wrzosek) Sat4Envi

and the planning and analysis work carried out by Duration: 1 December 2017 – crisis management institutions and rescue ser- 30 November 2020 vices; - the development and implementation of a trai- The Sat4Envi project (Operating system for ning program for users in the field of crisis mana- sharing and promotion of digital satellite infor- gement and rescue, including the acquisition, mation about the environment) has been imple- analysis and use of satellite data; and mented by the Institute of Meteorology and Wa- - providing support to users in accessing and in- ter Management, a National Research Institute, in terpreting data, as a part of the Customer Service cooperation with the Centrum Badan Kosmicz- System platform, with particular emphasis on cri- nych PAN, the Academic Computer Centre (CY- sis management and rescue. FRONET AGH) and the Polish Space Agency In the first year of the project (2018), the follo- (POLSA). The project is funded under the Opera- wing milestones were reached: tional Programme, Digital Poland 2014–2020. - development of the basic concept of how the The main purpose of the Sat4Envi project is to MCS will function; supply satellite data from the Copernicus pro- - development of the initial version of the Custo- gram, together with data from other environ- mer Service System platform for users from crisis mental and meteorological satellites. management institutions and rescue services; The CBK PAN is responsible for: - roll-out of a series of MCS pre-activation and - creating the Mobile Satellite Data Analysis Cen- pilot training sessions; and tre (MCS), which will provide operational support - development of informational and promotional for the use of satellite data during emergencies, materials, and their distribution among users.

(W. Hodowicz, T. Borkowski, A. Foks-Ryznar, M. Milczarek, A. Robak, J. Ryzenko, E. Woźniak, E. Wrzosek)

102 The Heliogeophysical Prediction Service Laboratory

The Heliogeophysical Prediction Service nowcasting of regional ionospheric conditions (HPS) Centre is part of the global In- over Europe, East Asia and Australia is also avai- ternational Space Environment Service lable. The HPS Centre provides the W-index over (ISES). It is responsible for mea- Europe based on European Geostationary Navi- surements and predictions of solar acti- gation Overlay Service ionospheric maps ob- vity and related Earth phenomena. tained from global navigation satellite system (GNSS) measurements. The same analysis can be The ISES is an international organisation that co- obtained using data from the Russian System for ordinates the rapid exchange of parameters con- Differential Corrections and Monitoring messa- cerning the Sun, the Earth and the Earth's envi- ges via GNSS observations. This will make it pos- ronment between participating observatories. sible to show plasma flow from the eastern region, The Warsaw centre has a special status as a Regio- which can be used as a fast warning for Polish nal Warning Centre (RWC). The Centrum Badań GNSS users. Kosmicznych PAN exchanges data with other In 2018, we carried out a structural analysis of the Warning Centres, and receives large amounts of spatial correlation of ionosphere characteristics at data from national observatories in different measurement points obtained from a single sta- countries. Data from Polish observatories are also tion and, therefore, ionosonde and recorded GPS collected. Together with the Geophysical Institute signals. The critical frequency of the foF2 layer of the Polish Academy of Sciences, the Warsaw and Total Electron Content (TEC) data were Centre provides data from the polar region (pro- analysed during ionospheric quiet and disturbed vided by the Polish Polar Station in Hornsund). conditions based on the ionospheric slab thick- Ionosonde data is completed by riometers and ness model. Kriging uses geostatistical techniques scintillation measurements. A special daily bulle- to calculate the autocorrelation between data tin (URSIGRAM Warsaw) is published and bro- points and is based on weighted averages, where adcast to ISES members. weights depend on separation distances provided The Ionospheric Despatch Centre, which is part directly by the semivariogram. Our results (Fig. 4) of the European web service, provides online indicate that the radius of the spatial correlation access to a database of critical frequency F2 iono- for GPS data between ionospheric stations should spheric layer forecasts for all sites. Continuous be no more than 120–300 km.

Fig. 4. Semivariograms during quiet (left) and disturbed (right) ionospheric days (01.03.2012 and 30.09.2012) for the Warsaw GPS station; time 06 – 09 UT.

103 The CBK PAN’s Ionosphere model In 2018, the CBK PAN's assimi- lated ionosphere model Helgeo2PT (H2PT) became operational, and has been used as source of total ele- ctron count (TEC) maps for GA- LILEO monitoring. The model in- cludes global navigation satellite sy- stem observations, bottom vertical and, if possible, oblique sounding. The structure of the algorithm also makes it possible to add data from oblique sounding to satellites with onboard beacons. Current data in- clude the electron density profile obtained directly from ionospheric sounding and assimilated upper profiles calculated from other mea- surements. The H2PT is an empi- rical model, which means that TEC maps are restricted by data availabi- lity and mapping function efficien- Fig. 5. Sample TEC map from the H2PT model. cy. A new website to check H2PT status In 2018, a system to check the status of the H2PT and generates a message in the case of a problem. model was created. This makes it possible to There is also an option to send an email with detect any errors that may arise when creating automatically-generated links to files containing output products. The site shows the hourly status, an error. A test website showing MUF and LUF maps Another new website was developed to show the cluding signal-to-noise ratios at recommended output of MUF (Maximum Usable Frequency) frequencies. It provides a database of operational, and LUF (Lowest Usable Frequency) mapping data-driven models and can produce messages programs. There are currently two MUF maps: and files tailored to user requirements. the first is the NeQuick model, indicating iono- An improved version of the Trasy 6.0 software has sondes from which data is taken to generate cor- been designed to estimate the best frequencies for rected maps; the second is the map after cor- communication between two antennas in the recting for MUF values. range 2–30 MHz based on their energetic gain, The CBK PAN provides forecasts of high- power and coordinates. The software is able to frequency radio signal intensity to governmental provide a daily forecast of frequency of trans- and commercial communications based on the mission, and lowest and maximum usable freq- software packages it has developed. The HEL- uencies. Trasy 6.0 also estimates signal-to-noise GEO package is an automatic system for solar- ratios and basic circuit reliability; it can provide a geophysical data processing and solar-geophysical monthly forecast and the user can choose antenna forecasting. The Ray-Route system forecasts coordinates. high-frequency communications' conditions, in-

104 Fig. 6. Screenshot of the website showing MUF and LUF maps.

Fig. 7. The on-line software package Trasy 6.0.

The Ionospheric Weather Expert Service Centre The Ionospheric Weather Expert Service Centre PAN's facilities continuously detect changes in the provides support to the European Space Agency's signal at a fixed frequency of 30 MHz. A decrease Space Situational Awareness Space Weather Seg- in the signal indicates absorption and can be inter- ment (SSA SWE) network, notably in the form of preted as an increase in ionization in the iono- the observation, monitoring, interpretation, mo- sphere. delling and forecasting of ionospheric and upper Measurements from the Borówiec station (52° 16' atmosphere weather conditions. 37.2” N; 17° 04' 28.56” E, near Poznań) show Within the framework of the Agency's 'Ionosphe- absorption in the ionospheric D-region. Data are ric Weather' project, the HPS Centre developed a displayed as time series and made available as a new service called RIO, which provides riometer text file. The default time resolution of measured data from its Borówiec and Hornsund stations. riometer data is one second and the longest avai- The Riometer (Relative Ionospheric Opacity Me- lable time resolution is one minute. Measurements ter for Extra-Terrestrial Emissions of Radio no- are available in their raw format (Volts) and as ise) instrument quantifies the amount of electro- relative (dB) data. magnetic wave ionospheric absorption in the High-frequency communication is crucial, espe- atmosphere, and riometers installed at the CBK cially in polar regions where ground infrastructure

105 and satellite coverage are limited. Here, riometer surements from its Hornsund (77° 00' N; 15° 33' data are an important indicator of absorption. In E, Svalbard) station. Hornsund data are only operational conditions, they can be used as a sour- available in raw format (Volts) for demonstration ce of alerts for ionospheric D-region absorption purposes, and measurements cover a short period and loss of communication. of time. Moreover, the equipment has been dama- The CBK PAN, in cooperation with the Polish ged by reindeer and no measurements are curren- Institute of Geophysics provides riometer mea- tly possible. Product name: Borówiec riometer Hornsund riometer (demonstration) Geographic coverage (bounding ±200 km from the ±200 km from the riometer box) riometer position position 52° 16' 37.2” N; 17° 04' 77° 00' N; 15° 33' E 28.56” E On event/ periodically/fixed Continuous Fixed dataset dataset for demonstration measurements Temporal resolution 1 min 1 min Latency 15 min Only archive data Data formats (image, ASCII, meta image, ASCII, meta image, ASCII, meta data data) data Archive (yes/no) yes yes

Fig. 8. Screenshot of RIO riometer data from Borówiec and Hornsund.

106 Fig. 9. RWC Warszawa daily solar activity report in VOEvent format. Within the framework of the EUROPLANET RWCs were required to prepare messages manu- project, RWC Warszawa has updated its warning ally (each message/ alert had to be reviewed by a system by implementing VOEvent technology. technician), which confused users who received This was necessary as the previous system produ- alerts from different sources. The standardised ced messages in text format that were hard to pro- VOEvent format will add value for the space wea- cess with external software. Furthermore, all ther community.

The VESPA DaCHS server

Fig. 10. Output from the DaCHS server.

107 The CBK PAN produces several types of measu- which will increase synergy in data processing rements, including warning messages and data tasks. Currently the Centre plans to share the fol- from active and passive radars that are shared on lowing data on the DaCHS platform: all data ob- the web. Our new VESPA DaCHS technology tained from ionosondes; all messages produced makes it possible to organize these data and make by RWC Warszawa, all products generated by the them more accessible to the scientific community. HPS Centre, and the set of LOFAR PL106 astro- In particular, the ADQL query feature allows nomical observations. users to perform an advanced database search, (B. Dziak-Jankowska, O. Grynyshyna-Poliuga, M. Marek, M. Miłodrowska, A. Pełech, Ł. Tomasik) The Global Navigation Satellite System (GNSS) Observatory in Warsaw MONITORING THE QUALITY OF THE GALILEO SYSTEM Centrum Badań Kosmicznych PAN since autumn 2018 - computation of independent ionospheric is participating in GSA project Galileo Reference Centre- models for different world regions, Member States. This project is designed to enable monito- - computation and monitoring of Key Perfor- ring of the Galileo system by research institutes from EU mance Indicators, countries, independent of the system manager. The main - computation and analysis of the NeQuick-G tasks are: model, which is broadcasted as an ionosphere - computation of independent rapid and precise model in the Galileo navigation message. orbits for Galileo satellites, (A. Świątek, L. Jaworski, Ł. Tomasik, M. Pożoga) MONITORING THE QUALITY OF EGNOS CORRECTIONS CBK PAN is one of the partners in the consor- cludes analysis and visualization of Key Perfor- tium in GSA project EGNOS Service Monitoring mance Indicators (KPI) of the EGNOS system Support. This project performs continuous moni- and a comparative analysis of EGNOS correc- toring of the availability, correctness, continuity tions transmitted directly by satellite and via the and accuracy of the EGNOSSIS (Signal in Space) internet. and EGNOS-EDAS corrections. The project in-

108 Fig. 11. Example of the EGNOS Signal in Space corrections analyses for the Warsaw site.

Fig. 12. Summary of the Horizontal and Vertical Position Error for the last 10 quarters for SIS and EDAS observations.

109 Fig. 13. Differences in horizontal and vertical position components for CSIS and CNET (EGNOS SIS and EDAS corrections) obtained for 95% of daily observables, for satellite PRN123 for the last 10 quarters as a function of the number of observations taken to compute the position. (A. Świątek, L. Jaworski, Ł. Tomasik)

110 PUBLICATIONS

* Total number of publications in 2018: 111 (including 68 in the journals from JCR) * Papers in refereed international and national science journals, books, and proceedings: 43

Papers in refereed international and national 3. Abdellaoui G., J. BŁĘCKI, P. ORLEAŃSKI, science journals and proceedings (JCR): and others 320 authors; Ultra-violet imaging of the night-time earth by EUSO-Balloon towards space- 1. Abdellaoui, G., S. Abe, J. H. Jr. Adams, A. based ultra-high energy cosmic ray observations; As- Ahriche, D. Allard, L. Allen, J. BŁĘCKI, P. troparticle Physics, 61pp, DOI: 10.1016/j. ORLEAŃSKI and JEM-EUSO collabora- astropartphys.2018.10.008, 2018 tion (360 authors); EUSO-TA – First results 4. Amati, L., P. O'Brien, D. Götz, E. Bozzo, C. from a ground-based EUSO telescope; Astroparti- Tenzer, F. Frontera, G. Ghirlanda, C. Labanti, cle Physics, Volume 102, Pages 98-111, DOI: J. P. Osborne, P. ORLEAŃSKI, and others 10.1016/j.astropartphys.2018.05.007, 2018 200 authors; The THESEUS space mission con- 2. Abdellaoui, G., S. Abe, J. H. Adams Jr., A. cept: science case, design and expected performances; Ahriche, D. Allard, L. Allen, G. Alonso, L. An- Advances in Space Research, Volume 62, Issue chordoqui, A. Anzalone, Y. Arai, J. BŁĘCKI, 1, Pages 191-244, Doi: 10.1016/j.asr.2018. 03. P. ORLEAŃSKI and JEM-EUSO collabora- 010, 2018 tion (360 authors); First observations of speed of 5. Arias M., J. Vink, F. de Gasperin, P. Salas, J. B. light tracks by a fluorescence detector looking down on R. Oonk, R. J. van Weeren, A. S. van Ame- the atmosphere; Journal of Instrumentation, sfoort, J. Anderson, R. Beck, M. E. Bell, M. J. Volume 13, Article Number: P05023, DOI: Bentum, P. Best, R. Blaauw, F. Breitling, J. W. 10.1088/1748-0221/13/05/P05023, 2018 Broderick, W. N. Brouw, M. Brüggen, H. R.

111 Butcher, B. Ciardi, E. de Geus, A. Deller, P. C. 10.24423/aom.3009, 2018 G. van Dijk, S. Duscha, J. Eislöffel, M. A. Gar- 9. CIĄŻELA, J., J. Koepke, H. J. B. Dick, R. Bot- rett, J. M. Grießmeier, A. W. Gunst, M. P. van charnikov, A. Muszyński, M. Lazarov, S. Schu- Haarlem, G. Heald, J. Hessels, J. Hörandel, H. th, B. Pieterek, T. Kuhn; Sulfide enrichment at an A. Holties, A. J. van der Horst, M. Iacobelli, E. oceanic crust-mantle transition zone: Kane Mega- Juette, A. Krankowski, J. van Leeuwen, G. mullion (23°N, MAR); Geochimica et Cosmo- Mann, D. McKay-Bukowski, J. P. McKean, H. chimica Acta, Volume 230, Pages 155-189, Mulder, A. Nelles, E. Orru, H. Paas, M. Pan- DOI: 10.1016/j.gca.2018.03.027, 2018 dey-Pommier, V. N. Pandey, R. Pekal, R. Pizzo, 10. Colmenarejo, P., M. Graziano, G. Novellia, D. A. G. Polatidis, W. Reich, H. J. A. Röttgering, Mora, P. Serra, A. Tomassini, K. SEWERYN, H. ROTHKAEHL, D. J. Schwarz, O. Smir- G. Prisco, J. Gil Fernandez; On ground validation nov, M. Soida, M. Steinmetz, M. Tagger, S. of debris removal technologies; Acta Astronautica, Thoudam, M. C. Toribio, C. Vocks, M. H. D. 14pp, DOI: 10.1016/j.actaastro.2018.01.026, van der Wiel, R. A. M. J. Wijers, O. Wucknitz, 2018 P. Zarka, P. Zucca; Low-frequency radio absorption 11. CZECHOWSKI, A., M. Hilchenbach K. C. in Cassiopeia A; ASTRONOMY & ASTRO- Hsieh, M. BZOWSKI, S. GRZĘDZIELSKI, PHYSICS, Volume: 612, Article Number: J. M. SOKÓŁ, J. GRYGORCZUK; Structure of A110, DOI: 10.1051/0004-6361/201732411, the heliosheath from HSTOF energetic neutral atoms 2018 measurements; Astronomy and Astrophysics, 6. Attree, N., O. Groussin, L. Jorda, D. Nébouy, Volume 618, Article number A26, DOI: N. Thomas, Y. Brouet, E. Kührt, F. Preusker, 10.1051/0004-6361/201732432, 2018 F. Scholten, J. Knollenberg, P. Hartogh, H. 12. CZECHOWSKI, A., I. Mann; Dynamics of Sierks, C. Barbieri, P. Lamy, R. Rodrigo, D. Ko- nanodust particles emitted from elongated initial orbits; schny, H. RICKMAN, H. U. Keller, M. F. Astronomy and Astrophysics, Vol. 617, A43 A'Hearn, A.-T. Auger, M. A. Barucci, J.-L. Be- (14pp), DOI:10.1051/0004-6361/2018 rtaux, I. Bertini, D. Bodewits, S. Boudreault, 32922, 2018 G. Cremonese, V. Da Deppo, B. Davidsson, S. 13. Deshapriya, J. D. P., M. A. Barucci, S. For- Debei, M. De Cecco, J. Deller, M. R. El- nasier, P. H. Hasselmann, C. Feller, H. Sierks, Maarry, S. Fornasier, M. Fulle, P. J. Gutiérrez, A. Lucchetti, M. Pajola, N. Oklay, S. Mottola, C. Güttler, S. Hviid, W.-H. Ip, G. Kovacs, J. R. N. Masoumzadeh, C. Tubiana, C. Güttler, C. Kramm, M. Küppers, L. M. Lara, M. Lazzarin, Barbieri, P. L. Lamy, R. Rodrigo, D. Koschny, J. J. Lopez Moreno, S. Lowry, S. Marchi, F. H. RICKMAN, J.-L. Bertaux, I. Bertini, D. Marzari, S. Mottola, G. Naletto, N. Oklay, M. Bodewits, S. Boudreault, G. Cremonese, V. Da Pajola, I. Toth, C. Tubiana, J.-B. Vincent and Deppo, B. J. R. Davidsson, S. Debei, M. D. X. Shi; Tensile strength of 67P/Churyumov– Cecco, J. Deller, M. Fulle, O. Groussin, P. J. Gerasimenko nucleus material from overhangs; Gutierrez, H. V. Hoang, S. F. Hviid, W. Ip, L. Astronomy & Astrophysics, Vol.611, A33 (12- Jorda, H. U. Keller, J. Knollenberg, R. Kramm, pp),DOI: 10.1051/0004-6361/201732155, E. Kührt, M. Küppers, L. Lara, M. Lazzarin, J. 2018 J. Lopez Moreno, F. Marzari, G. Naletto, F. 7. BARYLAK, J., A. BARYLAK, T. MROZEK, Preusker, X. Shi, N. Thomas, J.-B. Vincent; O. Grimm, A. Howard, P. PODGÓRSKI, M. Exposed bright features on the comet 67P/ Churyu- STĘŚLICKI; Simulation of charge sharing in the mov-Gerasimenko: Distribution and evolution; As- Caliste-SO detector; Nuclear Instruments and tronomy and Astrophysics, Volume 613, Arti- Methods in Physics Research Section A: Acce- cle number A36; DOI: 10.1051/ 0004-6361/ lerators, Spectrometers, Detectors and Asso- 201732112, 2018 ciated Equipment, Volume 903, Pages 234- 14. Dybczyński P. A., M. KRÓLIKOWSKA; Inve- 240, DOI: 10.1016/j.nima.2018.05.062, 2018 stigating the dynamical history of the interstellar object 8. BŁĘCKI, J., K. Mizerski; Subtle structure of 'Oumuamua; Astronomy & Astrophysics, Vol. streamers under conditions resembling those of 610, L11, (12pp), DOI: 10.1051/0004-6361/ Transient Luminous Events; ARCHIVES OF 201732309, 2018 MECHANICS, Vol.70 Issue 6, 535-550, DOI: 15. Fulle, M., I. Bertini, V. Della Corte, C. Güttler,

112 S. Ivanovski, F. La Forgia, J. Lasue, A. C. Radio Science, DOI: 10.1029/2017 Rs00 Levasseur-Regourd, F. Marzari, F. Moreno, S. 6310, 2018 Mottola, G. Naletto, P. Palumbo, G. Rinaldi, 20. Hendricks, R. J., F. Ozimek, K. Szymaniec, B. A. Rotundi, H. Sierks, C. Barbieri, P. L. Lamy, NAGÓRNY, P. DUNST, J. NAWROCKI, S. R. Rodrigo, D. Koschny, H. RICKMAN, M. Beattie, B. Jian, K. Gibble; Cs Fountain Clocks A. Barucci, J.-L. Bertaux, D. Bodewits, G. for Commercial Realisations — an Improved and Ro- Cremonese, V. Da Deppo, B. Davidsson, S. bust Design; IEEE Transactions on Ultrasonics, Debei, M. De Cecco, J Deller, S. Fornasier, O. Ferroelectrics and Frequency Control, DOI: Groussin, P. J. Gutiérrez, H. S. Hviid, W. H. Ip, 10.1109/TUFFC.2018. 2874550, 2018 L. Jorda, H. U. Keller, J. Knollenberg, J. R. 21. Herique, A., D. Plettemeier, C. Langec, J. T. Kramm, E. Kührt, M. Küppers, M. L. Lara, M. Grundmann, V. Ciarletti, T. Ho, W. KOF- Lazzarin, J. J. López-Moreno, X. Shi, N. MAN, B. Agnus, J. Du, W. Fa, O. Gassot, R. Thomas, C. Tubiana; The phase function and den- Granados-Alfaro, J. Grygorczuk, R. Hahnel, sity of the dust observed at comet 67P/Churyu- C. Hoarau, M. Laabs, C. Le Gac, M. Mütze, S. mov–Gerasimenko; Monthly Notices of the Ro- Ulame; A radar package for asteroid subsurface inve- yal Astronomical Society, Volume 476, Issue stigations: Implications of implementing and inte- 2, Pages 2835–2839, DOI:10.1093/ mnras/ gration into the MASCOT nanoscale landing platf- sty464, 2018 orm from science requirements to baseline design; Acta 16. Gerig, S.-B., R. Marschall, N. Thomas, I. Astronautica, 27pp, DOI: 10.1016/j.actaastro. Bertini, D. Bodewits, B. Davidsson, M. Fulle, 2018.03.058, 2018 W.-H. Ip, H. U. Keller, M. Küppers, F. Pre- 22. Hollick, S.J., C. W. Smith, Z. B. Pine, M. R. usker, F. Scholten, C. C. Su, I. Toth, C. Tubia- Argall, C. J. Joyce, P. A. Isenberg, B. J. Vasquez, na, J.-S. Wu, H. Sierks, C. Barbieri, P. L. Lamy, N. A. Schwadron, J. M. SOKÓŁ, M. BZOW- R. Rodrigo, D. Koschny, H. RICKMAN, J. SKI, M. A. KUBIAK; Magnetic Waves Excited by Agarwal, M. A. Barucci, J.-L. Bertaux, G. Newborn Interstellar Pickup Ions Measured by the Cremonese, V. Da Deppo, S. Debei, M. De Voyager Spacecraft from 1 to 45 au. I. Wave Proper- Cecco, J. Deller, S. Fornasier, O. Groussin, P. J. ties; Astrophysical Journal, Volume 863, Issue Gutierrez, C. Güttler, S. F. Hviid, L. Jorda, J. 1, Article number 75, DOI: 10.3847/1538- Knollenberg, J.-R. Kramm, E. Kührt, L. M. 4357/aac83b, 2018 Lara, M. Lazzarin, J. J. Lopez Moreno, F. 23. Hollick, S. J., C. W. Smith, Z. B. Pine, M. R. Ar- Marzari, S. Mottola, G. Naletto, N. Oklay, J.-B. gall, C. J. Joyce, P. A. Isenberg, B. J. Vasquez, N. Vincent; On deviations from free-radial outflow in A. Schwadron, J. M. SOKÓŁ, M. BZOWSKI, the inner coma of comet 67P/ Churyumov– M. A. KUBIAK; Magnetic Waves Excited by Gerasimenko; Icarus, Volume 311, Pages 1-22, Newborn Interstellar Pickup Ions Measured by the DOI: 10.1016/j.icarus. 2018.03.010, 2018 Voyager Spacecraft from 1 to 45 au. II. Instability 17. Giuranna, M., S. Fonte, A. Longobardo, G. and Turbulence Analyses; Astrophysical Journal, Sindoni, P. WOLKENBERG, V. Formisano; Volume 863, Issue 1, Article number 76, DOI: PFS/MEX limb observations of 4.3-µm CO2 non- DOI: 10.3847/1538-4357/aac839, 2018 LTE emission in the atmosphere of Mars; Icarus, 24. Hollick, S.J., C. W. Smith, Z. B. Pine, M. R. Volume 315, Pages 46-60, DOI: 10.1016/ Argall, C. J. Joyce, P. A. Isenberg, B. J. Vasquez, j.icarus.2018.06.018, 2018 N. A. Schwadron, J. M. SOKÓŁ, M. BZOW- 18. GRYCIUK, M., P. PODGÓRSKI, S. GBU- SKI, M. A. KUBIAK; Magnetic Waves Excited by REK, T. Mrozek, M. SIARKOWSKI, M. Newborn Interstellar Pickup Ions Measured by the STĘŚLICKI, J. BARYLAK, A. BARYLAK; Voyager Spacecraft from 1 to 45 au. III. Observation The expected fluxes observed by STIX during low Times; Astrophysical Journal, Supplement Ser- solar activity; Journal of Atmospheric and So- ies, Volume 237, Issue 2, Article number 34, lar-Terrestrial Physics, Volume 179, Pages 94- DOI: 10.3847/1538-4365/aac83a, 2018 96, DOI: 10.1016/j.jastp.2018.06.013, 2018 25. JANDA, A.Z., Exact solutions and singularities of 19. GRZESIAK, M., C. Cesaroni, L. Spogli, G. an X-point collapse in Hall magnetohydrodynamics; De Franceschi, V. Romano; Regional Short-Term Journal of Mathematical Physics, Volume 59, Forecasting of Ionospheric TEC and Scintillation;

113 Issue 6, Article number 061509, DOI: 10. Issue 2, Pages 2393–2398, DOI: 10.1093/ 1063/1.5026876, 2018 mnras/sty811, 2018 26. Jiang, Z., V. Zhang, Y. Huang, J. Achkar, D. 34. Kulczyk, S., E. WOŹNIAK, M. Derek; Land- Piester, S. Lin, W. Wu, A. Naumov, S. Yang, J. scape, facilities and visitors: An integrated model of NAWROCKI, I. Sesia, C. Schlunegger, Z. recreational ecosystem services; Ecosystem Servi- Yang, M. Fujieda, A. Czubla, H. Esteban, C. ces, DOI: 10.1016/j.ecoser.2018.02.016, 2018 Rieck, P. Whibberley; Use of software- 35. LEJBA, P., T. SUCHODOLSKI, P. MICHA- defined radio receivers in two-way satellite ŁEK, J. BARTOSZAK, S. Schillak, S. ZAPA- time and frequency transfers for UTC com- ŚNIK; First laser measurements to space debris in putation; Metrologia Vol. 55, 685–698, DOI: Poland; Advances in Space Research, DOI: 10. 10.1088/1681-7575/aacbe6, 2018 1016/j.asr.2018.02.033, 2018 27. KĘPA, A., B. SYLWESTER, J. SYLWE- 36. Macek, W. M., A. KRASIŃSKA, M. V. D. Sil- STER, M. GRYCIUK, M. SIARKOWSKI; veira, D. G. Sibeck, A. WAWRZASZEK, J. L. Analysis of the differential emission measure Burch, C. T. Russell; Magnetospheric Multiscale distributions for solar flares observed by RESIK; Observations of Turbulence in the Magnetosheath on Journal of Atmospheric and Solar-Terrestrial Kinetic Scales; Astrophysical Journal Letters, Physics, Volume 179, Pages 545-552, DOI: Volume 864, Issue 2, Article number L29, 10.1016/j.jastp.2018.09.004, 2018 DOI: 10.3847/2041-8213/aad9a8, 2018 28. KOTARBA, A. Z., A. NOWAKOWSKI; Im- 37. Macek, W. M., A. WAWRZASZEK, B. Ku- pact of snow cover on impervious surface detection; In- charuk; Intermittent turbulence in the heliosheath ternational Journal of Remote Sensing, Volu- and the magnetosheath plasmas based on Voyager and me 39, Issue 21, Pages 7607-7627, DOI: 10. THEMIS data; Nonlinear Processes in 1080/01431161.2018.1475775, 2018 Geophysics, Volume 25, Issue 1, Pages 39-54, 29. KOTARBA, A. Z.; Vertical profile of cloud amo- DOI: 10.5194/npg-25-39-2018, 2018 unt over Poland: Variability and uncertainty based on 38. McComas, D.J., E. R. Christian, N. A. Schwa- CloudSat-CALIPSO observations; International dron, N. Fox, J. Westlake, F. Allegrini, D. N. Journal of Climatology, Vol.38, 4142-4254p.; Baker, D. Biesecker, M. BZOWSKI, G. Clark, DOI: 10.1002/joc.5558, 2018 C. M. S. Cogen, I. Cohen, M. A. Dayeh, R. De- 30. KOWALSKA-LESZCZYŃSKA, I., M. cker, G. A. de Nolfo, M. I. Desai, R. W. Ebert, BZOWSKI, J. M. SOKÓŁ, M. A. KUBIAK; H. A. Elliott, H. Fahr, P. C. Frisch, H. O. Evolution of the Solar Lyα Line Profile during the Funsten, S. A. Fuselier, A. Galli, A. B. Galvin, Solar Cycle; Astrophysical Journal, Volume J. Giacalone, M. Gkioullidou, F. Guo, M. Ho- 852, Issue 2, Article number 115, DOI: 10. ranyi, P. Isenberg, P. Janzen, L. M. Kistler, K. 3847/1538-4357/aa9f2a, 2018 Korreck, M. A. KUBIAK, H. Kucharek, B. A. 31. KOWALSKA-LESZCZYŃSKA, I., M. Larsen, R. A. Leske, N. Lugaz, J. Luhmann, W. BZOWSKI, J. M. SOKÓŁ, M. A. KUBIAK; Mattheaus, D. Mitchell, E. Moebius, K. Oga- Evolution of the solar Lyα line profile during the solar sawara, D. B. Reisenfeld, J. D. Richardon, C. T. cycle. II. How accurate is the present radiation pres- Russell, J. M. SOKÓŁ, H. E. Spence, R. Sko- sure paradigm for interstellar neutral H in the helio- ug, Z. Sternovsky, P. Swaczyna, J. R. Szalay, M. sphere? The Astrophysical Journal, Volume Tokumaru, M. E. Wiedenbeck, P. Wurz, G. P. 868, Number 1, doi.org/10.3847/1538- Zank, E. J. Zirnstein; – 2018, Interstellar Map- 4357/aae70b, 2018 ping and Acceleration Probe (IMAP): A new NA- 32. KRÓLIKOWSKA, M., P. A. Dybczyński; SA mission, Space Science Reviews, 214:116, Dynamical evolution of C/2017 K2 PAN- 54pp, DOI:10.1007/s11 214-018-0550-1, STARRS; Astronomy & Astrophysics, Vol. 2018 15, A170, DOI: 10.1051/0004-6361/2018 39. Molotkov, I. A., B. ATAMANIUK; An Analy- 32917, 2018 sis of Processes in the Solar Wind in a Thin Layer 33. KRÓLIKOWSKA, M., P. A. Dybczyński; Adjacent to the Front of the Shock Wave; ASTRO- How the modified method of orbit quality assessment PHYSICAL JOURNAL, Volume: 859, Issue: works for Oort spike comets? Monthly Notices of 1, Article Number: 39, DOI: 10.3847/1538- the Royal Astronomical Society, Volume 477, 4357/aaba73, 2018

114 40. Mrozek, T., S. GBUREK, M. SIARKOWSKI, Continental Flood Basalt Province; Geochemistry, B. SYLWESTER, J. SYLWESTER, A. KĘPA, Geophysics, Geosystems, Vol. 19, Issue 10 pa- M. GRYCIUK; Solar Microflares Observed by ges 3917-3944, DOI: 10.1029/ 2018GC0077 SphinX and RHESSI; Solar Physics, Volume 24, 2018 293, Issue 7, Article number 101, DOI: 48. RYBUS, T., K. SEWERYN, J. OLEŚ, F. L. BA- 10.1007/s11207-018-1319-0, 2018 SMADJI, K. TARENKO, R. MOCZY- 41. NICOLAU-KUKLIŃSKA, A., A. Losiak; IF DŁOWSKI, T. BARCIŃSKI, J. Kindracki, Ł. TROILITE IS THE SOURCE OF BUBBLES Mężyk, P. Paszkiewicz, P. Wolański; Application FORMED IN THE FUSION CRUST?; of a planar air-bearing microgravity simulator for METEORITICS & PLANETARY SCIEN- demonstration of operations required for an orbital CE Volume: 53 Pages: 6324-6324 Supple- capture with a manipulator; Acta Astronautica, ment: 1 Special Issue: SI, 2018 Volume 155, Pages 211-229, DOI: 10.1016/j. 42. Phillips, K. J. H., J. SYLWESTER, B. SYLWE- actaastro. 2018.12.004, 2018 STER, M. KOWALIŃSKI, M. SIARKOW- 49. Schwadron, N. A., F. Allegrini, M. BZOWSKI, SKI, W. TRZEBIŃSKI, S. PŁOCIENIAK, E. R. Christian, M. A. Dayeh, M. I. Desai, K. Z. KORDYLEWSKI; Highly Ionized Calcium Fairchild, P. C. Frisch, H. O. Funsten, S. A. Fu- and Argon X-Ray Spectra from a Large Solar Flare; selier, A. Galli, P. Janzen, M. A. KUBIAK, D. J. Astrophysical Journal, Volume 863, Issue 1, McComas, E. Moebius, D. B. Reisenfeld, J. M. Article number 10, DOI: 10.3847/1538- SOKÓŁ, P. Swaczyna, J. R. Szalay, P. Wurz, E. 4357/aace5b, 2018 J. Zirnstein; Time dependence of the IBEX ribbon 43. PŁOCIENIAK, S., Ż. SZAFORZ; Laboratory and the globally distributed energetic neutral atom flux characterization of bent monocrystal wafers for Bragg using the first 9 years of observations, The Astro- X-ray spectroscopy; Experimental Astronomy, physical Journal Supplement Series, Volume Pages 1-14, DOI: 10.1007/s10686-018-9583- 239, Number 1, DOI:10.3847/1538-4365/ 4, 2018 aae48e, 2018 44. Popel, S.I., A. P. Golub, A. V. Zakharov, L. M. 50. Schwadron, N. A., M. BZOWSKI; The helio- Zelenyi, A. A. Berezhnoy, E. S. Zubko, M. sphere is not round, The Astrophysical Journal, Iten, R. Lena, S. Sposetti, Y. I. Velikodsky, A. Vol. 862, 11, 7pp., DOI: 10.3847/1538-4357/ A. Tereshchenko, B. ATAMANIUK; Forma- aacbcf, 2018 tion of Dusty Plasma Clouds at Meteoroid Impact on 51. SEWERYN, K., J. Z. Sąsiadek; Satellite angular the Surface of the Moon; JETP Letters, Volume motion classification for active on-orbit debris removal 108, Issue 6, Pages 356-363, DOI: 10.1134/ using robots; Aircraft Engineering and Aero- S0021364018180091, 2018 space Technology, DOI:10.1108/AEAT-01- 45. Puig, L., G. Pilbratt, A. Heske, I. Escudero, P.- 2018-0049, 2018 E. Crouzet, B. de Vogeleer, K. Symonds, R. 52. ŚLIWIŃSKA, J., M. Wińska, J. NASTULA; Kohley, P. Drossart, P. Eccleston, P. Hartogh, Terrestrial water storage variations and their effect on J. Leconte, G. Micela, M. Ollivier, G. Tinetti, polar motion; Acta Geophysica 23pp, DOI: D. Turrini, B. Vandenbussche, P. WOL- 10.1007/s11600-018-0227-x, 2018 KENBERG; The phase a study of the ESA M4 53. Stanica, D. A., D. Stanica, J. BŁĘCKI, T. Ernst, mission candidate ARIEL; Experimental W. Jóźwiak, J. SŁOMIŃSKI; Preseismic geoma- Astronomy, Volume 46, Issue 1, pp 211–239, gnetic and ionosphere signatures related to the Mw5.7 DOI: 10.1007/s10686-018-9604-3, 2018 earthquake occurred in Vrancea zone on September 46. RICKMAN, H., M. I. BŁĘCKA, J. GURGU- 24, 2016; Acta Geophysica, Volume 66, Issue REWICZ, U. G. Jørgensen, E. Słaby, S. SZU- 2, pp 167–177, DOI: 10.1007/ s11600-018-01 TOWICZ, N. ZALEWSKA; Water in the histo- 15-4, 2018 ry of Mars: An assessment; Planetary and Space 54. STANISŁAWSKA, I., T. Gulyaeva, O. GRY- Science DOI: 10.1016/j.pss.2018. 08.003, NYSHYNA-POLIUGA, L. Pustovalova; Io- 2018 nospheric Weather During Five Extreme Geoma- 47. Rooney, T. O., S. R. Krans, D. MÈGE, N. Ar- gnetic Superstorms Since IGY Deduced with the In- naud, T. Korme, J. Kappelman, G. Yirgu; Con- stantaneous Global Maps GIM-¦oF2; SPACE straining the Magmatic Plumbing System in a Zoned

115 WEATHER-THE INTERNATIONAL JO- geophysical models; Studia Geophysica et Geoda- URNAL OF RESEARCH AND APPLICA- etica, 24pp., DOI: 10.1007/s11200-018-1028- TIONS, Volume 15, Issue 3, 26pp, DOI: 10. z, 2018 1029/2018SW001945, 2018 62. Witkowski, M., R. Munoz-Rodriguez, A. Ra- 55. SWACZYNA, P., M. BZOWSKI, M. A. KU- czyński, J. Zaremba, B. NAGÓRNY, P. S. Zu- BIAK, J. M. SOKÓŁ, S. A. Fuselier, A. Galli, chowski, R. Ciuryło, M. Zawada; Photoioniza- D. Heirtzler, H. Kucharek, D. J. McComas, E. tion cross sections of the 5S1/2 and 5P3/2 states of Möbius, N. A. Schwadron, P. Wurz; Interstellar Rb in simultaneous magneto-optical trapping of Rb Neutral Helium in the Helio-sphere from IBEX Ob- and Hg; Physical Review A, Volume 98, Issue 5, servations. V. Observations in IBEX-Lo ESA Ste- Article number 053444, 2018 ps 1, 2, and 3; Astrophysical Journal, Volume 63. WOLKENBERG, P., G. Piccioni, M. BANA- 854, Issue 2, Article number 119, DOI: 10. SZKIEWICZ; Vertical temperature profiles in the 3847/1538-4357/aaabbf, 2018 Venus mesosphere obtained by two retrieval methods 56. Szymaniec, K., R. J. Hendricks, K. Turza, B. from the VIRTIS-VEX observations; Journal of NAGÓRNY, P. DUNST, J. NAWROCKI, P. Quantitative Spectroscopy and Radiative Krehlik, Ł. Śliwczyński, A. Czubla; Operation Transfer, Volume 217, Pages 407-415, DOI: of caesium fountain frequency standards with remote 10.1016/j.jqsrt.2018.06.010, 2018 hydrogen maser references, Metrologia, Volume 64. WOŹNIAK, E., W. KOFMAN, S. LE- 55, 8pp DOI: 10.1088/1681-7575/aae40d, WIŃSKI, P. WAJER, M. RYBICKI, S. ALE- 2018 KSANDROWICZ, A. WŁODARKIE- 57. Tinetti, G., P. WOLKENBERG, M. RATAJ, WICZ; Multi-temporal polarimetry in land-cover W. BUJWAN, M. BŁĘCKA, M. BANA- classification; International Journal of Remote SZKIEWICZ, R. GRACZYK, K. SKUP, P. Sensing, 18pp, DOI: 10.1080/01431161. WAWER, A. WAWRZASZEK, and 230 2018.1483084, 2018 others authors; A chemical survey of exoplanets 65. WOŹNIAK, E., S. Kulczyk, M. Derek; From with ARIEL; Experimental Astronomy, intrinsic to service potential: an approach to assess Volume 46, Issue 1, pp 135–209, DOI: 10. tourism landscape potential; Landscape and Urban 1007/s10686-018-9598-x, 2018 Planning, Volume 170, Pages 209-220, DOI: 58. Turrini, D., Y. Miguel, T. Zingales, A. Piccialli, 10.1016/j.landurbplan.2017.10.006, 2018 R. Helled, A. Vazan, F. Oliva, G. Sindoni, O. 66. Zalewska N., M. Mroczkowska-Szerszeń, J. Panić, J. Leconte, M. Min, S. Pirani, F. Selsis, V. Fritz, M. BŁĘCKA; Modeling of surface spe- Coudé du Foresto, A. Mura, P. WOLKEN- ctra with and without dust from Martian infra- BERG; The contribution of the ARIEL space mis- red data: new aspects; Aircraft Engineering sion to the study of planetary formation; Experi- and Aerospace Technology, Vol. 91 Issue: 2, mental Astronomy, Pages 1-21, DOI: 10.10 pp.333-345, DOI:10.1108/AEAT-01-2018- 07/s10686-017-9570-1, 2018 0051, 2018 59. WAJER, P., E. WOŹNIAK, W. KOFMAN, 67. Zhang, S., A. Santangelo, M. Feroci, Y. Xu, F. M. RYBICKI, S. LEWIŃSKI; Simulation of Lu, S. Brandt, M. Hernanz, M. MICHALSKA, SAR images of urban areas by using the ray tracing P. ORLEAŃSKI, L. Baldini, E. Bozzo et al.; method with measured values of backscatter The enhanced X-ray Timing and Polarimetry coefficients; INTERNATIONAL JOURNAL mission—eXTP; SCIENCE CHINA Physics, OF REMOTE SENSING, Volume: 39 Issue: Mechanics & Astronomy, Volume 62, Issue 2: 9 Pages: 2671-2689, DOI: 10.1080/0143 029502, DOI:10.1007/s11433-018-9309-2, 1161.2018.1430396, 2018 2018 60. WASILEWSKI T. G.; Evaluation of drilling- 68. Zucca, P., D. E. Morosan, A. P. Rouillard, R. based water extraction methods for Martian ISRU Fallows, P. T. Gallagher, J. Magdalenic, K.-L. from mid-latitude ice resources; Planetary and Klein, G. Mann, C. Vocks, E. P. Carley, M. M. Space Science, Volume 158, Pages 16-24, Bisi, E. P. Kontar, H. ROTHKAEHL, B. DOI: 10.1016/j.pss.2018.05.012, 2018 Dąbrowski, A. Krankowski, J. Anderson, A. 61. Wińska, M., J. ŚLIWIŃSKA; Assessing hydro- Asgekar, M. E. Bell, M. J. Bentum, P. Best, R. logical signal in polar motion from observations and Blaauw, F. Breitling, J. W. Broderick, W. N.

116 Brouw, M. Brüggen, H. R. Butcher, B. Ciardi, próbnika kosmicznego]; Przeglad Elektro- E. de Geus, A. Deller, S. Duscha, J. Eislöffel, techniczny, Volume 94, Issue 5, Pages 153- M. A. Garrett, J. M. Grießmeier, A. W. Gunst, 158; DOI: 10.15199/48.2018.05.27, 2018 G. Heald, M. Hoeft, J. Hörandel, M. Iacobelli, Other publications E. Juette, A. Karastergiou, J. van Leeuwen, D. McKay-Bukowski, H. Mulder, H. Munk, A. 1. Barbera, M., U. Lo Cicero, L. Sciortino, F. Nelles, E. Orru, H. Paas, V. N. Pandey, R. D'Anca, G. Parodi, M. RATAJ, S. POLAK, A. Pekal, R. Pizzo, A. G. Polatidis, W. Reich, A. Pilch, N. Meidinger, S. Sciortino, G. Rauw, G. Rowlinson, D. J. Schwarz, A. Shulevski, J. Slu- B. Raymont, T. Mineo, E. Perinati, P. Giglio, A. man, O. Smirnov, C. Sobey, M. Soida, S. Thou- Collura, S. Varisco, R. Candia; ATHENA dam, M. C. Toribio, R. Vermeulen, R. J. van WFI optical blocking filters development status toward Weeren, O. Wucknitz and P. Zarka; Shock loca- the end of the instrument phase-A; Proceedings of tion and CME 3D reconstruction of a solar type II SPIE - The International Society for Optical radio burst with LOFAR; ASTRONOMY & Engineering, Volume 10699, Article number ASTROPHYSICS, Vol. 615, A89, DOI: 10. 106991K, DOI: 10.1117/12.2314448, 2018 1051/0004-6361/201732308, 2018 2. Barret, D., T. Lam Trong, J.-W. Den Herder, L. Piro, M. Cappi, J. Houvelin, R. Kelley, J. M. Monographs, reviews in international and Mas-Hesse, K. Mitsuda, S. Paltani, G. Rauw, A. national publications Rozanska, J. Wilms, S. Bandler, M. Barbera, X. 1. Hauber, E., D. MÈGE, T. Platz, P. Brož; “En- Barcons, E. Bozzo, M. T. Ceballos, I. Charles, E. Costantini, A. Decourchelle, R. Den dogenic Processes”, Planetary Geology, part of Hartog, L. Duband, J.-M. Duval, F. Fiore, F. the Astronomy and Planetary Sciences book Gatti, A. Goldwurm, B. Jackson, P. Jonker, C. sub series, 147-183, DOI: 10.1007/978-3- Kilbourne, C. MacCuli, M. Mendez, S. 319-65179-8_8, 2018 Molendi, P. ORLEAŃSKI, F. Pajot, E. Other articles in international and national Pointecouteau, F. Porter, G. W. Pratt, D. Prêle, publications (listed by the Polish Ministry of L. Ravera, K. Sato, J. Schaye, K. Shinozaki, T. Science and Higher Education) Thibert, L. Valenziano, V. Valette, J. Vink, N. Webb, M. Wise, N. Yamasaki, F. Douchin., J.- 1. Chmaj, G., K. SEWERYN, T. RYBUS, T. M. Mesnager, B. Pontet, A. Pradines, G. Buratowski, M. Musioł, M. BANASZKIE- Branduardi-Raymont, E. Bulbul, M. Dadina, WICZ; The dynamics aspects of modeling and S. Ettori, A. Finoguenov, Y. Fukazawa, A. control of the flying robot with attached two Degree of Janiuk, J. Kaastra, P. Mazzotta, J. Miller, G. Freedom manipulator; GeoPlanet: Earth and Pla- Miniutti, Y. Naze, F. Nicastro, S. Scioritino, A. netary Sciences, Aerospace Robotics III, 121- Simonescu, J. M. Torrejon, B. Frezouls, H. 148, 10.1007/978-3-319-94517-0_8, 2018 Geoffray, P. Peille, C. Aicardi, J. André, C. 2. RYBUS, T., K. SEWERYN, J. Z. SĄSIADEK; Daniel, A. Clénet, C. Etcheverry, E. Gloa- Nonlinear Model Predictive Control (NMPC) guen, G. Hervet, A. Jolly, A. Ledot, I. Maus- for free-floating space manipulator; Geo- sang, A. Paillet, R. Schmisser, J.-M. Travert, B. Planet: Earth and Planetary Sciences, 17-29p, Vella, J.-C. Damery, K. Boyce, M. DIpirro, S. DOI: 10.1007/978-3-319-94517-0_2, 2018 Lotti, D. Schwander, S. Smith, B.-J. Van 3. WAWRZASZEK, R., M. Waraksa, M. KA- Leeuwen, H. Van Weers, N. Clerc, B. Cobo, T. LARUS, G. JUCHNIKOWSKI, T. Górski; Dauser, J. De Plaa, C. Kirsch, E. Cucchetti, M. Detection and Decoding of AIS Navigation Mes- Eckart, P. Ferrando, L. Natalucci; The sages by a Low Earth Orbit Satellite; GeoPlanet: ATHENA X-ray Integral Field Unit (X-IFU); Earth and Planetary Sciences, 45-62p, DOI: Proceedings of SPIE - The International 10.1007/978-3-319-94517-0_4, 2018 Society for Optical Engineering Volume 4. Wolski, L., W. Matelski, K. SEWERYN, P. 10699, Article number 106991G, 2018 PAŚKO; Supercapacitors based driving system for 3. BARYLAK, J., A. BARYLAK, T. MROZEK, space fast surface sample acquisition system M. STĘŚLICKI, P. PODGÓRSKI; Investi- [Superkondensatorowy układ napędowy gruntowego gation of cosmic ray and solar energetic particle

117 background of STIX using GEANT4 simulation; 11. Dudnik, O.V., I. V. Lazarev, E. V. Kurbatov, M. Proceedings of SPIE - The International So- KOWALIŃSKI, P. PODGÓRSKI, D. ŚCI- ciety for Optical Engineering Volume 10808, SŁOWSKI; Advisability of the axes orientation in Article number 1080848, DOI: 10.1117/12. p-terphenyl crystal of scintillation detector of the char- 2501722, 2018 ged particle monitor in ChemiX solar X-ray spectro- 4. BASMADJI, F. L., A. BIEDRZYCKA, M. photometer; Space Science and Technology, Vol. PAWLUS, K. SEWERYN, J. SĄSIADEK; 3 (112), p. 33-39 DOI: 10.15407/knit2018.03. Naziemna weryfikacja manewrów realizowanych 033, 2018 przez robota kosmicznego; Prace naukowe Poli- 12. DUNST, P., B. NAGÓRNY, D. LEMAŃSKI, techniki Warszawskiej – Elektronika, z.196, P. NOGAŚ, J. NAWROCKI, R. J. Hendricks, 35-50p., 2018 F. Ozimek, K. Szymaniec; Preliminary evaluation 5. Birylo, M., Z. Rzepecka, J. NASTULA; As- of the AOS-CsF1 primary frequency standard- sessment of the Water Budget from GLDAS Model; 2017; 2017 Joint Conference of the European Proceedings - 2018 Baltic Geodetic Congress, Frequency and Time Forum and IEEE Inter- BGC-Geomatics 2018, Article number 845 national Frequency Control Symposium, Arti- 3671, Pages 86-90, 2018 cle number 8088980, Page 628, DOI: 10. 6. Chen, C. Y., T. J. Y. Liu, I. T. Lee, H. ROTH- 1109/FCS.2017.8088980, 2018 KAEHL, D. PRZEPIÓRKA, L. C. Chang, B. 13. Dybczyński, P. A., M. KRÓLIKOWSKA; Ha- MATYJASIAK, K. Ryu, K.-I. Oyama; The ve we missed an interstellar comet four years ago?; Midlatitude Trough and the Plasmapause in the arXiv eprint, No. 1810.12766, 2018 Nighttime Ionosphere Simultaneously Observed by 14. Eyraud, C., A. Hérique, J. M. Geffrin, W. KOF- DEMETER During 2006–2009; Journal of MAN; Imaging the inner structure of a comet from Geophysical Research: Space Physics, 123, few measurements in a bistatic scenario: Case of a scale 5917 – 5932, DOI: 10. 1029/2017JA024840, model; IET Conference Publications, Volume 2018 2018, Issue CP741, 2018 7. CIĄŻELA, J., S. Roszak; NATURISTS OF 15. Feroci, M., M. Ahangarianabhari, G. Ambrosi, THE LUBIEWO RESORT, MIĘDZY- F. Ambrosino, A. Argan, M. Barbera, J. Bayer, ZDROJE, POLAND – CHARACTE- P. Bellutti, B. Bertucci, G. Bertuccio, G. Bor- RISTICS AND MOTIVATIONS; Geoprze- ghi, E. Bozzo, F. Cadeaux, R. Campana, F. Ce- strzeń 1, 97-111, 2018 raudo, T. Chen, D. Cirrincione, A. De Rosa, E. 8. CIĄŻELA, M., D. MEGE, J. CIĄŻELA, J. Del Monte, S. Di Cosimo, S. Diebold, Y. Evan- GURGUREWICZ, P. TESSON; Lithology of gelista, Q. Fan, Y. Favre, F. Ficorella, F. Fu- the Martian surface from thermal remote sensing data; schino, O. Gevin, M. Grassi, B. Hong, H. Mao, MINERALOGIA - SPECIAL PAPERS, Vol. V. Karas, T. Kennedy, C. Labanti, O. Limousin, 48, p.42, 2018 U. Lo Cicero, F. Lu, T. Luo, P. Malcovati, A. 9. Dąbrowska-Szewczyk, E., A. Zawadzka, P. Martindale, A. Meuris, M. MICHALSKA, A. Kowalczyk, R. Podgórski, M. Wojasiński, T. Morbidini, F. Muleri, P. ORLEAŃSKI, S. Ciach, R. GRACZYK, T. Zawistowski, P. Paltani, T. Pan, E. Perinati, A. Picciotto, M. Kukołowicz; [P213] Influence of beam spoiler and Pohl, I. Rashvskaia, A. Santangelo, S. Schanne, air gap on dose distribution in build-up region for X6 K. SKUP, J. Svoboda, C. Tenzer, A. Vacchi, D. MV static field; Physica Medica,Volume 52, Walton, B. Winter, X. Wu, Y. Xu, G. Zampa, N. Supplement 1, Pages 161-162, DOI: 10.10 Zampa, S. Zane, A. Zdziarski, L. Zhang, S. 16/j.ejmp.2018.06.505, 2018 Zhang, S. Zhang, W. Zhang, X. Zhang, Y. 10. De Angelis, A., V. Tatischeff, I. A. Grenier, J. Zhou, N. Zorzi; The Large Area Detector onboard McEnery, M. Mallamaci, M. Tavani, P. ORLE- the eXTP mission; Proceedings of SPIE - The AŃSKI, and other 230 authors; Science with e- International Society for Optical Engineering, ASTROGAM: A space mission for MeV–GeV Volume 10699, Article number 106991C, gamma-ray astrophysics; Journal of High Energy DOI: 10.1117/12.2312466, 2018 Astrophysics, Volume 19, Pages 1-106, DOI: 16. Galano, D., A. Bemporad, S. Buckley, I. Cer- 10.1016/j.jheap.2018.07.001, 2018 nica, V. Dániel, F. Denis, L. De Vos, S. Fine-

118 schi, C. Galy, R. GRACZYK, P. Horodyska, J. measurements; E3S Web of Conferences Volu- Jacob, R. Jansen, N. Kranitis, M. Kurowski, M. me 29, Article number 00021, DOI: 10.1051/ ŁADNO, P. Ledent, D. Loreggia, R. Melich, e3sconf/20182900021, 2018 D. Mollet, M. Mosdorf, A. Paschalis, R. 21. Kozłowski, S., K. KUREK, J. Skarzyński, K. Peresty, M. Purica, B. Radzik, M. RATAJ, R. Szczygielska, M. DARMETKO; Investigation on Rougeot, L. Salvador, C. Thizy, J. Versluys, T. adaptive satellite communication system performance Walczak, A. Zarzycka, J. Zender, A. Zhukov; using SDR technique; MIKON 2018 - 22nd In- Development of ASPIICS: A coronagraph based on ternational Microwave and Radar Conference, Proba-3 formation flying mission; Proceedings of Pages 363-366, DOI: 10.23919/MIKON. SPIE - The International Society for Optical 2018.8405226, 2018 Engine-ering, Volume 10698, Article number 22. Lewandowski, W., L. Błaszkiewicz, B. Śmier- 106982 Y, 2018 ciak, M. POŻOGA, J. Kijak, A. Krankowski, 17. Hernanz, M., S. Brandt, M. Feroci, P. OR- K. Chyży, H. ROTHKAEHL, R. Pękal, T. LEAŃSKI, A. Santangelo, S. Schanne, Xin Sidorowicz, M. Sendyk, M. Curyło, B. MATY- Wu, J. in't Zand, S. N. Zhang, Y. P. Xu, E. JASIAK; Observations of the interstellar scattering Bozzo, Y. Evangelista, J. L. Gálvez, C. Tenzer, of pulsars with the POLFAR stations; 2018 Baltic F. Zwart, F. J. Lu, S. Zhang, T. X. Cheng, F. URSI Symposium (URSI), No. 17899165, Ambrosino, A. Argan, E. Del Monte, C. DOI: 10.23919/URSI.2018.8406733, 2018 Budtz-Jorgensen, N. Lund, P. Olsen, C. Man- 23. MAKOWSKI, A. E., J. BARYLAK, M. STĘ- sanet, R. Campana, F. Fuschino, C. Labanti, A. ŚLICKI, Z. SZAFORZ, P. PODGÓRSKI, J. Rachevski, A. Vacchi, G. Zampa, N. Zampa, I. BĄKAŁA, D. ŚCISŁOWSKI; Geant4-based Rashevskaya, P. Bellutti, G. Borghi, F. Fi- simulations of the x-ray luminescence background in corella, A. Picciotto, N. Zorzi, O. Limousin, the rotating drum spectrometer/ SOLPEX; Procee- A. Meris; The wide field monitor onboard the eXTP dings of SPIE - The International Society for mission; Proceedings of SPIE - The Interna- Optical Engineering, Volume 10808, Article tional Society for Optical Engineering, Volu- number 1080846, DOI: 10.1117/12.2501715, me 10699, Article number 1069948, DOI: 2018 10.1117/12.2313214, 2018 24. MAREK, M., R. SCHREIBER; Is the AKR 18. JENEROWICZ, M., M. BANASZKIE- Cyclotron Maser Instability a self-organized criticality WICZ; ASTEROID (21) LUTETIA: SEMI- system? Planetary Radio Emissions VIII, 269- AUTOMATIC IMPACT CRATERS 277, Proceedings of the 8th International DETECTION AND CLASSIFICATION; Workshop on Planetary, Solar and Helio- International Archives of the Photogramme- spheric Radio Emissions held at Seggauberg try, Remote Sensing and Spatial Information near Graz, Austria, 2018 Sciences - ISPRS Archives, Volume 42, Issue 25. Parodi, G., F. D'Anca, U. Lo Cicero, L. Scio- 2, Pages 479-486, DOI: 10.5194/isprs- rtino, M. RATAJ, S. POLAK, A. Pilch, N. archives-XLII-2-479-2018, 2018 Meidinger, K. Dittrich, J. Hartwig, V. Samain, 19. KACZOROWSKI, M., D. Kasza, R. ZDU- A. Collura, S. F. Bonura, A. Buttacavoli, M. NEK, R. WRONOWSKI; Application of obser- Barbera; Structural modelling and mechanical tests vations of recent tectonic activity in the Świebodzice supporting the design of the ATHENA X-IFU Depression (the Sudetes, SW Poland) in assessing thermal filters and WFI optical blocking filter; seismic hazard in the Fore-Sudetic Monocline; E3S Proceedings of SPIE - The International So- Web of Conferences Volume 55, Article nu- ciety for Optical Engineering, Volume 10699, mber 00001, 23rd Autumn School of Geode- Article number 106994C, DOI: 10.1117/12. sy, DOI: 10.1051/ e3sconf/20175500001, 2314451, 2018 2018 26. Pascale, E., N. Bezawada, J. Barstow, J.-P. Be- 20. Kasza, D., A. Kowalski, J. Wojewoda, M. KA- aulieu, N. Bowles, V. Coudé Du Foresto, A. CZOROWSKI; Indicators of recent geodynamic Coustenis, L. Decin, P. Drossart, P. Eccleston, activity in the Książ Castle area (Świebodzice Unit, T. Encrenaz, F. Forget, M. Griffin, M. Güdel, Sudetes) in the light of structural analysis and geodetic P. Hartogh, A. Heske, P.-O. Lagage, J. Leconte,

119 P. Malaguti, G. Micela, K. Middleton, M. Min, Volume 28, Issue 1, Pages 105-118, DOI: 10. A. Moneti, J. C. Morales, L. Mugnai, M. Olli- 24425/119079, 2018 vier, E. Pace, A. Papageorgiou, G. Pilbratt, L. 33. SEWERYN, K., T. RYBUS, P. Colmenarejo, Puig, M. RATAJ, T. Ray, I. Ribas, M. Rocchet- L. Mollinedo, G. Novelli, J. OLEŚ, M. Pietras, to, S. Sarkar, F. Selsis, W. Taylor, J. Tennyson, J. Z. SĄSIADEK, M. Scheper, K. TAREN- G. Tinetti, D. Turrini, B. Vandenbussche, O. KO; Validation of the Robot Rendezvous and Gras- Venot, I. P. Waldmann, P. WOLKENBERG, ping Manoeuvre Using Microgravity Simulators; G. Wright, M.-R. Zapatero Osorio, T. Zinga- 2018 IEEE International Conference on Ro- les; The ARIEL space mission; Proceedings of botics and Automation (ICRA), DOI:10. 11 SPIE - The International Society for Optical 09/ICRA.2018.8460475, 2018 Engineering, Volume 10698, Article number 34. SKUP, K., S. POLAK, M. RATAJ, P. Życki, A. 106980H, DOI: 10.1117/12.2311838, 2018 Różańska; Polish contribution to the ATHENA 27. Patkó, L., J. CIĄŻELA , L. Aradi, N. Liptai, I. Wide Field Imager; Proceedings of the Polish Kovács, F. Holtz, C. Szabó; Fe and Cu isotope Astronomical Society, Vol. 7, 349-354, 2018 signatures in sulfide blebs from various upper 35. Tatischeff, V., A. De Angelis, M. Tavani, I. mantle xenoliths from the Nógrád-Gömör Grenier, U. Oberlack, L. Hanlon, R. Walter, A. Volcanic Field (Northern Pannonian Basin); Argan, P. von Ballmoos, A. Bulgarelli, I. Don- MINERALOGIA - SPECIAL PAPERS, Vol. narumma, M. Hernanz, I. Kuvvetli, M. Malla- 48, p.72, 2018 maci, M. Pearce, A. Zdziarski, A. Aboudan, M. 28. Porczek, M., D. Rucińska, S. LEWIŃSKI; Ajello, G. Ambrosi, D. Bernard, E. Bernardini, Using raster and vector data to identify objects for clas- V. Bonvicini, A. Brogna, M. Branchesi, C. sify in flood risk. A case study: Raciborz; E3S Web Budtz-Jorgensen, A. Bykov, R. Campana, M. of Conferences, Volume 29, Article number Cardillo, S. Ciprini, P. Coppi, P. Cumani, R. M. 00026, 17th Conference of PhD Students and Curado da Silva, D. De Martino, R. Diehl, M. Young Scientists, DOI: 10.1051/e3sconf/ Doro, V. Fioretti, S. Funk, G. Ghisellini, J. E. 20182900026, 2018 Grove, F. Giordano, C. Hamadache, D. H. Ha- 29. POŻOGA, M., B. MATYJASIAK, H. RO- rtmann, M. Hayashida, J. Isern, G. Kanbach, J. THKAEHL, D. PRZEPIÓRKA, M. GRZE- Kiener, J. Knödlseder, C. Labanti, P. Laurent, SIAK, R. WRONOWSKI; Observations of M. Leising, O. Limousin, F. Longo, K. Man- the geomagnetic storm 27-28.05. 2017 with nheim, M. Marisaldi, M. Martinez, N. M. Maz- LOFAR PL610; Proceedings of the Polish ziotta, J. E. McEnery, S. Mereghetti, G. Miner- Astronomical Society, Vol. 7, pp.91-93, 2018 vini, A. Moiseev, A. Morselli, K. Nakazawa, P. 30. Prinsloo, D. S., M. Ruiter, M. Arts, J. V. D. ORLEAŃSKI, J. M. Paredes, B. Patricelli, J. Marel, A. J. Boonstra, G. Kruithof, M. Wise, Peyré, G. Piano, M. Pohl, R. Rando, M. Ron- H. Falcke, M. Klein-Wolt, H. ROTHKAEHL, cadelli, F. Tavecchio, D. J. Thompson, R. Tu- B. Cecconi, M. Dekkali, J. Ping; EMI modelling rolla, A. Ulyanov, A. Vacchi, X. Wu, A. Zogla- of an 80 kHz to 80 MHz wideband antenna and uer; The e-ASTROGAM gamma-ray space obser- low-noise amplifier for radio astronomy in space; IET vatory for the multimessenger astronomy of the 2030s; Conference Publications, Volume 2018, Issue Proceedings of SPIE - The International So- CP741, DOI:10.1049/cp.2018.0820, 2018 ciety for Optical Engineering, Volume 10699, 31. ROTHKAEHL, H., M. POŻOGA, M. MO- Article number 106992J, DOI: 10.1117/12. RAWSKI, B. MATYJASIAK, D. PRZE- 2315151, 2018 PIÓRKA, M. GRZESIAK, R. WRO- 36. WITEK, P., P. WAJER, M. BANA- NOWSKI; Near Earth space monitoring with SZKIEWICZ, W. KOFMAN, L. Czechowski, LOFAR PL610 station in Borówiec; Proceedings A. Pommerol; Photochemical model of the Martian of the Polish Astronomical Society, Vol. 7, 48- atmosphere to investigate the fate of trace gases; 54, 2018 European Planetary Science Congress Ab- 32. RYBUS, T., K. SEWERYN, J. Z. Sąsiadek; Ap- stracts, Vol. 12, EPSC2018-648, 2018 plication of predictive control for manipulator moun- 37. WRONOWSKI, R.; Ionospheric scintillations over ted on a satellite; Archives of Control Sciences, the polish LOFAR station PL610; Proceedings

120 of the Polish Astronomical Society, Vol. 7, Publications not shown in the pp.94-96, 2018 Annual Report for 2017 38. ZDUNEK, R., M. KACZOROWSKI, R. WRONOWSKI, D. Kasza; Relations Between 1. Kulczyk, S., E. WOŹNIAK, M. Derek; Eco- Distribution of Extension and Compressions Phases system services in tourism and recreation research - the of Świebodzice Depression Massif Registered by example of fishing in the Great Masurian Lakes, Po- Water-Tube Tiltmeters With Southern Fault Wings land; Problemy Ekologii Krajobrazu [The Pro- Movements Observed On GPS Vector; Abstracts blems of Landscape Ecology] , Vol. 44, 79- of the 19th Chech-Polish Workshop "On 88p., 2017 Recent Geodynamics Of Central Europe", 27-28, 2018

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123 Invited lectures Other lectures on conferences not organized by the CBK PAN Lectures on national conferences organized by the CBK PAN 1. Atamaniuk Barbara, Mariusz Pożoga, H. Ro- thkaehl, B. Matyjasiak, M. Grzesiak, K. Bu- 1. Gabryszewski Ryszard, Projekt "Od śrubki do dzińska, Ł. Tomasik, R. Wronowski, A. Pe- satelity" - założenia i rezultaty, I - Interdyscy- łech, D. Przepiórka, PL610 Borówiec, Face-to plinarne nauczanie przedmiotów przyrodni- Face ILT-TO meeting, 26-27.09.2018 czych i ścisłych, 28.02.2018, Łódź 2. Ciążela Marta, Mège, D., Ciażela, M., Pirajno, 2. Gabryszewski Ryszard Dobre praktyki w nau- F., The role of ACS in the EXOMHYDR pro- czaniu przedmiotów przyrodniczych i ścisłych, I - ject, ExoMars 2016 ACS Science Working Interdyscyplinarne nauczanie przedmiotów Team Meeting, 19-21.02.2018,Padwa,Włochy przyrodniczych i ścisłych, 28.02.2018, Łódź 3. Czechowski Andrzej, Small dust grains in the 3. Krupiński Michał, A. Wawrzaszek, W. Drze- solar wind, Solar Wind 15, 18-22.06.2018, wiecki,S. Aleksandrowicz,M. Jenerowicz Mul- Belgia tifraktalna analiza zobrazowań satelitarnych, 4. Gabryszewski Ryszard, Dobre praktyki w na- VII seminarium Sekcji Teledetekcji KBKiS uczaniu przedmiotów przyrodniczych i ści- PAN, Obserwacje satelitarne, przykłady za- słych,IX Sieradzka Konferencja Kosmiczna, stosowań, część III, 28.05.2018, Warszawa 2-4.10.2018, Sieradz 4. Stanisław Lewiński, Artur Nowakowski, Mar- 5. Gabryszewski Ryszard, O orbitach (nie tylko) cin Rybicki, Radek Malinowski, Ewa Kukaw- szternfeldowskich, IX Sieradzka Konferencja ska, Michał Krupiński, Adam Włodarkiewicz, Kosmiczna, 2-4.10.2018, Sieradz Ewa Bilska, Cezary Wojtkowski, Małgorzata 6. Mège D., Gurgurewicz Joanna, SHARAD die- Jenerowicz Elke Krätzschmar, Sylvia Günt- lectric view of the Ladon site, a Ladon cross- her, Denise Dejon, Eric Krüger Conrad Biel- section, and joint analysis of VNIR +IR data ski, Klasyfikacja form pokrycia terenu na wie- for the CRISM cube covering the CaSSIS ima- loczasowych zdjęciach Sentinel-2, projekt S2 ge of Ladon, ExoMars 2016 CaSSIS Science GLC, VII seminarium Sekcji Teledetekcji KB Working Team Meeting #12, 24-25.09.2018, KiS PAN, Obserwacje satelitarne, przykłady Berno, Szwajcaria zastosowań, część II, 28.05.2018, Warszawa 7. KACZOROWSKI M., Kasza D., ZDUNEK 5. Wajer Paweł, Obserwacje Marsa: od starożyt- R., WRONOWSKI R., Odległe wydarzenia ności do czasów współczesnych, Sympozjum kosmiczne - Wielki Wybuch, a współczesny "Kierunek Mars", 6.04.2018, Warszawa obraz Ziemi widziany przez instrumenty La- Lectures on international conferences organized boratorium Geodynamicznym w Książu, by the CBK PAN XVIII Konferencja Doktorantów i Młodych Uczonych, 22-25.05.2018, Szklarska Poręba 1. Gabryszewski Ryszard, Materkowska, K., 8. Lewiński Stanisław, Michał Krupiński, ZDJĘ- Sprawska, M., Sprawski, S., SAT project sum- CIA SATELITARNE i produkty europej- mary, SAT Project M5 Final Meeting, 28 skiego programu „COPERNICUS”– ich wy- marca 2018 korzystywanie, IX Sieradzka Konferencja Ko- 2. Gabryszewski Ryszard, Materkowska, K., smiczna, 2-4.10.2018, Sieradz Educational projects as the result of SAT pro- 9. Lewiński Stanisław, Gromny Ewa SCERIN-6 ject, SAT Project M5 Final Meeting, 28 marca Capacity Building Workshop on Earth System 2018 Observations, 11-14 06 2018, Zagreb, Croatia 3. Gabryszewski Ryszard, Sat project - evalu- 10. Macek Wiesław, Complex Dynamics in the ation & continuation, SAT Project M5 Final Generalized Lorenz System, 11th Chaotic Meeting, 29 marca 2018 Modeling and Simulation International Con- 4. Rataj Mirosław, Szymon Polak, Robert Pie- ference, 5-8.06.2018, Wlochy trzak, WFI/Filter Wheel Assembly (FWA) 11. Macek Wiesław, Testing for Anisotropy of In- design development, ATHENA/WFI Pro- termittent Turbulence in the Magnetosheath, gress Meeting Exploring system science techniques for

124 Earths Magnetosphere-Ionosphere Termo- Status, JUICE/SWI 10th Consortium Mee- sphere Workshop, 24-26.06.2018, Los Ala- ting, 11-13.12.2018 mos, USA 22. Schwadron, N.A., McComas, D.J., Fuselier, 12. Matyjasiak Barbara, Hanna Rothkaehl, Ma- S.A., Desai, M., Dayeh, M., Funsten, H.O., riusz Pożoga, Dorota Przepiórka, Marcin Janzen, P., Reisenfeld, D., Kucharek, H., Grzesiak, Roman Wronowski, Marek Moraw- Fairchild, K., BZOWSKI, M., SOKÓŁ J. J.M., ski, Barbara Atamaniuk, Probing ionospheric KUBIAK, M.A., Galli, A., Wurz. P., Christian, structures with LOFAR, 2018 LOFAR Ma- E.R., DeMajistre, R., Frisch, P., Separation of gnetism KSP Annual Meeting, 10-14.09.2018, the IBEX ribbon from the globally distributed Kraków flux using nine-year IBEX data, IBEX Science 13. Mege Daniel, Rooney, T.O., Peterson, L., Team Meeting , 27-31.08. , 2018 Phillips, R., Krans, S.R., Steiner, R.A., Mège, 23. Wronowski Roman, M. Kaczorowski, R. Zdu- D., Nelson, W., and Hanan, B.B., Insights from nek, D. Kasza, Odległe wydarzenia kosmiczne the magmatic record into the development of - Wielki Wybuch, a współczesny obraz Ziemi the East African Rift, AGU Fall Meeting 2018, widziany przez instrumenty Laboratorium 10-14.12.2018, USA Geodynamicznym w Książu, XVIII Konfe- 14. Mège, D., Ciażela, M., Pirajno, F., The role of rencja Doktorantów i Młodych Uczonych, 22- ACS in the EXOMHYDR project, ExoMars 25 maj, Szklarska Poręba 2016 ACS Science Working Team Meeting, 24. Zdunek Ryszard, Marek Kaczorowski, Da- 04-05.04.2018, Guyancourt, Francja mian Kasza, Roman Wronowski, Odległe wy- 15. Pożoga Mariusz, H. Rothkaehl, B. Matyjasiak, darzenia kosmiczne - Wielki Wybuch a współ- M. Grzesiak, K. Budzińska, Ł. Tomasik, R. czesny obraz Ziemi widziany przez instru- Wronowski, B. Atamaniuk, A. Pełech, D. menty Laboratorium Geodynamicznego w Przepiórka, PL610 Borówiec, Face-to Face Książu, XVIII Konferencja Doktorantów i ILT-TO meeting, 26-27.09.2018, Olsztyn, Młodych Uczonych, 22-25 maj, Szklarska Polska Poręba 16. Rataj Mirosław, Sz. Polak, R. Pietrzak, WFI/ 25. Ryzenko J. , Możliwości wykorzystania technik Filter Wheel Assembly (FWA) design deve- satelitarnych przez jednostki samorządu tery- lopment, ATHENA/ WFI 7th Consortium torialnego w obszarze monitorowania środo- Meeting, 17-19.04 - 2018 Garching, Niemcy wiska, Zadania własne, zlecone i powierzone 17. Rataj Mirosław, Filter Wheel Assembly cur- jednostek samorządu terytorialnego z zakresu rent status, PROBA-3 Consortium Meeting, ochrony środowiska, Senat RP, 8.01.2018 War- 1-3 10.2018 CSL Liege , Belgia szawa 18. Rybus Tomasz, Estable S., Pruvost C., Luig 26. Ryzenko J., Techniki satelitarne jako możli- K., Hölzer J., Ahrns I., Telaar J., Fruhnert M., wość zwiększenia efektywności działania Imhof Ch., Peckover G., Lucas R., Ahmed R., administracji publicznej, Działalność kosmi- Oki T., Wygachiewicz M., Kicman P., Lukasik czna – prawo i administracja, Senat RP, 28.5. A., Santos N., Milhano T., Arroz P., Biesbroek 2018 Warszawa R., Wolahan A., Capturing and deorbiting 27. Ryzenko J., M. Milczarek, A. Robak, Możli- Envisat with an Airbus Spacetug. Results from wości wykorzystania obserwacji satelitarnych the ESA e.deorbit Consolidation Phase study, w kontekście zarządzania kryzysowego na Clean Space Industrial Days 2018, 23- obszarach morskich, Kosmos a morze – na 25.10.2018, Holandia styku horyzontów, 8.03.2018 Sopot 19. Skup Konrad, WFI/ATHENA PDU Design 28. Ryzenko J., Możliwości wykorzystania nowych Concept, ATHENA/ WFI 8th Consortium rozwiązań satelitarnych i dronowych w ocenie Meeting, 20-22.11.2018 zagrożeń i zwalczaniu pożarów lasów, Semina- 20. Skup Konrad, SWI/JUICE DPU & PSU rium z zakresu ochrony przeciwpożarowej Status, JUICE/SWI 9th Consortium Meeting, lasu Regionalnej Dyrekcji Lasów Państwo- 14-18.05.2018 wych w Zielonej Górze, 11.12.2018 Łagów 21. Skup Konrad, SWI/JUICE DPU & PSU (lubuskie)

125 Other wiecki, S. Aleksandrowicz, M. Jenerowicz, Multifraktalna analiza zobrazowań satelitar- 1. Gurgurewicz J., Mège D., Enigmatyczne wy- nych, Zebranie Sekcji Teledetekcji Komitet stąpienia metanu w atmosferze Marsa: jakie Badań Kosmicznych i Satelitarnych PAN, procesy geologiczne mogą za nie odpowia- Centrum Badań Kosmicznych PAN, 11 gru- dać?, Seminarium "Kierunek: Mars", Pałac dnia 2018 r. Staszica, Warszawa, 06.04.2018 12. Wronowski Roman, M. Kaczorowski, R. Zdu- 2. Kaczorowski M., Zdunek R., Wronowski R., nek, D. Kasza, Laboratorium Geodynamiczne Badania tektonicznych deformacji w Depresji CBK PAN w Książu i wybrane kierunki ba- Świebodzic i jej związków czasowych z dawcze, Seminarium naukowe Ośrodka Bada- aktywnością sejsmiczną w Monoklinie wczego ING PAN, Kraków, 07.03.2018 Przedsudeckie, Seminarium CBK 22.03.2018, 13. Zalewska Natalia, Rootless cones czyli stożki 3. Kaczorowski Marek, R. Zdunek, D. Kasza, R. bez korzeni jako konsekwencja marsjańskiego Wronowski, Laboratorium Geodynamiczne wulkanizmu”, Seminarium CBK, 19.04.2018 CBK PAN w Książu i wybrane kierunki ba- 14. Zalewska Natalia, Problemy badawcze zwią- dawcze, Seminarium naukowe Ośrodka Bada- zane z misjami marsjańskimi", Seminarium wczego ING PAN, Kraków ING PAN, 07 Naukowe Instytutu Lotnictwa, 22.05.2018 marca 2018 roku 15. Zdunek Ryszard, Marek Kaczorowski, Da- 4. Kalarus Maciej, ESA Industry Day: Galileo mian Kasza, Roman Wronowski, Labora- Programme - Second Generation, Semina- torium Geodynamiczne CBK PAN w Książu i rium ZGP, Warszawa CBK PAN, 9.02.2018 wybrane kierunki badawcze, Seminarium nau- 5. Kalarus Maciej, Analiza możliwości pomiaru kowe Ośrodka Badawczego ING PAN, Kra- perturbacji niegrawitacyjnych na pokładzie ków, 2018-03-07 satelitów GNSS, Seminarium ZGP, Warszawa 16. Nawrocki J., P. Dunst, B. Nagórny, D. Le- CBK PAN, 9.11.2018 mański, P. Nogaś, "AOS Laboratory Report", 6. Kalarus Maciej, Propozycja pomiaru prędko- 26th Meeting of the CCTF WG on TWSTFT ści propagacji grawitacji przy użyciu satelitów Central Office of Measures (GUM), 07.07. nawigacyjnych, Seminarium ZGP, Warszawa 2018. – 08.07.2018, Warszawa CBK PAN, 23.02.2018 17. Nawrocki J., P. Dunst, B. Nagórny, D. Le- 7. Lejba Paweł, Tomasz Suchodolski, Piotr mański, P. Nogaś, "Space Research Centre Michałek, Jacek Bartoszak, Stanisław Schillak, PAS Astrogeodynamical Observatory Time & Stanisław Zapaśnik, Laserowe obserwacje Frequency Laboratory Borowiec", Spotkanie śmieci kosmicznych w Obserwatorium CBK w NTSC w Xian Chiny, 06.11.2018. – 08.11. PAN w Borówcu, 2016-2017, Seminarium 2018, Chiny ZGP, Warszawa CBK PAN, 07. 05. 2018 18. Nawrocki J., P. Dunst, B. Nagórny, D. Le- 8. Matyjasiak Barbara, Marcin Grzesiak, Mariusz mański, P. Nogaś, "Fontanny cezowe - 'Pri- Pożoga, Hanna Rothkaehl, Łukasz Tomasik, mary Frequency Standards' w Laboratorium Scyntylacje obserwowane LOFAR'em, Semi- czasu i częstotliwości w Borowcu", Spotkanie narium CBK, Warszawa, 11 10. 2018 w ZGP, 10.08.2018, Warszawa 9. Orleański Piotr, Perspektywy rozwoju firm w 19. Nawrocki J., P. Dunst, D. Lemański, P. Nogaś, obliczu Polskiej Strategii Kosmicznej do 2030 "TWOTFT in Europe", Measures (GUM), roku, Przyszłość Branży Producentów 07.07.2018. – 08.07.2018, Warszawa Elektroniki, Włocławek, 18-19.04.2018 20. Nawrocki J., P. Dunst, B. Nagórny, D. Lemań- 10. Stęślicki Marek, Szymon Gburek, Amir Caspi, ski, P. Nogaś, Activities ath the AOS time nad Piotr Podgórski, Daniel Ścisłowski, Jarosław frequency laboratory, Spotkanie w NTSC w Bąkała, STC: Spectrometer for Temperature Xian Chiny, 06.11.2018. – 08.11.2018, Chiny and Composition Level 3 Requirements, 21. Nogas P., Calibration of GNSS equipment for FOXSI SMEX w Instrument System Require- time transfer”, Effective participation in Co- ment Review, NASA Goddard, 17-18 X 2018 ordinated Universal Time (UTC), luty 2018, 11. Wawrzaszek Anna, M. Krupiński, W. Drze- Francja

126 22. dr hab. inż. Stanisław Lewiński i dr inż. Artur 28. dr hab. Maciej Bzowski "Ciepła Bryza w Nowakowski "Klasyfikacja form pokrycia te- obserwacjach IBEX-a jako źródło informacji renu na zdjęciach Sentinel-2 w skali globalnej - o stopniu jonizacji materii międzygwiazdowej projekt S2GLC (ESA)", Seminarium CBK, w pobliżu Słońca”, Seminarium CBK, 22.02.2018 24.05.2018 23. dr hab. Małgorzata Królikowska-Sołtan "Co 29. dr Edyta Woźniak i S. Aleksandrowicz "Glo- dziś pozostało z pierwotnej hipotezy Oorta?", balne kartowanie pożarzysk na optycznych Seminarium CBK, 01.03.2018 zdjęciach satelitarnych - automatyczny algo- 24. Jakub Ciążela, Marta Ciążela, Pierre Antoine rytm detekcji”, Seminarium CBK, 07.06.2018 Tesson, Daniel Mege "The FNP TEAM 30. dr Piotr Witek "Rzeki i jeziora Tytana - po za- EXOMHYDR project in CBK: 3 years to kończeniu misji Cassini”, Seminarium CBK, identify crustal trace gas sources on Mars”, 14.06.2018 Seminarium CBK, 08.03.2018 31. prof. Wiesław Macek "Turbulencja na skalach 25. prof. Włodek Kofman "Struktura, skład orga- kinetycznych w otoku magnetosfery Ziemi na niczny i mineralogiczny wnętrza komety 67P podstawie danych z magnetosferycznej misji na podstawie obserwacji radaru CONSERT z wieloskalowej MMS", Seminarium CBK, misji ROSETTA", Seminarium CBK, 15.03. 04.10.2018 2018 32. mgr Łukasz Tomasik i dr Mariusz Pożoga 26. dr hab. Andrzej Czechowski "Heliosferyczne "Modele jonosfery wykorzystywane w wybra- ENA w szerokim zakresie energii: Od SO- nych aplikacjach Pracowni Prognoz Heliofizy- HO/HSTOF do IBEX-a" *), Seminarium cznych”, Seminarium CBK, 18.10.2018 CBK, 12.04.2018 33. mgr inż. Gordon Wasilewski "Zasoby kosmi- 27. dr hab. Romana Ratkiewicz „Kilka uwag nt. czne - ich potencjał, wyzwania i przyszłość możliwości rozwiązania dylematu modelo- rozwoju”, Seminarium CBK, 08.11.2018 wania heliosfery”, Seminarium CBK, 17.05. 2018

127 Grants and Contracts Modeling Caliste-So Detectors Respon- ses To X-Ray Illumination Form Solar Fla- National Science Centre Grants res With The Use Of The GEANT4 Tool- 1. Synteza metod sterowania adaptacyjnego dla kit; układów z dynamiczną stabilizacją położenia (Barylak Jaromir, grant - PRELUDIUM, TT/ (robot typu ballbot) 248/2016) Synthesis of adaptive control methods for 9. Analiza pola magnetycznego oraz rekoneksji and under actuated dynamically stable magnetycznej w zewnętrznym otoczeniu he- mobile robot (ballbot type) liosfery. (Wiśniewski Łukasz, grant własny, TT/167/ Analysis of the Magnetic Field and the 13) Magnetic Reconnection in the Outer Re- 2. Udział Polski w projekcie LOFT; gion of the Heliosphere. Polish participation in LOFT mission; (Figura Przemysław, grant - PRELUDIUM, (Michalska Małgorzata, projekt międzynaro- TT/249/2016) dowy niewspółfinansowany, TT/196/14) 10. Polski udział w misji kosmicznej NASA Inter- 3. Rentgenowski polarymetr-spektrometr SOL- stellar Boundary Exploret (IBEX): Skąd PEX pochodzi ciepła bryza i jaki ma związek z asy- X-ray polarimeter-spectrometer SOLPEX metrią heliosfery?; (Sylwester Janusz, grant własny, TT/197/14) Polish Participation In The Nasa Space 4. Badanie krótkotrwałych zjawisk świetlnych Mission Interstellar Boundary Explorer (TLE) oraz ziemskich błysków gamma (TGF) (Ibex): What In The Source For The Warm w górnej atmosferze ziemskiej; Breeze And How Is It To The Asymmetry Studies of the transient luminous events Of The Heliosphere?; (TLE) and terrestrial gamma flashes (Bzowski Maciej, projekt międzynarodowy (TGF) in the upper Earth's atmosphere; niewspółfinansowany, TT/250/2016) (Błęcki Jan, grant własny, TT/215/15) 11. Udział Polski w naukowym rozwoju nowego 5. Analiza modeli ziemskich ośrodków ciekłych teleskopu rentgenowskiego ATHENA; oraz modeli klimatycznych CMIP celem ich Polish Contribution In Scientific Develop- weryfikacji pod względem zgodności ich ment New XRay Telescope ATHENA; ekscytacji ruchu bieguna z obserwowanymi (Rataj Mirosław, projekt międzynarodowy zmianami tego ruchu; niewspółfinansowany, TT/255/2016) Analysis of geophysical surficial fluids 12. Ośrodek międzygwiazdowy w okolicy Słońca: models and CMIP climate models for ve- wnioski z analizy obserwacji strumieni ato- rification of polar motion excitation fun- mów neutralnych; ctions in terms of their compatibility with Interstellar medium in the vicinity of the changes in the observer polar motion; Sun: inferences from analysis of the flux (Nastula Jolanta, grant własny, TT/216/15) of neutral atoms; 6. Analiza turbulencji w plazmie kosmicznej; (Bzowski Maciej, grant własny, TT/256/ Analysis of Turbulence in Space Plasmas; 2016) (Macek Wiesław, grant własny, TT/230/15) 13. Rentgenowski spektrometr obrazujący STIX: 7. Powstawanie pęcherzyków w skorupie obto- symulacje rekonstrukcji widm i obrazów rent- pieniowej meteorytów eukrytowych; genowskich Formation Of Vesicles Within The Fusion X-Ray imaging spectrometer STIX: si- Crust Of Eucritic Meteorites; mulations of spectra and images recon- (Nicolau-Kuklińska Agata, grant - PRELU- struction DIUM, TT/247/2016) (Sylwester Janusz, grant własny, TT/258/ 8. Modelowanie Odpowiedzi Detektorów 2016) Caliste-So Na Oświetlenie Promieniowaniem 14. Mobilność nieholonomicznych robotów ko- Rentgenowskim Rozbłysków Słonecznych Z smicznych w obecnosci przestrzennie rozle- Użyciem Pakietu Geant4; głych przeszkód posiadających moment pędu "NONHOLONOMIC";

128 Mobility Of A Nonholonomic Space Ro- 21. Badanie zmian parametrów fizycznych górnej bot Constrained By Large Movable Obsta- jonosfery wywoływanych wyładowaniami ele- cles; ktrycznymi w atmosferze; (Sąsiadek Jerzy, grant własny, TT/259/2016) The studies of the changes of the upper 15. V-MACS: Nowy obraz gigantycznego mars- ionospheric physical parameters caused jańskiego systemu kanionów; by electric discharges in the atmosphere; V-MACS - Novel views of the Martian (Błęcki Jan, grant własny, TT/293/18) giant canyon system; 22. Badanie rozbłysków słonecznych na podsta- (Mege Daniel, grant własny, TT/261/16) wie obserwacji wykonanych za pomocą pol- 16. Polski wkład w przygotowanie i przeprowa- skiego spektrofotometru SphinX; dzenie programu badawczego projektu CTA The investigations of solar flares based on w pierwszej fazie działania; the data of Polish spectrophotometer Polish input into preparation and realiza- SphinX; tion of the first phase of CTA scientific (Gryciuk Magdalena, grant - ETIUDA, TT/ program; 298/ 18) (Seweryn Karol, projekt międzynarodowy niewspółfinansowany, TT/271/2017) National Centre for Research 17. Ocena przydatności formalizmu multifrak- and Development Grants talnego w przetwarzaniu i analizie optycznych 1. Penetrator planetarny z systemem pobierania obrazów teledetekcyjnych; gruntu na misje Luna-Resurs 1; Evaluation of the usefulness of multifrac- Planetary penetrator equipped with a soil tal formalism in the processing and ana- sampling system intended for the Luna- lysis of optical remote sensing images; Resurs 1 mission; (Wawrzaszek Anna, grant własny, TT/273/ (Barciński Tomasz, TT/214/15) 2017) 2. Woda w glebie - monitoring satelitarny w po- 18. Ocena równoważnego słupa wody uzyska- prawie retencji wodnej przy użyciu biowęgla nego z modeli klimatycznych CMIP5 na pod- (SoilAqChar); stawie pomiarów satelitarnych GRACE; Water in soil - satellite monitoring and im- Evaluation of the CMIP5 equivalent water proving the retention using biochar (Soil- thickness output using GRACE satellite AqChar); observations; (Słomiński Jan, BIOSTRATEG, TT/285/18) (Wińska Małgorzata, grant - MINIATURA, TT/276/2017) Ministry of Science and Higher 19. Badanie stanu plazmy w rozbłyskach słonecz- nych na podstawie analizy widm rentgenow- Education Grants skich uzyskanych za pomocą przyrządu Bent 1. Badania kosmiczne dla młodych naukowców - Crystal Spectrometer z pokładu satelity NA- Odyseusz 2; SA Solar Maximum Mission; Youth for space challenge - Odysseus 2; Investigation of physical conditions in (Gabryszewski Ryszard, wsparcie uczestnic- flaring plasma based on the analysis of X- twa jednostki w programie HORYZONT ray spectra observed by Bent Crystal Spec- 2020, TT/211-M/17) trometer on NASA Solar Maximum Mis- 2. Europlanet 2020 Infrastruktura Badawcza; sion satellite; Europlanet 2020 Research Infrastructure; (Sylwester Barbara, grant własny, TT/286/18) (Tomasik Łukasz, wsparcie uczestnictwa 20. Reprezentatywność globalnych ocen zachmu- jednostki w programie HORYZONT 2020, rzenia z satelitarnych misji lidarowych i rada- TT/232-M/17) rowych (LiRa-C); 3. Wsparcie monitorowania skuteczności serwi- Representativeness of global lidar and ra- su EGNOS; dar climate record on clouds (LiRa-C); (Świątek Anna, międzynarodowy współfinan- (Kotarba Andrzej, grant własny, TT/284/18) sowany, TT/233-1M/17)

129 4. LOFAR dla Pogody Kosmicznej; 7. Centrum Referencyjne Galileo-Krajów człon- LOFAR for Space Weather; kowskich; (Rothkaehl Hanna, wsparcie uczestnictwa Galileo Reference Centre - Member Sta- jednostki w programie HORYZONT 2020, tes; TT/288-M/18) (Świątek Anna, TT/296/18) 5. Wprowadzanie innowacji w zarządzaniu kry- 8. Nowoczesny moduł sterowania i przetwarza- zysowym w Europie (DRIVER+); nia danych dla platformy i aparatury sateli- Driving InnoVation in crisis manage- tarnej na pokładzie mikrosatelitów; ment for European Resilience + (DRI- Future control and data handling unit for VER+); platforms and payloads for micro- (Foks-Ryznar Anna, międzynarodowy współ- satellites; finansowany,TT/274-M/18) (Orleański Piotr, POIR,TT/300/18) 9. Wsparcie Monitorowania Wyników Systemu EU Programme Grants EGNOS; EGNOS Service Performance Monitoring 1. Europlanet 2010 Infrastruktura Badawcza; suport (SPMS) Specyfic Agreement No3; Europlanet 2020 Research Infrastructure; (Świątek Anna, GNSS, TT/311/19) (Tomasik Łukasz, HORYZONT 2020, TT/232/15) 2. Wsparcie Monitorowania Wyników Systemu ESA Grants EGNOS; 1. Zespół koła z filtrami i polaryzatorami; EGNOS Service Performance Monitoring Sterownik koronografu dla misji PROBA3; suport (SPMS) Specyfic Agreement No1; PROBA 3 Coronagraph Control Box (P3 (Świątek Anna, GNSS, TT/233-1/16) CCB) Filter Wheel Assembly & Polarisers 3. Wspieranie innowacyjności w zarządzaniu (FWA); kryzysowym – DRIVER; (Rataj Mirosław/Cichocki Andrzej, TT/193/ Driving Innovation in Crisis Management 15) for European Resilience; 2. Polski udział techniczny w fazie D projektu (Foks-Ryznar Anna, 7PR, TT/274/15) STIX/Solar Orbiter (STIX-D); 4. EXOMHYDR – Wpływ systemów magmo- Polish Technical Participation in Phase D wych i tektoniki na aktywność hydrotermalną of STIX/Solar Orbiter; na Marsie w świetle badań misji ExoMars/ (Skup Konrad, PRODEX, TT/198/14) TGO: warunki dla obecności życia i zasobów 3. Galileo i akcelerometry; naturalnych; Galileo and Accelerometers (GalAc); EXOMHYDR – Magmatic plumbing sys- (Kalarus Maciej, TT/203/14) tems and tectonic control of hydrother- 4. Robotycznie wspierane ladowanie (REST); mal activity on Mars revealed by Exo- Robotically Enhanced Surface Touch- Mars/TGO: constraints for life and reso- down/REST; urces; (Seweryn Karol, TT/204/14) (Mege Daniel, POIR,TT/280/17) 5. Badanie związków między nocnym wzrostem 5. System operacyjnego gromadzenia, udostęp- koncentracji plazmy jonosferycznej a zmien- niania i promocji cyfrowej informacji sateli- nością pola magnetycznego; tarnej o środowisku (Sat4Envi); Investigation of the linkage between System of operational collection, sharing, ionospheric plasma night-time density and promotion of digital satellite data enhancements and magnetic field varia- about the environment (Sat4Envi); bility; Foks-Ryznar, POPC, TT/283/17) (Błęcki Jan, TT/212.1/18) 6. LOFAR dla Pogody Kosmicznej; 6. Polska realizacja instrumentu RPWI dla misji LOFAR for Space Weather; JUICE; (Rothkaehl Hanna, HORYZONT 2020,TT/ Overall contribution to the RPWI instru- 288/18)

130 ment for JUICE mission; Testing the Potential of the PaaS (plat- (Rothkaehl Hanna, TT/217.1/14) form as a Service) Solution for Ionosphe- 7. OPS-SAT faza B2/C/D/E1; ric Segment of the Space Weather Domain OPS-SAT phase B2/C/D/E1; (SW satellite); (Rajkowski Tomasz, podwykonawstwo, TT/ (Dziak-Jankowska Beata, TT/292/17) 222/15) 17. WFI (WIDE FIELD IMSAGER) Na Pokła- 8. Jupiter Icy Moons Explorer (JUICE) Submil- dzie Satelity ATHENA. Projekt I Wykonanie limetre Wave Instrument - misja ESA L2; Dwóch Podsystemów: Filter Wheel Assembly Jupiter Icy Moons Explorer (JUICE) Sub- (FWA)( Zespół Koła Z Filtrami) Oraz Power millimetre Wave Instrument - misja ESA Distribution Unit(PDU) - System Rozdziału L2; Mocy; (Skup Konrad, TT/223/13) Wfi (Wide Field Imager) On Board Of 9. Wykorzystanie Naukowe Operacyjnych Misji Athena (Advanced Telescope For High Obserwacyjnych (SEOM) S2-4Sci Woda i Energy Astrophysics) Satellite. Design Lądy, Studium 3: Klasyfikacja; And Manufacture Of Two Subsystems:- Scientific Exploitation of Operation Mis- Filter Wheel Assembly (Fwa),- Power sions (Seom) S2-4sci Land and Water, Stu- Distribution Unit (Pdu; dy 3: Classification; (Rataj Mirosław, TT/294/18) (Lewiński Stanisław, TT/246/15) 18. Rolnictwo w Polsce. System informacji statys- 10. Eksperckie centra pogody kosmicznej: defini- tycznej dla rolnictwa w oparciu o dane sateli- cja i rozwój; tarne / Eostat; Space Weather Expert Service Centres: Agriculture Poland. Services for Earth Definition And Development; Observation- Based Statistical Informa- (Dziak-Jankowska Beata, TT/254/16) tion for Agriculture / Eostat; 11. Obserwacja Ziemi dla Partnerstwa Wschod- (Woźniak Edyta, TT/295/18) niego (EO4EP); 19. Odbiornik GNSS dla małych rakiet nośnych i Earth Observation For Eastern Partner- mikro-satelitów na bazie radia programo- ship (E04EP); walnego; (Milczarek Marta, TT/257/16) Sw defined radio GNSSW receiver for 12. Lekki, kompaktowy system optyczny bazujący micro-launchers and micro-satellites; na DOE i Elementach asferycznych (DOE); (Wawrzaszek Roman, TT/297/18) A Lightweight, compact optical system 20. Serwis monitoriningu obszarów zabudowa- based on DOE; nych Mazowsza/BAMS-Mazovia; (Rataj Mirosław, podwykonawstwo, TT/275/ Built-up Areas Monitoring Service for 17) Mazovvia/BAMS-Mazovia; 13. HIPERO: Rekonfigurowalny Komputer Po- (Malinowski Radosław, TT/301/18) kładowy o Dużej Mocy Obliczeniowej; 21. Udział techniczny w projekcie Athena/XIFU; HIPERO: High Performance Reconfi- Technical Participation in Athena/XIFU; gurable OBC; (Skup Konrad, TT/302/18) (Cichocki Andrzej, TT/279/17) 22. Planowanie obserwacji SST przez internet; 14. LOOP - Lądując raz na Fobosie; WebPlan: Web-based sensor planning LOOP - Landing Once On Phobos; tools SST; (Barciński Tomasz, TT/281/18) (Lejba Paweł, TT/303/18) 15. Faza konsolidacyjna misji e.Deorbit; 23. Fine Guidance System (FGS) misji ESA AR- E.Deorbit Consolidation Phase; IEL (Atmospheric Remote-sensing Infrared (Rybus Tomasz, TT/290/18) Exoplanet Large-survey) – M4 mission. Faza 16. Testowanie potencjału rozwiązania PaaS ( pla- B1- FGS/ ARIEL; tforma jako usługa ) dla segmentu jonosfery- (Rataj Mirosław, TT/309/18) cznego domeny pogody kosmicznej;

131 Projects supported by other 6. Udział w opracowaniu projektu pomiaru GNSS kolejowej osnowy geodezyjnej oraz Polish organizations and opracowanie obserwacji i sporządzenie spra- institutions wozdania z opracowania obserwacji GNSS; Participation in the project and the GNSS 1. Dostarczanie danych obserwacyjnych GPS, measurements of the railway geodetic pochodzących ze stacji referencyjnej BOR1 control network. Computation of observa- znajdującej się w Borowcu; tions and preparation of a report; Providing GPS observational data from re- (Jaworski Leszek, TT/289/18) ference stations BOR1 located in Boro- 7. Opracowanie opinii eksperckiej co do jakości i wiec; merytorycznej poprawności w zakresie prze- (Lejba Paweł, TT/7.10/17) twarzania danych satelitarnych; 2. Bieżące opracowanie zestawu danych helio- Experts opinion about quality and merits geofizycznych do prognozowania warunków related accuracy referring to satellite data łączności radiowej oraz rozwój metodyki i sys- analysis; temów prognozowania warunków łączności (Lewiński Stanisław, TT/291/18) radiowej; 8. Opracowanie wektorowej warstwy wylesień w The current development of a heliophysic latach 2016-217 na terenie m. st. Warszawy na data set to predict conditions of the radio podstawie danych satelitarnych Sentinel-2 na communication and the development of potrzeby "Aktualizacji opracowania ekofi- methodologiest and forecasting systems zjologicznego podstawowego do polityki of radio communication conditions; przestrzennej m.st. Warszawy wyrażonej w (Dziak-Jankowska Beata, TT/67.6/16) studium uwarunkowań i kierunków zagospo- 3. Projekt, wykonanie i testy hiperspektralnego darowania przestrzennego m.st. Warszawy”; spektrometru obrazującego; (Aleksandrowicz Sebastian, TT/299/18) Design, manufacturing and tests hyper- 9. Projekt, pomiar techniką GNSS i opracowanie spectrak imaging spectrometers; szczegółowej osnowy dwufunkcyjnej na tere- (Rataj Mirosław, TT/278/17) nie powiatu lubartowskiego; 4. Opracowanie intefejsu pomiędzy modułem (Jaworski Leszek, TT/304/18) uruchomieniowym MAX2769EVKIT i płyta 10. Rozwój Badań Kosmicznych; ewaluacyjną GR-CPIC-GR740; (Denis Mirosław, program Akademickie Part- Design of interface between MAX2769 nerstwa Międzynarodowe, TT/305/18) EVKIT and GR-CPIC-GR 740 develop- ment board; Projects supported by other (Wawrzszek Roman, TT/282/18) 5. Opracowanie systemu pozycjonowania i kon- foreign organizations and troli orientacji satelity (AOCS - Attitude and institutions Orbital Control Systems) dla platformy sateli- 1. Techniczna obsługa stacji EGNOS-RIMS; tarnej HyperCube budowanej w ramach Pro- Technical service of the EGNOS-RIMS jektu Renesans; station; Design and development of positionning (Jaworski Leszek, TT/13.3/13) and orientation control system (AOCS - 2. Jonosonda LAERT; Attitude and Orbital Control Systems) for LAERT Ionosonde; HyperCube satellite platform under deve- (Rothkaehl Hanna, TT/68/10) lopment in a frame of Renesans project; (Wawrzaszek Roman, TT/287/18)

132 Monitoring the sustainability 2. Development of the remote sensing facilities of the projects co-financed in Centrum Badań Kosmicznych PAN (RPO from European funds WM 207-2013). 3. PROTEUS. Integrated mobile system for coun- CBK PAN monitors the projects co-financed terterrorism and rescue operations (POIG). from European structural funds after the com- 4. Future control and data handling unit for pletion of their implementation in the life of the platforms and payloads for microsatellites project. The monitoring covers the output and (POIR). outcome indicators as outlined for each projects. 5. EXOMHYDR. Magnetic plumbing systems The following projects are under monitoring: and tectonic control of hydrothermal activity 1. SPEKTROP. Elaboration of imaging and on Mars revealed by ExoMars/TGO cons- spectrum analyzing systems designed for ob- traints for life and resources (POIR). servation of remote objects (POIG 1.3.1). (M. Michalska)

133 GENERAL INFORMATION Staff research associates. Paweł Swaczyna, Przemy- sław Figura, Tomasz Rybus were advanced with At the end of 2018 the Centrum Badań Kosmi- PhD degree. cznych, PAN employed 203 persons of whom 16 (H. Żurek) are professors, 15 habilitated doctors and 42 PhD

Finances – preliminary estimates The state budget of Centrum Badań Kosmicz- 11% national grants, 10% EU framework pro- nych, PAN, in 2018 was 11.785 thousand PLN jects, 21% contracts (national and international, while total was 32.904 thousand PLN. The budget ESA), 22% other sources. structure was following: 36% basic allocation, (W. Roszkowska) Grants and Contracts Centrum Badań Kosmicznych, PAN was involved for Research and Development, 23 from ESA, 9 in 73 projects including 5 from the Ministry of from EU Programme including 3 funded by the Science and Higher Education, 22 from the Na- EU Structural Funds, and 12 other contracts. tional Science Centre, 2 from the National Centre (A. Kamińska) Intellectual Rights Management Policy Polish Patent No 227712 United State Patent No US 9995096 B2 Title: Zwierciadło oraz sposób wykonywania Title: Drilling Head driving device, spragging zwierciadła mechanism and drilling method Assignee: Centrum Badań Kosmicznych PAN Assignee: Centrum Badań Kosmicznych PAN, Developer: K.Seweryn, M.Rataj, P.Wawer, Akademia Górniczo-Hutnicza M.Karczewski, Ł. Wiśniewski Developer: K. Seweryn, T.Kuciński, K.Grassmann (M. Michalska) Awards Prof. Włodek Kofman - Andre Lallemand from the space sector in Poland (under 30 years of Award of the French Academy of Sciences for his age). The competition was organized by Industrial work on Mars and comets. Development Agency JSC (Agencja Rozwoju Gordon Wasilewski - Hope of the Polish Space Przemysłu SA). M. Sc. Gordon Wasilewski is the Sector award in frame of Constellation 2018 researcher at the CBK PAN and a grant holder of Competition, granted to the young employees the Colorado School of Mines.

134 Activities inside and outside of Poland Institute's employees were actively involved in laboratory work, diagnostic stations and observatories operating within the Centre structures: IONOSOND (Warsaw) —monitoring the iono- Analysis Centers (Acs ILRS), Crustal Dynamics sphere over Warsaw for the purposes of telecom- Data Information System (CDDIS) and Eurolas munication and navigation Data Center (EDC) data banks; observations of Crisis Information Center —the use of satellite so called ‘Space junk’ by the Space Debris Study imagery to improve performance in the area of Group. emergency and crisis management. PL LOFAR 610 Borowiec - operate in an inter- International forecasting centre for cosmic national network of telescopes LOFAR ILT weather - collecting real-time data about the sta- International Lofar Telescope, which consists of tus of the space activity around Earth and Sun for 50 stations located in Europe; LOFAR was desi- the purpose of forecasting potential problems af- gned to test the frequency range between 30 - 240 fecting economic processes (in particular, com- Mhz; scintillation receiver, a digital radio receiver munication and navigation); results are used both for the diagnosis of the ionosphere and riometr public and private sector were located in Borowiec. International Space Environment Service CBKA station (Warsaw) — permanent GPS ISES - an international organisation coordinating observations for national network ASG-EUPOS; quick exchange of data on the Sun, and Earth's used for the purpose of calculating precise RTK environmental corrections for the system users; station defines IDCE (Ionospheric Dispatch Centre in the national spatial reference system Europe)—European centre for gathering and CBKS station - permanent GPS observations - distribution of ionospheric data EGNOS in the frame of the IMAGE/ PER- Mobile GNSS Laboratory — examining accu- FECT (ESA) project. GWAR station — perma- racy and quality of EGNOS corrections in the nent GPS and GA-LILEO observations; station field working in experimental network of stations tra- Presence on the Polish Polar Station HORN- cking GALILEO system SUND — local monitoring of conditions in the RIMS station of EGNOS system (Warsaw) - space around the Earth using: ionosond, GPS re- permanent GNSS observation for the purpose of ceiver and receivers to measure the absorption creating EGNOS correction Regional Warning Centre Warsaw — branch The Geodynamic Laboratory of the Centrum of International Space Environment Service Badań Kosmicznych PAN in Książ - perma- (ISES) nent observations of tidal and non tidal signals of Service of Time and Frequency (Astrogeo- gravity, and plumb line variations as well as tecto- dynamic Observatory in Borowiec) - AOS Boro- nic deformations of Świebodzice Depression wiec time distribution on the Internet; providing Massive; investigation of tidal, recent tectonic master frequency for POLKOMTEL S.A activity and middle-high frequency oscillations. BOR1 station (Astrogeodynamic Observatory in • The use of geodetic poles at the Observatory in Borowiec) permanent GPS observations; station Borowiec for surveying companies working in IGS, EPN and ASG-EUPOS stru- • Guest rooms ctures; data used to determine a global reference system ITRF, regional development in Europe, CBK PAN is part of 40 scientific and to define the national spatial reference system consortia, among them: International Laser Ranging Service (Astro- geodynamic Observatory in Borowiec) Laser Discorsi Galilei, 2007, topics related to the measurements of Artificial Satellites movement, European Galileo satellite system project, Galileo; providing data for international services and Centrum Badań Kosmicznych Polskiej Akademii databases of International Laser Ranging Service Nauk; Institute of Communications, Naval

135 Academy; Warsaw University of Technology; The Badań Kosmicznych Polskiej Akademii Nauk, the University of Warmia and Mazury in Olsztyn; Swedish Institute of Space Physics (IRF) and the The Polish Air Force Academy is located in Dę- experiment RPWI (Radio Plasma Waves Investi- blin; Polspace. gation) - diagnostics of electric and magnetic DRIVER+, 2014, A scientific and industrial con- fields, and measurements of the electron and ion sortium to implement the project "Driving Inno- space plasma properties, Swedish Institute of vation in Crisis Management for European Resi- Space Physics, IRF-u, LESIA - Observatoire de lience" (DRIVER +) financed by the 7th Euro- Paris; Institute of Atmospheric Physics, Prague; pean Union Framework Program. It brings toget- Tohoku University, Sendai, Japan; Space and her institutions and companies from over 14 Atmospheric Physics group at Imperial College countries representing practitioners in the field of London; Royal Institute of Technology KTH crisis management and rescue, non-governmental Sweden; Université d'Orléans, France; 8. Ecole organizations dealing with humanitarian aid, Polytechnique, France; Observatoire de Paris; technology providers and scientists. Université de Toulouse, France; Astronomical ESPAS; 2011; integration of e-science data STFC Institute of the Czech Academy of Sciences; The Rutherford Appleton Laboratory, Oxfordshire, Institute of Atmospheric Physics in Prague, UK; National Observatory of Athens, Greece; Czech Republic; University of Sheffield, UK; EISCAT Scientific Association, Kiruna, Sweden; Space Research Institute, Austrian Academy of DLR Neustreitz, Germany; INGV, Rome, Italy; Sciences, Graz, Austria; Kyoto University, Kyoto, JFWconsult, France; IPAG, Grenoble, France; Japan; Kanazawa University, Japan. Athena Research Centre, Athens, Greece; Univer- National Centre of Radioastronomy and En- sity of Oulu, Finland; Sodankyla Geophysical gineering; 2012; technical science, space explo- Observatory, Finland; University College Lon- itation, transfer, processing data and radio- don, UK; Met Office, Exeter, UK; University of astronomy; Nicolaus Copernicus University, Birmingham, UK; Belgian Institue for Space Gdańsk University of Technology, Military Uni- Aeronomy, Brussels, Belgium; Centrum Badań versity of Technology, Centrum Badań Kosmi- Kosmicznych Polskiej Akademii Nauk, Warsaw, cznych PAN, Jagiellonian University, University Poland; Technical University of Denmark, Nati- of Zielona Góra, Nicolaus Copernicus Astrono- onal Space Institute, Copenhagen, Denmark; mical Center PAS, University of Technology and Finnish Meteorological Institute, Helsinki, Fin- Life Sciences, Institute of Bioorganic Chemistry land; University of Leicester, UK; GeoForsch- PAS. ungsZentrum Potsdam, Germany; Royal Obser- Polish Consortium of the Project "Cherenkov vatory of Belgium, Brussels, Belgium; DH Con- Telescope Array” 2010, Faculty of Physics, sultancy, Leuven, Belgium; Lowell Digisonde In- Astronomy and Applied Computer Science of the ternational. Jagiellonian University; Nicolaus Copernicus GeoPlanet; 2009; geophysics, oceanography, Astronomical Center of the Polish Academy of geology, space physics; Centrum Badań Kosmicz- Sciences; Polish Academy of Sciences Faculty of nych Polskiej Akademii Nauk, Geophysics Insti- Physics and Applied Informatics (University of tute PAS, Institute of Geological Sciences PAS, Łódź); The Henryk Niewodniczański Institute of Institute of Oceanology PAS, Nicolaus Coper- Nuclear Physics (Polish Academy of Sciences); nicus Astronomical Center PAS. Faculty of Physics, University of Warsaw (xPolish JUICE 2014; network founded to carry out the Academy of Sciences); Department of Physics, experiment SWI (Submillimeter Wave Instru- Astronomy and Applied Informatics Nicolaus ment) of mission ESA JUICE (execution of mo- Copernicus University; Centrum Badań Kosmicz- dules DPU, PSU and subsystems of the telescope nych; AGH University of Science and Technology mechanism) - Observatoire de Paris, LESIA, of Stanisław Staszic in Cracow, Faculty of France, Observatoire de Paris, LERMA, France, Electrical Engineering, Automatics, Computer Chalmers, Sweden, University of Bern, Switzer- Science and Biomedical Engineering (Polish land, NICT, Japan, Omnisys Instrument AV, Academy of Sciences). Sweden, Radiometer Physics GmbH, Centrum

136 CBK PAN is part of scientific nasa.gov/network/stations/active/index.html networks, among them: Satellite Geophysics, 2005, satellite geophysics, IG PAN, IGIK, CBK PAN, UW, PW AirClim-Net, 2005, problems of atmospheric International Laser Ranging Service; 1997; pollution and climate change, http //www.airclim coordination of satellite and lunar laser stations, -net.eu/ analysis centers, laser technology data banks, 42 ASG-EUPOS – Active Geodetic Network - laser stations, 29 Analysis centers, 2 Data banks European POsition determination System, ..., National Center for Space and Satellite coordination of GNSS measurements and their Engineering; 2013; space and satellite enginee- transfer in real time to the computing center; 126 ring, Military University of Technology in War- stations, full description available at the: saw, Centrum Badań Kosmicznych Polskiej Aka- http//www.asgeupos.pl/index.php?wpg_type=s demii Nauk; yst_descr&sub=ref_st. International Space Environment Service - EUROLAS – EUROpean LASer Network, 1989, ISES; 1977; cosmic weather; 22 local branches lo- coordination of satellite and lunar laser measu- cated around the world, Regional Warning Cen- rements and observational campaigns carried out ters (RWC), e.g. RWC Warsaw. by European stations, 16 stations:http//ilrs.gsfc. CBK PAN organized and co-organized conferences and meetings:

National: 9. Prof. Janusz Sylwester, „Widma jonów Ca XV 1. Interdyscyplinarne Kształcenie w Przedmio- – Ca XIX otrzymane za pomocą przyrządu tach Przyrodniczych i Ścisłych, Łódź, 28.02. Diogeness, problemy ich redukcji i analizy”, 2018 Seminarium heliofizyczne, Instytut Astrono- 2. VII seminarium Sekcji Teledetekcji KBKiS miczny Uniwersytet Wrocławski, 21.05.2018 PAN, Obserwacje satelitarne, przykłady zasto- 10.Prof. Barbara Sylwester „Emisja rentgenowska sowań, część II, Warszawa, 28.05.2018 Słońca podczas minimum aktywności”, Semi- 3. VII seminarium Sekcji Teledetekcji KBKiS narium heliofizyczne, Instytut Astronomiczny PAN, Obserwacje satelitarne, przykłady zasto- Uniwersytet Wrocławski, 16.04.2018 sowań, część III, Warszawa, 11.12.2018 11.Żanetta Szaforz „Spektroskopia korony 4. Sympozjum "Kierunek Mars", Warszawa, słonecznej z wykorzystaniem prawa Bragga”, 06.04.2018 Seminarium heliofizyczne, Instytut Astrono- 5. Dr. Szymon Gburek “The Focusing Optics X- miczny Uniwersytet Wrocławski, 12.03.2018 ray Solar Imager (FOXSI)”, Seminarium helio- 12.Prof. Marek Siarkowski „Co "zobaczy" fizyczne, Instytut Astronomiczny Uniwersytet STIX?”, Seminarium heliofizyczne, Instytut Wrocławski, 05.11.2018 Astronomiczny Uniwersytet Wrocławski, 6. Anna Kępa „Rozkłady różniczkowej miary 08.01.2018 emisji otrzymane w oparciu o widma zmierzo- International: ne spektrometrem RESIK”, Seminarium he- 1. Conference of the Polish-Russian Workgroup liofizyczne, Instytut Astronomiczny Uniwer- for Fundamental Space and Satellite Research, sytet Wrocławski, 22.10.2018 Warszawa, 22-24.10.2018 7. Dr. Tomasz Mrozek „Katalog zatrzymanych 2. SAT Project M5 Final Meeting, Warszawa, 28- erupcji”, Seminarium heliofizyczne, Instytut 29.03.2018 Astronomiczny Uniwersytet Wrocławski, 3. ATHENA/WFI Progress Meeting, Warszawa, 15.10.2018 11-12.10.2018 8. Jaromir Barylak „Symulacje tła pochodzącego 4. JUICE/ SWI CBK face to face Meeting, od luminescencji w przyrządzie Rotating Warszawa, 7.07.2018 Drum Spectrometer/SOLPEX”, Seminarium heliofizyczne, Instytut Astronomiczny Uni- wersytet Wrocławski, 04.06.2018

137 EDUCATIONAL AND PROMOTIONAL ACTIVITIES

Doctoral studies ideal sphere, but it is flattened at poles and what are the consequences of that fact. There were 23 students in the Doctoral Studies in In addition, presentations of scientific instru- Centrum Badań Kosmicznych PAN in 2018, 4 ments, developed in the CBK and currently new students were admitted in 2018. operating in space on different satellites and the Trainings and internships International Space Station ISS, took place. in CBK PAN Additionally, on this day every half an hour, 15-20 minute screenings took place in the mobile Edu- 39 external scientists, engineers and students cational Center Planetarium “Planeta Anuka”. participated in the trainings and internships in On the 25th and 27th of September 2018, as part of various research groups and laboratories of CBK the 22nd Scientific Festival, academic lectures for PAN in 2018. high school students took place: - "Asteroid collisions with Earth - what was 100 years ago List of activities undertook by the and what will happen in 100 years?" (Prof. M. employees of Centrum Badań Królikowska-Sołtan) Kosmicznych, PAN: - "Space technologies in everyday life" (Dr. J. Ryzenko) - "Climate change on Mars" (dr P. Witek) SCIENCE FESTIWALS AND PICNICS - "Modern space technologies in the world and in Poland" 22nd Science Picnic in Warsaw, 9.06.2018 - this (Dr. P. Orleański) year's main theme was "Movement". Shows. At 21st Lower Silesian Festival of Science, 21- the CBK PAN stands, one could see the "Earth 26.09.2018, 11-25.10.2018; classes with children circulation movement around the Sun" and pre- (A. KĘPA); popular science lectures: "Methane sentations on the issues related to the Earth's rota- riddle in the atmosphere of Mars: Where does it come tion (including day and night, daily change of from and what does it tell us?" (J. CIĄŻELA, M. time, the change of the Sun's height over the CIĄŻELA, J. GURGUREWICZ, D. MEGE), horizon during the day, star movement in the sky "Dark matter and mass extinctions", "The future of over a day, flattening of the Earth at the poles, Earth and the Sun" (M. STĘŚLICKI), "FOXSI: a Coriolis force). We explained why Earth is not an new heliophysical NASA mission" (S. GBUREK ); ideal sphere, but it is flattened at poles. The se- display of space devices (S. GBUREK, Z. cond demonstration concerned the movement of KORDYLEWSKI, Ż. SZAFORZ, J. BĄKAŁA, artificial Earth satellites. We also learned why P. PODGÓRSKI, M. GRYCIUK) satellites do not fall on Earth. There were also ga- Night at the Institute of Aviation, 12.10.2018 - mes and activities for children, a show of photos lecture: "Research problems of Planet Mars" (N. from Mars and a presentation of the future Mar- Zalewska) tian base. 22nd Warsaw Science Festival 2018, 23.09.2018 CBK held an Open Day event. On this day our employees were talking, also to the youngest guests, about many subjects; among others about Mars, our nearest neighbor in the solar system - what is this planet like, how we study it and how we get to know it. There were workshops demonstrating how the nucleus of the comet is formed and how the impact craters are created. Younger children took part in numerous competitions and educational games, solved crosswords and puzzles. Older children readily listened to talks and various Fig. 1. Educational lesson for children. presentations, including: why satellites do not fall on Earth. We also explained why Earth is not an

138 Fig. 2. XXII Warsaw Science Festival 2018 in CBK PAN.

139 EXHIBITIONS OF RESEARCH EQUIPMENT 2nd Space Sector Forum, 24.05.2018 - an exhibi- Exhibition and organization of the children's tion of achievements of Polish entities in the stand during the 2nd Final of “Choinka dobrych space sector and supporting institutions that took serc” (Charity foundation) 17.12.2018. Our scien- place at the Warsaw EXPO XXI Center. CBK tists prepared attractions for young and older PAN was the organizer of the exhibition. children. Children under the age of six indepen- Exhibition at the Presidential Palace accompa- dently built rockets, satellites and even comets. nying the conference "Modern technologies. Enthusiasts of intellectual entertainment were Space industry" 22.10.2018. CBK presented the confronted with cosmic puzzles. Youth learned BRITE-PL satellite, a scanner for the Mertis about the secrets of the organization of space spectrometer for the BepiColombo mission to missions, including the construction of satellites Mercury, a power module for the CaSSiS camera and scientific instruments built at the CBK PAN for the ExoMars mission and a penetrator for the (including instruments for the BRITE, Rosetta, ROSETTA mission. BepiColombo and Trace Gas Orbiter missions). "Poland in Space" exhibition at the Copernicus Everyone could see how Mars presents itself in Science Center on the occasion of the Insight front of the lenses of the space probes and how mission landing on Mars 26.11.2018. the manned bases on the Red Planet will look like in the future.

Fig. 3. 2nd Space Sector Forum, 24.05.2018

140 Fig. 4. Exibition of CBK PAN’s space instruments during 2nd Space Sector Forum, 24.05.2018.

Fig. 5. Educational lessons during 2nd Final of “Choinka dobrych serc” (Charity foundation) 17.12.2018.

141 VISITS AT CBK LECTURES AND TALKS OUTSIDE OF In 2018, there were numerous groups of children CBK and youth in CBK, as well as students and emplo- Design Days in NSP - COSMOS, 26.02.2018; les- yees of various Polish and foreign companies sons on the topics: Comets seen from near and far cooperating with CBK. During these visits, guests (S. Szutowicz), What can we see from outer space? had the opportunity to see our laboratories and (E.Woźniak), Tour of the Solar System (P.Witek) learn about the work carried out in the Center. Popular science lectures / reports: "Kuiper Belt Talks and lectures were prepared for pupils and Secrets" (T. Mrozek, 6/04/2018, Astronomical students. In total we have hosted 24 different Institute, University of Wrocław), "X-ray carousel groups. These included: is not spinning anymore. RHESSI (2002 - 2018)" Dedicated lectures and talks on “Space catastro- (T. Mrozek, 28/10/2018, Conference of Student phes" and "Cometes and science" (R. Gabry- Astronomical Scientific Clubs),"Comets - from szewski), the fire whirls to modern times"(R. Gabryszewski, CBK PAN for schools: 10.01.2018 – paper enti- 5/2012, Detention center in Grochów) tled; "Mars observations: from antiquity to mo- Workshops at Primary School no. 76 "How are dern times" (P. Wajer), impact craters created?" (B. Dziak-Jankowska) Entrepreneurship Day, 23.03.2018 - demonstra- Kórnik Science Days, 19-22.09.2018 - lectures: tion of the "Birth of comets" (P. Wajer); presenta- "Curiosity rover on Mars" at Primary School no. 2 tion: "Satellite Observations of the Earth. A few Kórnik / Bnin and Primary School in Kamionki words about remote sensing "(E. Woźniak); popu- (P. Lejba), "Everything you would like to know lar reading "Comets of the Solar System" (Kró- about gravity and are not afraid to ask" at the likowska-Sołtan); Primary School in Szczodrzykowo and at the Primary School in Kamionki (P. Lejba) May Film Marathon FAMA, 05.05.2018 - popular science lecture "Where are the Aliens?" (T. Mrozek) Matlab 2018, 17.04.2018 - a paper created as a response to an invitation of the conference organizer: "Application of Matlab Simulink in the space robotics" (F. Basmadji) Open-air Astrophotography, 31.08.2018 - popular science papers: "Will we fly to the stars?" (T. Mrozek), "Astrophotography for beginners" (T. Mrozek) SAT project "From a screw to the satellite" - lectures for young people in selected schools in Warsaw, Zabrze and Płock (R. Gabryszewski) Lubuskie Voivodeship Day, June 2018 - parti- cipation in a discussion panel on the future of the space sector in Poland (P. ORLEAŃSKI) School Astronomical Workshops, 15.05.2018, 04.10.2018 - popular science papers: "I will think of something, or ... When will we go to the stars?" (T. Mrozek), "A history of one proton" (T. Mro- zek); 16.05.2018 - popular science lectures: "Mass extinctions and solar movement in the Galaxy" (M. Stęślicki); 15-16.05.2018, 02-03.10.2018 - Fig. 6. School visit in Space Mechatronics and Robotics classes on the use of the amateur telescope and Laboratory. night observations of the sky (M. Stęślicki)

142 School Physics Workshops, 15.03.2018 - popular Izery" Project & Astrophotography: elements science lecture "Astrophotography for beginners" “(T. Mrozek),"Celestial sphere "(T. Mrozek), (T. Mrozek) Voivodeship competition for a paper in the field A WEEK OF SPACE EVENTS, 7.10.2018 - of astronomy and astronautics and the Voivo- popular science lecture "Wroclaw instruments fly deship Youth Astronomical-Astronaut Seminar, in space" (T. Mrozek) 07.03.2018 - an employee of CBK PAN was a chairman of the competition court (R. Schreiber) CONTACTS WITH MEDIA In addition, popular science publications: Poland In Space, 26.11.2018 - interviews for the Gabryszewski, R., Grochowalski, P., Królikow- Polish Press Agency and RMF radio (P.Witek) ska-Sołtan, M., Meritum, Kometa w szkole (Co- Interviews in the media, participation in radio and met in school), vol. 39, pp. 39-45, 2018; television programs: about planetoids close to the Królikowska M., Komeciarz, Dynamika Komet z Earth (P. Witek, 28.08.2018, radio Chilli Zet and Obłoku Oorta (Dynamics of comets from the 23.08.2018 Polish Radio 24), about a post-glacial Oort Cloud), vol.50, str.14, 2018; lake on Mars (P. Witek, 26.0./2018, Polsat News); Mrozek T., Academia, Czekanie na plamę (Wai- Platon TV program on the Rosetta mission, pre- ting for the spot), No. 2, vol. 54, pp. 9, 2018; pared by the Institute of Bioorganic Chemistry Rybus T., Forum Akademickie, Kosmiczne śmieci PAN in Poznań, October 2018 (M. Królikowska- (Space junk), vol.11, 2018; Sołtan, M. Banaszkiewicz, A. Kotarba); many Schreiber R., Urania - Advances in Astronomy, others (including P. Orleański); Analog astro- Interesting websites (permanent heading), 1 - 6, nauts. How Poles are preparing for the mission to LXXXIX, 1/56, 2/49, 3/57, 4/72, 5/25, 6/33, Mars (N. Zalewska, 07.01.2018, for the Business 2018; Insider Polska); "Świat" about travels to space (N. Zalewska N., Kubiak K., School Physics, Mars on Zalewska, 21/02/2018,); Experts: landing on Earth. Debriefing of the Polish crew from their Mars is the full success of the InSight mission (N. stay at the Martian base in Utah (USA), No. Zalewska, 27/11/2018, for the portal Nauka in 2/2018, pp. 42-49, 2018 Poland, editor Karolina Duszczyk). MEETINGS, SCIENCE PICNICS, PU- OTHERS BLIC LECTURES AND MEDIA INTER- European Rover Challenge, 09.2018; member- VIEWS ship in the referee team (M. Kalarus) All members of the SSDP department were Regional competition in physics and astronomy deeply involved in science dissemination activi- for middle and high school students – 12.03.2018, ties, including meetings with teachers and stu- Competition organized for many years with the dents, public lectures and media interviews. participation of the Marshal's Office of the Ryszard Gabryszewski organised an internatio- Kuyavian-Pomeranian Voivodeship, Toruń nal meeting at CBK PAN to summarise the out- Branch of the Polish Society of Amateur Astro- comes of the Erasmus+ SAT Project on inno- nomy (PTMA Polskie Towarzystwo Miłośników vations in teaching physics. Together with the Astronomii), Planetarium of Władysław Dzie- teacher training centre in Łódź, he prepared a wulski in Toruń, Kuyavian-Pomeranian Center meeting for teachers to disseminate the project's for Teacher Education in Toruń and I High outcomes. Ryszard also took part in the IX Space School of Nicolaus Copernicus in Toruń as part Conference in Sieradz, presenting two lectures, of the subject competitions of the Kuyavian- the first on the heritage of Ari Sternfeld's ideas on Pomeranian Board of Education; CBK PAN space exploration, and the second on best practi- employee was a chairman of the competition ces in teaching physics. He gave 10 popular lectu- commission, also participated in the preparation res on the evolution of the Solar System both at and evaluation of tasks at all stages (R. Schreiber) CBK PAN and at schools across Poland. Ryszard EXRECO working meeting (within ERASMUS is the co-author of two popular science articles: +), 19.04.2018 - popular science lecture "Astro Rewolucja kopernikańska okiem fizyka - równanie Keple-

143 ra, granica Laplace'a i rekurencyjne szeregi potęgowe and related to Mars on 6 April. Paweł is a co-author of Kometa w szkole. the article Rewolucja kopernikańska okiem fizyka - Joanna Gurgurewicz and Daniel Mège pre- równanie Keplera, granica Laplace'a i rekurencyjne szeregi sented the lecture Enigmatyczne wystąpienia metanu w potęgowe. He also prepared an innovative lesson Life atmosferze Marsa: jakie procesy geologiczne mogą za nie in the Universe, for upper secondary schools in the odpowiadać? at the seminar Kierunek: Mars context of the Erasmus+ SAT Project. organized by CBK PAN and the Polish Geophy- Piotr Witek gave four interviews to TV and radio sical Society at Pałac Staszica, in Warsaw on 6 stations on Mars research and Near Earth Astero- April. Together with Jakub Ciążela, Marta Ciążela ids (Polsat News, Polskie Radio 24, RMF FM and and Daniel Mège, Joanna was also co-author of Chilli Zet). He prepared a lesson on the Solar the lecture Enigmatyczne wystąpienia metanu w atmo- System for pupils in primary school (4–6 grades), a sferze Marsa presented at the XXI Lower Silesian lecture on Mars research for students in upper Science Festival in Warsaw on 22 September. secondary schools and a demonstration lesson on Małgorzata Królikowska-Sołtan is an author Mars research for primary school children visiting and co-author of the following popular science CBK PAN. Together with Natalia Zalewska, he articles: Dynamika Komet z Obłoku Oorta and Ko- gave an interview to the Polish Press Agency meta w szkole. She gave a popular science lecture service Nauka w Polsce on the topic of the InSight Komety Układu Słonecznego at the Entrepreneurial mission. Piotr is also an active contributor to the Day at CBK PAN on 23 March. Małgorzata also Polish Wikipedia. His main topics are astronomy took part in a TV show on the Rosetta mission for and planetary sciences; for example, he wrote the Platon TV, prepared by the Institute of Bioor- article on the InSight mission, including details of ganic Chemistry in Poznań. the involvement of the CBK PAN. Hans Rickman gave two popular lectures at Natalia Zalewska is a co-author of the article Örebro Astronomical Association and Köping Mars desert research station, czyli Mars na Ziemi - relacja Rotary Club. He was also interviewed by the polskiej załogi z pobytu w bazie marsjańskiej w Utah. Tycho Brahe Astronomical Society in Malmö, She also gave interviews; the first, Udane lądowanie Sweden. sondy InSight na Marsie - sukces polskiej myśli technicznej Sławomira Szutowicz and Piotr Witek gave was published on the website of the Institute of lectures at Warsaw schools during Project Days on Aviation, the second, written together with Piotr 26 February. Witek, Eksperci: lądowanie na Marsie to pełen sukces Paweł Wajer gave the lecture Obserwacje Marsa: od misji InSight was published by the Polish Press starożytności do czasów współczesnych on 20 January at Agency service –. Natalia gave also lectures at CBK PAN and a demonstration on The birth of schools and the Institute of Aviation on Mars comets at the Entrepreneurial Day at CBK PAN on research. 23 March. He took part in a symposium on issues

Fig. 7. Academic lectures in CBK PAN during XXII Warsaw Science Festival 2018.

144 (Astrogeodynamical Observatory of the Centrum Badań Kosmicznych PAN) The BORL team has actively participated in the In 2018, the results of the laser tracking of space popularisation of science. The most notable acti- debris carried out by the BORL station were vities in 2018 included: published in the journal Advances in Space Research: • Kórnickie Dni Nauki (KDN), 19–22 Septem- • Lejba P., Suchodolski T., Michałek P., Barto- ber, 2018, several theoretical classes were given szak J., Zapaśnik S., Schillak S., First laser mea- at the Observatory and in local schools. The surements to space debris in Poland, Advances most important event was a night laser show at in Space Research, Vol. 61, Issue 10, pp. Borowiec, which presented the capabilities of 2609–2616, DOI: https://doi.org/10.1016/ the station's satellite/space debris lasers. j.asr.2018.02.033. • Numerous lectures and visits to the Borowiec (P. Lejba) Observatory by independent schools and university students. Additional information on the selected activity (The Solar System Dynamics and Planetology (SSDP) Department) FROM SCRATCH TO A SATELLITE – the voting systems, smartphone apps, e-experi- ERASMUS+ project ments, video measurements, etc; Od śrubki do satelity – dobre praktyki w nauczaniu fizyki • three innovative physics curricula for lower (1 w gimnazjach oraz fizyki z elementami astronomii w curriculum) and upper (2 curricula, one basic szkołach ponadgimnazjalnych or, in English, as 'From and one advanced level of teaching) secondary Scratch to a Satellite' (SAT Project) was an inter- schools in Poland. The curricula included a national project within the ERASMUS+ progra- large number of ICT tools, educational pro- mme. The consortium consisted of three part- jects, methods for student assessment and pro- ners: the Centrum Badań Kosmicznych PAN gress monitoring tools; (CBK PAN), Warsaw, Poland, the Cité de l'espace • a set of best practises in teaching physics in the (Toulouse, France) and the National Space Centre form of PDFs published by French and UK (Leicester, United Kingdom). The SAT Project partners. had two main goals: a) to change the teaching Both short and long-term benefits of the SAT system in Poland by providing an innovative cur- Project were reinforced by follow-up events and riculum, with inquiry-based learning methods ba- actions. Results were disseminated during confe- sed on modern tools such as ICT, open educatio- rences, workshops and demo lessons attended by nal resources and experiments; and b) to provide a teachers. Follow-up events allowed us to directly set of best practices in teaching science to public reach nearly 500 science teachers from all over schools all over Europe. Poland. Many more were reached indirectly via The project ended in 2018 and its achievements teacher training centres and kuratoria across were as follows: Poland, where information on the SAT Project • the analysis of the current state and needs in was disseminated. Other dissemination actions Polish, French and British lower and upper se- included Facebook profiles and the Ambassador condary schools. The study described educa- Programme created by the CBK PAN. Project tional systems in the three countries and cove- outcomes were published in SCIENTIX red various issues associated with teaching magazine, which is used worldwide by teachers. physics and other science subjects: methods, General information about the SAT Project and learning conditions, laboratory equipment, etc; its results is also available in Polish, English and • thirty-seven interdisciplinary educational pro- French at http://sat.cbk.waw.pl/. jects were developed. These projects allowed The SAT Project had a significant impact on its teachers to work in the classroom using partners. It allowed them to enhance their com- inquiry-based methods and ICT techniques: petences in the field of education, due to coopera-

145 tion with teachers. We furthered research on the experiments that could be carried out even in current state of physics teaching in Polish, French poorly-equipped classrooms. All of this new and British schools, and also updated our own experience is now being implemented in schools. information on teaching practises in the educatio- Five members of the CBK PAN were involved in nal landscape. We were able to analyse convergen- the creation of educational projects: Ryszard Ga- ces and divergences among educational systems in bryszewski, Małgorzata Królikowska-Sołtan, Mi- terms of the curriculum and student experience, chał Krupiński, Edyta Woźniak and Paweł Wajer. and in terms of government approaches and tea- (R. Gabryszewski) cher training. The project allowed us to showcase many existing physics resources and approaches, POPULAR SCIENCE ARTICLES and to invite feedback from partners. It was an Gabryszewski, R., Grochowalski, P., Królikow- opportunity to explore new science activities that ska-Sołtan, M., have not yet been developed, which led to nume- Kometa w szkole rous educational projects that can be used by part- Meritum no 2 (49) / 2018, pp. 39 - 45 ners in their everyday didactic activities. We also (Mazowiecki Kwartalnik Edukacyjny) learnt how to present scientific content more effe- Królikowska-Sołtan, M., ctively, and in a more intelligible form. Dynamika Komet z Obłoku Oorta The SAT Project had also a major impact on Komeciarz no 50 (2018), pp. 7-14, teachers who participated in activities. They were (Biuletyn Naukowy Sekcji Obserwatorów Komet able to share their experience with their counter- PTMA; ISSN 1644-1303) parts, and participate in international workshops Wajer, P., Gabryszewski, R., that showcased best practices. They were able to Rewolucja kopernikańska okiem fizyka - równanie debate the most effective methods of teaching, Keplera, granica Laplace'a i rekurencyjne szeregi potęgowe visited schools, and observed physics lessons in all Fizyka w Szkole nr 1/2019 three countries. Furthermore, they learnt how to Zalewska, N., Kubiak, K., implement soft skills during physics classes, and Mars desert research station, czyli Mars na Ziemi - relacja how to use ICT tools, with special emphasis on polskiej załogi z pobytu w bazie marsjańskiej w Utah the use of smartphone apps and other simple Fizyka w Szkole nr 2/2018.

146 Fig. 6. Some press releases on CBK PAN activity in 2018.

147 CONTENTS

03 ...... ACHIEVEMENTS 05 ...... SPACE PROJECTS 25 ...... OTHER INNOVATIVE TECHNOLOGIES 32 ...... DATA ACQUISITION 40 ...... INTERPRETATION AND MODELLING 97 ...... APPLICATIONS 111 ...... PUBLICATIONS 128 ...... GRANTS AND CONTRACTS 134 ...... GENERAL INFORMATION 138 ...... EDUCATIONAL AND PROMOTIONAL ACTIVITIES

Cover: Antennas for Chinese Chang’e 4 mission. Pointing unit for MERTIS Spectrometer for ESA Bepi Colombo mission. ZENKA SAWICKA

Edited by: MAŁGORZATA MICHALSKA JOLANTA NASTULA and MARCIN GADOMSKI Technical editor: EDYTA LISIECKA

Publikację wykonano na papierze ksero 80 gr oraz w wersji elektronicznej. Okładkę wykonano na Z-Laser kolor 250 gr. Skład: Edyta Lisiecka Druk i oprawa: CBK PAN 00-716 Warszawa, ul. Bartycka 18a