CENTRUM BADAŃ KOSMICZNYCH POLSKA AKADEMIA NAUK

SPACE RESEARCH CENTRE, Polish Academy of Sciences

ANNUAL REPORT 2019

WARSAW Cover: New editions of European Land Cover maps S2GLC

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

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] CONTENTS

04 ...... THE YEAR 2019 - FOR SCIENCE AND SOCJETY

07 ...... SPACE PROJECTS ARIEL ASIM ATHENA IMAP / GLOWS JUICE LAERT OPS-SAT PROBA-3 SOLAR ORBITER TARANIS

18 ...... OTHER INNOVATIVE TECHNOLOGIES SPACE TECHNOLOGIES TECHNOLOGY DEVELOPMENT OTHER PROJECTS

36 ...... DATA ACQUISITION ASTROGEODYNAMICAL OBSERVATORY IN BOROWIEC GNSS OBSERVATORY IN WARSAW

45 ...... INTERPRETATION AND MODELLING SPACE PHYSICS PLASMA PHYSICS PHYSICAL AND GEODETIC STUDIES OF SOLAR SYSTEM BODIES AND EARTH SPACE MECHATRONICS

101 ...... APPLICATIONS EARTH OBSERVATIONS HELIOGEOPHYSICAL PREDICTION SERVICE CENTRE GNSS OBSERVATORY IN WARSAW

116 ...... PUBLICATIONS

131 ...... GRANTS AND CONTRACTS

137 ...... GENERAL INFORMATION

141 ...... EDUCATIONAL AND PROMOTIONAL ACTIVITIES The year 2019 - for science and socjety.

The year 2019 was rich in impressive scientific results, but also in innovative importance application of social and economic works.

Using the observations of neutral interstellar helium from the NASA IBEX-Lo space experiment, the density of He+ ions in the closest interstellar environment of the Sun was determined and the degree of ionization of helium, hydrogen and electron density in this medium was measured. In the model developed at CBK PAN, it was possible to reconstruct the spectra of neutral energy atoms in the full range of observed energies and to verify the mechanism of acceleration of super-thermal protons in the final shock of the solar wind on this basis.

Using data from the Magnetospheric Multiscale Mission (MMS), turbulence in solar wind plasma was analyzed on kinetic scales of tens of kilometers, much smaller than the scales characteristic of plasma description in fluid mechanics theory (MHD). In particular, it turned out that the change in the slope of the magnetic spectrum is consistent with the predictions of the kinetic theory.

2019 was the first full year when Atmosphere-Space Interactions Monitor (ASIM) instruments constructed in cooperation with the CBK PAN performed the continuous routine observations on- board International Space Station. The aim of the ASIM is to study high-altitude optical emissions from the stratosphere and mesosphere related to thunderstorms. The first results are very promising with the profit of publications in serious JCR journals.

On 18th December 2019 European Space Agency launched the OPS-SAT (3U CubeSat) – a safe, hardware/ software laboratory, flying in a LEO orbit, reconfigurable at every layer from channel coding upwards. The satellite aims to provide powerful, in-orbit tools to the emerging experimenter's community that is keen to demonstrate advanced concepts for future space applications, such as: an in- orbit testbed for onboard software applications; advanced communication protocols; compression techniques; demonstrations of advanced software-defined radio concepts for communication purposes; and others. CBK PAN cooperates in developing the hardware for the CCSDS Engine.

CBK PAN is actively involved in international cooperation, in many ESA programs and as a desirable and reliable partner has its share in the integration of European science and technology.

In close cooperation with scientists and technicians in many international and European research organizations and programs, works are created that help to understand the evolution of the surface and atmosphere of Mars and reflect the uniqueness of the Martian ecosystem. The CBK PAN conducted analyzes of color and stereoscopic images of Mars from three instruments of the ExoMars Trace Gas mission. The aim of the research is to discover gases in the Martian atmosphere that can be produced in the Mars crust, and to identify sources of subsurface water bodies in which biological activity can exist today.

The ESA Sentinel-2 Global Land Cover (S2GLC) project was completed. In this project a method of automatic and quick creation of detailed maps of land cover was developed. A map of land classification for Europe was made. Copernicus databases were used to make 15,000 classifications. This European land cover classification was presented as showcase of EC and ESA at the GEO summit in Canberra. It was the first such a high distinction for a Polish institution at this summit.

4 On November 7, CBK PAN launched a special experimental website (24/7) for the International Civil Aviation Organization (ICAO); service dedicated to radiocommunications, navigation along with information on radiation doses, as services for civil aviation in the world, for crews and ground services. ICAO has chosen three global consortia of space weather services. Over the next three years, they are to introduce a professional space weather service for aviation, providing operational support and increasing flight safety and ground infrastructure. CBK PAN is a member of the PECASUS consortium (including the British MET OFFICE, the Belgian Solar-Terrestrial Center of Excellence and the Finnish Meteorological Institute).

In Poland, CBK PAN has established the first in Europe DRIVER+ Competence Center, whose task will be to reduce the risk of implementing new solutions in crisis management. The center will realistically test technical and organizational innovations before they will be bringing to operational service.

The CBK PAN analyzes changes in groundwater and total water resources important for the Polish rivers the Vistula and Oder. For the first time, observations from the GRACE gravimetric mission were compared with well groundwater observations, results from GLDAS hydrological models as well as CMIP5 climate models.

The ongoing CBK PAN BAMS-Mazovia project is to provide data on changes taking place in built-up areas based on automated classifications of Sentinel-2 satellite imagery. Through its operation, the built platform enables faster database updates and allows reducing the costs of maintaining and managing data.

We are developing our staff by gaining further degrees and academic titles, as well as enrich the infrastructure necessary for the further development of our technological capabilities.

In 2019, with the support of the President of the Polish Academy of Sciences and the Marshal of the Lubuskie Voivodeship, CBK PAN opened a branch in Zielona Góra – the Laboratory of Dynamics of Satellite Manipulators. This is the only PAN facility in this province. Together with the University of Zielona Góra and local companies, the Laboratory will create a new, strong scientific and technical center operating in the field of space exploration.

Active in so many various areas of space science, space engineering, space policy, education and outreach activities, CBK PAN proves its truly comprehensive approach to the research and space exploration. State-of-the-art science and technology and its innovative applications makes us reliable

(I. Stanisławska) Director CBK PAN

5 We announce with deep regret that our colleagues and friends, long-time employees of the Centrum Badań Kosmicznych PAN, passed away in 2019:

Jacek Krasowski in January 2019, Zbigniew Zbyszyński in October 2019, Zbigniew Błoński in November 2019.

We will miss them deeply.

CBK PAN's Management and staff

6 SPACE PROJECTS ARIEL (Atmospheric Remote-sensing Infrared Exoplanet Large-survey) ARIEL, the Atmospheric Remote-sensing Infrared Exo- tion. The system also takes parallel photometric planet Large-survey, was selected as the fourth medium- measurements of selected objects. The CBK PAN class mission in ESA's Cosmic Vision programme. It will team is responsible for the following items, and study what exoplanets are made of, how they formed and for providing any equipment needed to adjust and how they evolve, by surveying a diverse sample of about commission the device: 1000 extrasolar planets, simultaneously in visible and • the opto-mechanical part of the FGS; infrared wavelengths. It is the first mission dedicated to • its warm front end electronics; measuring the chemical composition and thermal structures • its control electronics; of hundreds of transiting exoplanets, enabling planetary • mechanical structures for the above items; and science far beyond the boundaries of the Solar System. • mechanical, engineering and optical ground This project concerns measurements of the spe- support equipment for the above items. ctral characteristics of the atmosphere of planets Engineering, Qualification, Flight and Spare orbiting stars of type F, G, K and M. These planets models of the FGS will be developed. Laboratory have temperatures in the range of 250–1,000 K, performance models are at an early stage of deve- and masses that range from a few to 100 Earth lopment. The FGS operates at a temperature of masses. The Polish team is involved in technical 50–55 K with detectors and so-called 'cold' front and scientific aspects. On the technical side, we end electronics; the other electronic devices will are responsible for the so-called Fine Guidance operate at a temperature of 250–300 K. System (FGS). On the research side, we are simu- In 2019, CBK PAN researchers focused on the lating the measurements and interpretation of the development of Bread Board models and FEM data that is collected. structural and thermal analyses. The design of an The FGS measures the spectral characteristics of opto-mechanical head that can work in cryogenic distant planets at high resolution, with high-pre- temperatures has been developed. A method and cision positioning. The optical axis jitter is desi- procedures for gluing optical elements to their gned to be of the order of a single milli-arc se- holder in cryogenic temperatures has also been cond. This instrument determines the highest developed. Relevant documentation and reports possible measurement precision, and can hold the were delivered to the ARIEL Consortium. position for a few minutes while measurements (M. Rataj) are taken. It continuously sends data to a satellite system to ensure the correct measurement direc- ASIM ASIM / MXGS on ISS The aim of the Atmosphere-Space Interactions Monitor (ASIM) flown onboard the International Space Station (ISS) is to study high-altitude optical emissions from the stratosphere and mesosphere related to thunderstorms. One of the two, main ASIM instruments is the Miniature-X and Gamma-ray Sensor (MXGS) de- signed by the University of Bergen and the Uni- versity of Valencia, in cooperation with the CBK Fig. 1. The terrestrial gamma-ray flash and ionospheric ultraviolet emissions powered by lightning and observed PAN. The Centre is responsible for the design and by ASIM on the ISS. This is the scenario reported by manufacture of the Power Supply Unit and its au- Norbert et al. in Science, Vol. 367. tonomous (FPGA-based) Housekeeping System. onboard the ISS. The results have been published In 2019, ASIM performed routine observations in papers in several journals, notably Science. (P. Orleański)

7 ATHENA counting. The instrument is designed to make op- timal use of the grasp (the product of the colle- The ATHENA (Advanced Telescope for High Energy cting area and solid angle) that is provided by the Astrophysics) is a European Space Agency (ESA) mis- optical design of the ATHENA mirror system. sion, contributing to the ESA's Cosmic Vision Theme, The WFI is a very powerful survey instrument, “Hot and Energetic Universe”. significantly surpassing current capabilities. In The Wide Field Imager (WFI) is one of two scien- addition, it will provide unprecedented, simul- tific instruments proposed for the ATHENA X- taneous, high time resolution and high count rate ray observatory. The lead institution for this pro- capabilities for the observation of bright sources, ject is the Max Planck Institute for Extraterrestrial with low pile-up and high efficiency. Physics (Germany). The WFI will provide ima- The CBK PAN is involved in the development of ging in the 0.1–15 keV band over a wide field, with two subunits: the Filter Wheel Assembly (FWA) simultaneous spectral and time resolved photon and the Power Distribution Unit (PDU).

ATHENA/WFI/FWA In 2019, activities related to development of the which was used to conduct an acoustic test cam- FWA were at the top of the agenda for the entire paign at AGH University of Science and Techno- WFI consortium, because they were most proble- logy in Kraków. Thanks to the joint efforts of the matic from the engineering point of view. The entire team, all tests were successful and the re- FWA includes a filter that is only 200 nm thick, but sults are currently being analysed. The conclu- has to survive the mechanical and acoustic loads sions will serve as input for further design and of the launch rocket. In 2019, the CBK PAN's optimisation – an activity that will be continued in engineers built a simplified versionof the FWA, 2020.

Fig. 2. The WFI FWA Acoustic Development Model. Fig. 3. The WFI FWA during acoustic testing. (T. Barciński, Sz. Polak, J. Musiał, A. Sikorski)

The Comet Interceptor The Comet Interceptor is a new F1(fast) mission to a Dynamically New Solar System Object selected by the European Space Agency in July 2019. The mis- sion will be launched in 2028 on the same rocket as the M4 mission ARIEL. The main goal of this mission is to explore a comet very likely entering the inner Solar System for the first time or, possibly, to en-

8 counter an interstellar object originating at ano- ved in the construction of one the primary instru- ther star. Based on both the catalogue of historic ments: the DFP (Dust Field, Plasma) for the main LPCs and simulations of a large, synthetic set of space-craft and one smaller, daughter satellite LPC orbits, the Comet Interceptor will have to provides five sensors and central electronics that wait only 2–3 years for a target it can reach. The will provide multi-point, in situ measurements of satellites will be launched to a stable, halo orbit the dust, electric and magnetic field, and charged around the Sun–Earth L2 point and wait there and neutral particles in the cometary environ- until the discovery of a suitable comet that it can ment. The CBK PAN is responsible for manage- reach. ment, and Prof. H. Rothkaehl is PI for the DFP The Comet Interceptor mission will involve three, instrument. CBK PAN responsibilities with res- separate spacecraft working together to obtain pect to instrument implementation are PSU sup- multi-point measurements and get the 3D infor- ply redundancy system and instrument E-box mation provided on the target and its jets/ coma. construction. Its scientific involvement also inclu- Similarly, in situ observations of the cometary des data analysis and science interpretation of environment can be also obtain from multiple registered data, and preparing the details of sampling paths. The multiple elements can sample scientific program for mission. In 2019, the gas composition and density, dust flux, and pla- overall design for each of the subunits of the DFP sma and solar wind interactions, to build up a 3D instru-ment was prepared, and the appropriate 'snapshot' of the region around the target. One docu-ments were completed, the Instrument spacecraft will make remote and upstream in situ Design Report IDR, the Instrument Management observations of the target from afar, to protect it Plan IMP, the Instrument Development Plan IDP, from the dust environment of an active comet, and the Instrument Interface Development Plan and act as the primary communications hub with IIDD. The first phase of the project has ended Earth for all other mission elements. Two other successfully. spacecraft will be deployed to venture closer to (H. Rothkaehl PI for the DFP instrument the target, carrying complementary instrument J. Baran Project Manager for the DFP Instrument payloads, to build up a 3D picture of the comet. M. Morawski Lead electronic engineer, T. Barciński The CBK PAN Space Plasma department is invol- LEAD mechanical engineer) IMAP/GLOWS The CBK PAN is participating in the helioglow, collected from a Sun-centred circle NASA space mission, the Interstellar with a radius of 75°. Mapping and Acceleration Probe (IM- In 2019, the IMAP mission completed Phase A. AP), which is scheduled for launch in The IMAP project (including GLOWS) success- 2024, operating near the liberation fully passed the IRR in December 2019, and its point L1, about 1.5 million km sun- successful evaluation by NASA was officially an- ward from the Earth. The objective of nounced on 28 January, 2020. This formally clo- the IMAP mission is to investigate the interaction of the sed Phase A and initiated Phase B of the mission. solar wind with the Sun's galactic environment and cosmic Another outcome of the IRR was that the general ray acceleration processes. GLOWS architecture, proposed by the CBK The CBK PAN has provided a Lyman-α PAN, has been accepted by NASA. photometer called GLOWS (GLObal solar Wind In 2019, we developed the IMAP/ GLOWS docu- Structure), one of the ten science instruments on mentation required to close Phase A. In parallel, IMAP. The GLOWS experiment will use remote- our technical and scientific activities focused on sensing photometric observations of the helio- the most critical elements of the instrument. spheric backscatter glow to investigate variation in The geometry of planned observations, i.e., the solar wind flux with heliolatitude, and its evolu- diameter of the instrument field of view and the tion during the cycle of solar activity. These radius of the scanning circle in the sky were cho- obser-vations will provide daily lightcurves of the sen based on an extensive analysis of the expected

9 helioglow intensity and the distribution of background extraheliospheric radiation sou- rces. On this basis, performance require- ments for the instrument's entry system (the light baffle, the collimator and the filter) we- re formulated. The instrument's UV channeltron model and UV filter were selected based on a care- ful scientific analysis of the expected signal. To that end, a model of the expected helio- glow intensity and its evolution during the Fig. 4. The one-channel UV photometer that has been accepted as cycle of solar activity was developed, and a the baseline for the GLOWS instrument. database of the spectra of extraheliosphe- ric EUV sources was compiled based on exi- sting astronomical observations. Signal: observer at Crosswind

Fig. 5. Simulation of the expected signal for two days: the epoch of low solar activity (left column) and high activity (right column). Simulation of the expected signal for two days: A tentative model of the instrument collimator the epoch of low solar activity (left column) and function was developed and combinations of the high activity (right column) is shown in Fig. 5. The expected signal composed of the heliospheric and upper row of panels presents simulated count extraheliospheric components was simulated for rates expected from the GLOWS instrument each day of the year, for several alternative spec- (black lines). The signal is composed of the com- tral characteristics of the filter. These studies were ponent due to the heliospheric backscatter glow used to select the manufacturers and models of (blue lines), which is the subject of the planned the channeltron detector and the narrow-band science analysis, and a background signal due to EUV filter. extraheliospheric radiation sources. The sky di- In 2019, a test UV radiation source (lamp) and the stribution of these sources is presented in the lo- selected channeltron detector were procured, wer row of panels (coloured dots), with the loca- initial drafts of the baffle and collimator design tion of the sky strip observed by GLOWS marked were developed and their performance was by the black circle. The position of the Sun against simulated using the ZEMAX ray-tracing package. the sky is marked by the black dot in the centre of The first hardware model of the collimator was the scanning circle; the intensity scale of point produced and tested. Requirements for data pro- sources is given by the coloured bars.

10 ducts were formulated and, based on simulations using EUV-bright stars as standard candles. of the signal, a study of the expected data rate was Specifically, we developed prototype methods to performed. These insights, based on the planned extract the star signal free from the contribution mission telemetry rate, led to the design of a first- from the heliospheric glow, which made it cut approach to the onboard data compression possible to compile a tentative list of can-didate scheme. calibration stars. The IMAP mission is carried out by an interna- tional science team led by Principal Investigator Dr David J. McComas from Princeton University. The IMAP project is managed by the Applied Physics Laboratory of Johns Hopkins University. Co-Investigators on the IMAP Science Team include Maciej Bzowski, Justyna M. Sokół, and Marzena A. Kubiak from the CBK LSSPA. The GLOWS science team includes Maciej Bzowski (lead), Marzena Kubiak, Marek Strumik, and Izabela Kowalska-Leszczyńska from LSSPA. The GLOWS engineering team, led by Piotr Orleański Fig. 6. The first model of the GLOWS Collimator (GLOWS Project Manager) and Roman Waw- module. The final design should integrate five or six of rzaszek (GLOWS Systems Engineer) includes the identical, vertically-stacked modules shown above. Mirosław Rataj, Przemysław Kaźmierczak, To- Since the sensitivity of the instrument is expected masz Kowalski, Jędrzej Baran, Marek Winkler and to change during planned observations, we deve- Waldek Bujwan. loped a tentative instrument calibration scheme, (M. Bzowski, P. Orleański, R. Wawrzaszek) JUICE – the Jupiter Icy Moons Explorer JUICE is an L-class mission of the European Space Agency (ESA) under its Cosmic Vision 2015–2025 programme. It is expected to launch in 2022. JUICE, with its combined remote sensing and in-situ payload, will critically advance our knowledge. The spacecraft is speci- fically designed to characterize 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, Europa and Calisto. The mission will determine the characteristics of liquid- water oceans below the icy surfaces of the moons. It will also focus on characterizing the diversity of processes in the Jupiter system, which may be required in order to provide a stable environment at Ganymede, Europa and Calisto on geologic time scales, including gravitational coupling bet- ween the Galilean satellites and their long-term tidal influ- ence on the system as a whole. Additionally, studies of Jupiter's atmosphere (its structure, dynamics and composition), and ma- gnetosphere (three-dimensional properties of the magneto-disc and coupling processes) and their interaction with the Galilean satellites will enhan- ce our understanding of the evolution and dyna- mics of the Jovian system. Fig. 7. The JUICE satellite.

11 Sub-millimeter Wave Instrument (SWI) SWI is one of the scientific instruments on board We are participating in the following work- JUICE. Its science goals are to: 1) study the Jovian packages: system with particular emphases on the chemistry, 1. Data Processing Unit (DPU), including Boot meteorology and structure of Jupiter's middle SW software; atmosphere, and atmospheric coupling processes; 2. Power Supply Unit (PSU); 2) characterize the regolith, icy crust, atmosphere 3. Radiator; and exosphere of Ganymede, Europa and Calli- 4. Structural and Thermal Modelling of the sto, thereby providing important inputs for the DPU, PSU and Radiator subunits. exploration of their habitable zones; 3) study Work on the DPU and PSU is being carried out at Ganymede as a planetary object and possible ha- the Laboratory of Space Applications of FPGA bitat; study and explore Europa's young icy crust Circuits at the CBK PAN. Most of our time has in recently-active zones; and 4) explore the Jovian been dedicated to manufacturing and testing the system as an archetype for gas giants in characte- DPU EM2 and PSU EM2 models, and updating rizing the Jovian atmosphere, and its satellite and the design of FM models. The two EM2s have ring systems. been manufactured, and successfully tested and The SWI is a passive, heterodyne microwave delivered to the Principal Investigator for further spectrometer that is sensitive to radiation in the integration with other SWI subsystems. A model frequency bands 530–625 and 1080–1275 GHz. of an auxiliary DPU (the so-called AX) has been Radiation is received through a quasi-optical off- manufactured. This model was used to functio- axis telescope with 30 cm aperture diameter, nally test the Boot SW and FPGA before the providing a spatial resolution of 2 mrad (FWHM) PROM and flight FPGA are programmed/ bur- at 600 GHz. The telescope is equipped with a two- ned. axis scan mechanism that allows scanning around In parallel, work was carried out on DPU and PSU the nadir viewing direction in a range of ±76° STM models, with the aim of performing vibra- within the spacecraft's orbital plane and ±4.3° tion tests at the beginning of 2021. Work related perpendicular to the plane. to the development of the Radiator unit was Two, independent double-sideband receivers are conducted by the Micromechanical and Photo- used to obtain simultaneous observing capability nics Laboratory of the CBK PAN. The SWI requi- for two different frequencies within the 530–625 res the Radiator unit to be able to cool heterodyne range of the baseline frequency band. Each mixers to the range of ~130K, in order to mini- receiver is connected to its own high-resolution mise noise. In 2019, we concentrated on manufac- chirp transform spectrometer (CTS), providing a turing EM2 and STM models. Both were success- total bandwidth of 1 GHz at 100 kHz resolution fully tested and, consequently, work began on (10000 equidistant channels). manufacturing FM and FS models.

Fig. 8. The DPU Em2. Fig. 9. The PSU Em2.

12 Fig. 10. DPU & PSU Em2s. Fig. 11. The DPU Em2.

Fig. 12. The Radiator STM. Fig. 13. DPU & PSU STM Trays. (K. Skup) The Radio & Plasma Waves Investigation (RPWI) The Radio & Plasma Waves Investigation (RPWI) is the second JUICE's scientific payload instruments developed in CBK PAN. It consists of a highly-integrated package of instruments designed to carry out comprehensive science investigations of the space environments around Jupiter (primarily near Ganymede, Europa and Callisto), as well as monitoring radio wave emissions in the Jupiter system. The RPWI sensors can provide complete measurements of electric and magnetic field vectors. The RPWI makes use of several different sensors and receivers. Altogether, the instrument uses 10 sensors and 3 receivers, which cover a wide frequency range, from DC up to 45 MHz. There are 4 Langmuir probes (LP-PWI) for plasma and electric field measurements, a search coil magnetometer (SCM) with 3 coils for magnetic fields measurement, and 3 radio antennas (RWI).

13 Fig. 14. Digital Processing Unit DPU for the RPWI's of Fig. 15. E-Box FM flight model for the RPWI. STM structural thermal model. The CBK PAN plays a major role in the JUICE/ RPWI consortium, both with regard to hardware and software, and the scientific investigation. In particular, the Centre is responsible for: • the design of the main RPWI Digital Processing Unit (DPU) (Figure 14); • the design of the E-Box and preamplifier box for the LP-PWI. In 2019, the design phase was completed and the final design of flight models for the digital pro- cessing unit DPU, E-Box and Pre-box were ap- proved. Therefore, we started the implementation phase, and the first flight models were put into Fig. 16. Preamplifier box STM structural thermal model for production. The E-box, which is the first flight the LP-PWI. element for the RWPI, has been completed. (H. Rothkaehl Co-PI RPWI consortium, M. Morawski (DPU Lead), G. Juchnikowski, T. Barciński and J. Baran, (Mechanics Lead), T. Kowalski, P. Szewczyk)

LAERT ionosondes for the JONOSOND mission Within the framework of a contract with a Russian company, LAERT ionosondes for the top-side ionosphere were designed by the CBK PAN (Figure 17). New, advanced so- unding techniques were developed for the spa- ceborne exploration of the Earth's magneto- sphere and topside ionosphere. The mission's four, identical spacecraft will be located in a polar orbit at altitudes of 600 and 800 km. Each instrument consists of two parts: receiver and transmitter boxes, and an antenna preamplifier.

Fig. 17. Two sets of FM fight model LAERT ionosondes.

14 This active investigation of the near-Earth envi- transparency band for the considered waves. ronment is a unique opportunity to diagnose its Special LAERT regimes will be designed to regi- complex space plasma. The project is a milestone ster both first and second wave harmonics using for future spaceborne services, which will focus both a trans-ionospheric sounding regime and the on diagnoses of ionospheric perturbations satellite itself in sounding and radio-spectrometer caused by seismic activity. Nonlinear resonance modes. of extraordinary waves has already been In 2019, work on developing hardware for the examined. This found that plasma conditions are next two flight modes was finalised and testing unconnected with resonance plasma properties, process has been started. but are determined by the magnitude of the (H. Rothkaehl, A. Rokicki, magnetic field and electron concetrations in the M. Morawski, M. Winkler) OPS-SAT OPS-SAT (3U CubeSat) is a safe, hardware/software laboratory, flying in a low Earth Orbit, reconfigurable at every layer from channel coding upwards. This European Space Agency mission aims to provide powerful, in-orbit tools to an emerging experimenter community that is keen to demonstrate advanced concepts for future space appli- cations, such as: an in-orbit testbed for onboard software applications; advanced communication protocols; compres- sion techniques; and demonstrations of advanced software- defined radio concepts for communication purposes, among others. The CBK PAN was responsible for developing Fig. 18. The OP-SAT Flight Model, courtesy of the the hardware for the CCSDS Engine (the satel- European Space Agency. lite's protocol conver-ter). Its firmware was provi- In 2019, all of the hardware was integrated, and ded by a subcontractor (Creotech Instruments OPS-SAT was successfully launched (on 18 S.A.). December 2019) by Soyuz from Kourou. (P. Orleański) The PROBA-3 CORONAGRAPH Filter Wheel Assembly PROBA-3 is the third PROBA (Project for Onboard craft will fly in formation, which requires milli- Autonomy) mission. This experimental mission is devoted metre-accurate relative positioning, and consis- to the in-orbit demonstration of formation flying techniques tently precise relative navigation. The spacecraft and technologies. The mission's high-level objectives are: can manoeuvre independently of one another, development to technology readiness level 9, and in-orbit and they will typically be separated by about demonstration of formation flying techniques and asso- 150 m. ciated technologies; development and validation of the engi- The Coronagraph Instrument includes a Filter neering approach, ground verification tools and formation Wheel Assembly (FWA) subsystem. This opto- flying facilities; and observation of the solar corona as part mechanical system is situated in front of the focal of the demonstration of formation flying, based on a plane assembly. Its main task is to sequentially po- coronagraph. sition the different filter/ polarisers in the optical The mission will be carried out by a pair of small beam of the Coronagraph Instrument. spacecraft, which together form a coronagraph. In 2019, the CBK PAN designed and manufac- The two-year mission (including commissioning) tured a complete FWA Qualification Model that is based on a highly elliptical orbit. The two space- performed successfully in the qualification cam-

15 paign at unit level, and was delivered to the Centre Spatial de Liège (CSL) for instrument-level tes- ting. The Flight Model is planned to be delivered to the CSL by mid-2020.

Fig. 19. The FWA Qualification Model during TVAC testing.

(J. Baran, J. Musiał, T. Kowalski, K. Aleksiejuk) STIX (X-ray Spectrometer/Telescope Instrument) for Solar Orbiter Mission) Solar Orbiter is a mission dedicated to solar and helio- spheric physics. It was selected as the first medium-class mis- sion of ESA's Cosmic Vision 2015-2025 Programme. The programme outlines key scientific questions which need to be answered about the development of planets and the emergence of life, how the Solar System works, the origins of the Universe, and the fundamental physics at work in the Universe. X-ray Spectrometer/Telescope Instrument (STI- X), one of 6 remote sensing instruments on- board SolO, provides imaging spectroscopy of IDPU and PSU (Power Supply Unit to be solar thermal and non-thermal X-ray emission. delivered by Czech Republic) (K. Skup) STIX will provide quantitative information on the 3. Thermal Modeling of the instrument and its timing, location, intensity, and spectra of accele- subsystems (K. Seweryn) rated electrons as well as of high temperature 4. Instrument EGSE (M. Kowaliński) thermal plasmas, mostly associated with flares The 2019 activities in STIX on science and EGSE and/or microflares. PI of the Instrument: Dr. are described in the chapter dedicated to Solar Sam Krucker, FHNW, Windisch, Switzerland. Physics Group in Wrocław. Collaborating countries (HW and SW): CH, PL, STIX IDPU was delivered in 2018 to the PI in D, CZ, F. Switzerland. In 2019 it was integrated with the The Polish participation in STIX consists of the STIX instrument and the whole spacecraft. Then following work-packages: the Solar Orbiter was subjected to undergo a 1. Participation in STIX scientific program and series of tests at the premises of IABG facility in Data Reduction and Archiving (J. Sylwe- in Ottobrunn, Germany. ster) 2. Instrument Data Processing Unit (IDPU) Solar Orbiter is scheduled for launch in including IDPU hardware, low level flight February 2020. software and mechanical frame for both: (K. Skup) TARANIS/MEXIC Power Units The MEXIC Power Units (MPU1 and MPU2) are two management of electrical power for the entire scientific blocks of electronics designed and developed by CBK PAN payload onboard the French TARANIS satellite, develo- that are responsible for the conversion, distribution and ped by CNES (Centre National d'Études Spatiales).

16 TARANIS is a low Earth orbit microsatellite mission that will provide a set of unprecedented and complementary measurements on the physics of TLEs (Transient Lumin- ous Events) and TGFs (Terrestrial Gamma ray Flashes). In 2019, MPU modules, integrated with the entire TARANIS satellite were intensively tested by CNES. Currently, the launch of the satellite is scheduled for June 2020.

Fig. 20. The TARANIS satellite (Credits: Prodigma Films, “CNES - Taranis - AIT Préparation”).

(R. Wawrzaszek)

17 OTHER INNOVATIVE TECHNOLOGIES SPACE TECHNOLOGIES An Attitude and Orbital Control System for the HyperCube platform The purpose of the AOCS (Attitude and Orbital Control System) project is to design and develop a positioning and orientation control system for the new, modular and scalable satellite platform that is being developed by the company Creotech Instruments SA. The project is the result of a contract with Creotech Instruments, which obtained finan- cial support from the Polish National Centre for Research and Development (Narodowe Centrum Badań i Rozwo- ju). In 2019, the system's design concepts were evalu- ated, and hardware components were designed and purchased. In December 2019, the Prelimi- nary Design Review was held, and this phase has Fig. 1. Mock-up of the Astro-Sat, the satellite forming the base for the HyperCube platform (Credits: Creotech ended successfully. Instruments SA). The most significant progress has been achieved nents selected for implementation has been in the field of hardware development. All mecha- studied and emulator and structural-thermal nical parts and components have been manufac- models have been designed and manufactured tured and prepared for further development of (Fig. 2, Fig. 3). the complete AOCS system. Each of the compo-

Fig. 2. Hardware purchased and used in the framework of the project's gyroscope and the models that have been designed and manufactured for testing purposes.

Fig. 3. Startracker models designed and manufactured for testing purposes.

18 The heart of the system will be the SAB module; this is where the overall control algorithms will run. In 2019, we finalised the design of the SAB model (Figure 4) and it is expected to be manu- factured in February 2020. A so-called flat-sat frame has been designed and manufactured for testing purposes. A dedicated Simulation and Testing Platform has also been designed for functional verification of the whole system. This system will make it possible to run control algorithms on the target AOCS controller Fig. 4. The AOCS controller. The module's format is and verify all of its functionalities using a com- compatible with the SVPX standard. bination of hardware and software tools. The overall project is expected to be finalised in June 2020.

A GNSS RECEIVER FOR MICRO-LAUNCHERS AND MICRO-SATELLITES The main aim of this project is to develop advanced ting the experimental micro-launcher, MIURA-1. software for a Global Navigation Satellite System In 2019, CBK PAN activities were focused on har- (GNSS) receiver, based on registering and processing dware development. As a result, several versions GNSS signals (the so-called SDR technique). The project of the On-Board Computer (OBC) were deve- is funded by the European Space Agency within the loped. One option that was ex-plored was based framework of the NAVISP (NAVigation Innovation on the SAMV71 microcon-troller, however, deve- Support) Programme, and the consortium is made up of lopment was frozen due to unsatisfactory perfor- GMV Innovating Solutions Sp. Z.o.o. (leader), Hertz mance. The second version of the OBC uses the Systems and the Centrum Badań Kosmicznych PAN. Zynq7030 System-on-Chip, and this version has CBK PAN is responsible for the design and deve- been approved for use in the framework of lopment of hardware, and preparations for tes- further development of the project.

Fig. 5. Left: the OBC module based on the SAMV71 microcontroller. Right: stacked GNSS receiver electronics, consisting of a Zynq7030-based OBC on the bottom and RF front-end on the top. A prototype of the radio frequency (RF) front-end of the receiver has also been manufactured and tested. The overall design of the module that will be used in the framework of onboard tests of the sounding rocket has also been finalised, and mechanical components have been manufactured.

19 Fig. 6. The experimental GNSS receiver module, showing the design of the mechanics and arrangement of internal components.

Improving the mobility of a nonholonomic space robot The main goal of our project is to define a new class of planning and control algorithms dedicated to nonholonomic systems with drift in the presence of surrounding obstacles. The project is funded by the National Science Center, and executed by the Centrum Badań Kosmicznych PAN and Wrocław University of Technology. In the framework of this project, the testing facility at the CBK PAN was upgraded. First, the robotic arm of the space robot was equipped with a third kinematic pair. Secondly, new PCB boards for the main computer, joint controllers and a cold-gas thruster controller were developed. Mo- Fig. 7. The space robot at the CBK PAN. reover, the space robot was equipped with two, stereovision cameras to detect obstacles in its surroundings. The updated platform is presented in Figure 7, and the updated electronic archite- cture is presented in Figure 8. All of the functions of the space robot are con- trolled by three microprocessors called, respec- tively the space robot computer, the joint con- troller and the cold-gas controller. The space robot computer is based on a microchip, low po- wer ARM Cortex-A5 processor running embed- ded Linux. It also features a floating-point unit, CAN-BUS, Ethernet and WIFI interfaces. Com- munication with joint and cold-gas controllers uses the CAN-BUS protocol. The USART inter- face is used to receive data about satellite angular velocity and linear acceleration from the onboard inertial measurement unit. The RS232 interface is

Fig. 8. The electronic architecture of the testing facility.

20 used to communicate with the onboard vision tree method; robotic arm path planning using an computer that computes information received artificial potential field method; and robotic arm from onboard stereo cameras. path planning using an endogenous configuration Time synchronization between the space robot space approach. Typical results are presented in computer and the controllers is governed by a Figure 9 for a scenario that is related to satellite Linux OS. The joint controller and cold-gas trajectory planning in the presence of obstacles in controller, like the space robot computer, are the robot's surroundings. First, a collision-free based on an ARM architecture; however, as an trajectory was generated, then sent to the space operating system was not needed, a Cortex-M4 robot's onboard computer to be executed. As Fi- core was selected. gure 9 (a) shows, the trajectory was correctly exe- In 2019, various algorithms were tested in a 2D cuted. The satellite maintained its orientation with microgravity test-bed, these included: robotic arm an accuracy of about 1 degree, as shown in Figure path planning using a rapid-exploration random 9 (b). X- and y-axis errors presented in (c) and (d) show, respectively, that they do not exceed 1 cm.

Fig. 9. Exemplary results space robot trajectory planning and control system.

(J. Sąsiadek, F. Basmadji, K. Seweryn)

TECHNOLOGY DEVELOPMENT A lightweight, compact optical system based on DOE and aspherical elements The main objective of this project is to design, manufacture and mounting precision lenses that meet the and test a compact optical system based on state-of-the-art highest global standards will be mobilised. The design, manufacturing and assembly technologies, notably project is the result of a contract with the DOE and aspherical surfaces. The proposed design is European Space Agency. The proposed design is characterised by parameters that perform better than any of shown in Figure 10. the systems currently available on the market, or described In 2019, the first laboratory model was produced in the scientific/ technical literature. and tested. A progress report was delivered to the Polish technological expertise in manufacturing European Space Agency.

21 Fig. 10. DOE proposed design.

(M. Rataj)

Landing on low-gravity bodies – tests of landing gear (REST project) The goal of the REST project is to design, develop and test a scaled proto- type of an actively compliant landing gear for the Phobos sample return mi- ssion. The CBK PAN is responsible for: (i) the landing gear control system; (ii) upgrade of the air-bearing test fa- cility for simulations of landing ope- rations; and (iii) execution of the test campaign. In 2019, the CBK PAN success- fully finalised the test campaign, Fig. 11. The air-bearing test set-up showing the lander mock-up on the air- which ended its involvement in bearing cart approaching the mock-up of the Phobos surface. the project. (T. Barciński, J. Musiał, A. Sikorski, J. Baran, K. Aleksiejuk)

R&D in the ZFS Optical Laboratory three groups of problems: grid quality, grid Testing grid collimator systems alignment and collimator reciprocal alignment. In order to improve grid quality we need to choose Grid collimator systems are the basic tools used to the best grids, and measure deviations from study hard x-ray source displacement, especially expected parameters. To improve grid alignment in solar observation instruments. In recent years, we must be able to improve its precision and two-grid systems have become more popular than understand any deviations from expected multigrid systems. The basic problem in the measurements. Similar issues apply to alignment mathematic analysis of observations is a discre- collimator systems; in all cases deviations must be pancy between real, and perfect grid collimator taken into account in the mathematic analysis of systems. These discrepancies can be divided into observations.

22 Grid quality measurements Measurements were taken for one-dimensional Figure 12 shows an example of a photograph ta- grids (see the example in Figure 11), and two- ken with a digital camera. These photographs we- dimensional grids with square slots. A particular re analysed by a dedicated computer program, measurement problem is distortion in the came- which identified the position and width of the ra's optical system. Because of this, we only tested grid's 'slots' (Figure 13). undistorted systems: a pinhole camera and a pro- jection system. Pinhole cameras have poor resolu- tion, which reduces their usefulness. Projection systems have a resolution that is somewhere bet- ween a pinhole camera and a regular camera. One way to improve resolution is by using X-rays. In all cases, there are limitations on the maximum num- ber of grid slots that can be measured. We there- fore attempted to use a Moiré pattern for grids with a very high number of slots. With this techni- que, bright and dark strips can be seen if two, similar grids are placed in the vicinity of each other (Fig. 14). Fig. 12. A photo of a collimator grid.

Fig. 14. Moiré pattern for two grids with square slots. By changing the system geometry, it is possible to produce different numbers of strips. If the relative positions of the two grids' slots are Fig. 13. Slot positions for the grid shown in Figure 12. not identical, then the Moiré strip is deformed. We Dark areas indicate a left shift (minimum value is - 2.7 pix=- 8.4 µm), while bright areas indicate a right shift are developing a way to use Moiré patterns to (maximum value is 2.4 pix=7.4 µm). obtain slot positions for individual grids.

Measurements of alignment precision A method to align multigrid collimator systems was developed long ago, and is used in optical spectral power distribution. In this technique, a lightened triangle coincides with diffraction strips found in collimator grid systems (Fig. 15). In 2019, our work focused on an extension to the method, which makes it possible to align grids with square slots. The approach was taken because recently, two-grid systems have become more popular than multigrid systems (Fig. 16). Fig. 15. Lightened triangle and diffraction strips using a four-grid collimator.

23 Using a digital camera, we have developed a new alignment technique. First, we take pictures of ali- gnments in the traditional manner. Then, we ap- ply a computer program that can calculate devia- tions from perfect alignment (Fig. 17). This me- thod is a precise way to measure alignment para- meters and, possibly, align two-grid systems with extremely high precision in the future.

Fig. 16. Lightened triangle and diffraction strips based on a two-grid collimator.

Fig. 17. Position of diffraction strips relative to the triangle shown in Figure 5.

The ASPIICS coronagraph onboard Proba-3 PROBA-3 is the next project in the PROBA line initiated the development of the ASPIICS/ of technology demonstration satellites developed PROBA-3 SOC. The key objectives are the prepa- by the European Space Agency. The PROBA-3 ration of long- and short-term plans for ASPIICS mission consists of two spacecraft, and hosts two operations, the optimization of its science return, scientific instruments. DARA is an absolute ra- and the provision of the mission's outputs to the diometer, designed to measure total solar irra- science community and to the community at large. diance. ASPIICS (Association of Spacecraft for The CBK PAN's contributions to the ASPIICS/ Polarimetric and Imaging Investigation of the PROBA-3 SOC group are as follows: Corona of the Sun) is a coronagraph equipped • The CBK PAN will contribute, in colla- with an external occulter, which is placed on one boration with the ISS (Romania), to the inde- spacecraft and an optical telescope on the other. pendent testing and verification of ASPIICS/ The two craft will fly on a highly elliptical orbit PROBA-3 SOC performance. The aim is to verify around the Earth, and precise formation flying correct performance, by developing the Parame- around the orbit's apogee will accurately align the terizable ASPIICS Instrument Emulator (PAIE). telescope and the external occulter in a Sun- The PAIE will consist of two distinct modules, pointing direction. The outcome will be a very low namely the Instrument Environment (INS- baseline coronagraph configuration (around 150 TENV) module and the Detector Electronics m); this is an a unique opportunity to study dyna- (DETEL) module. The CBK PAN is responsible mic plasma processes in the Sun's magnetized for development of the DETEL module. atmosphere in eclipse-like conditions for exten- ded periods, by observing the solar corona close • Another, simplified version of the PAIE will to the solar limb and under very low straylight also be developed. This tool will estimate the conditions. exposure time of the ASPIICS instrument during PROBA-3's observation campaigns. The emula- The ASPIICS instrument PI, in collaboration tor will be known as the Image Quality Emulator with the PROBA-3 ESA Project Officer and a (IQE), and will operate at fixed values that repli- consortium consisting of SIDC/ ROB (Belgium), cate some of the PAIE's parameters (e.g. perfect MPS (Germany), INAF (Italy), CBK PAN (Po- Sun/ ASPIICS instrument alignment) and will ha- land), ISS (Romania) and IGAR (Romania) has

24 ve user-settable parameters such as exposure time, and forecasts about the state of onboard mass filters, and the position of the OSC and CSC memory. This will help to plan future observation along the orbit. programs in order to avoid overwriting existing • The emulator is required due to a limited data that can contain scientifically-interesting me- telemetry budget and limited onboard mass asurements. memory. The software will provide information

Thermal properties of coronal cavities Cavities are dark, elongated, elliptical structures Using SDO/AIA (Solar Dynamics Observatory, with rare? ed density. They often surround quies- Atmospheric Imaging Assembly) data and the cent prominences, especially in the polar-crown XRT_dem iterative2.pro routine, we calculated dif- regions. They are long-lived, their structure chan- ferential emission measure (DEM) maps and pro- ges slowly with time, but they can also erupt as files for a cavity-streamer system. We calcu-lated coronal mass ejections (CME). The thermal pro- averaged temperature in each pixel (Fig. 18), but perties of cavities have been studied for many also measured averaged temperature in the centre years, addressing the question of whether a cavity of a cavity (white box) and in the surroun-ding is hotter or cooler than the surrounding helmet streamer (red box). streamer, which is important for constraining co- ronal cavity models.

Fig. 18. Left: AIA 193 Å image of the cavity observed on 20 March 2012. This image was enhanced using the aia_rfilter procedure. Average temperatures were measured in the white and red boxes (for cavity and streamer, respectively). Right: Average temperature map (log T).

Fig. 19. DEM profile of the 20 March 2012 cavity (the signal was averaged over the white box in figure above). The red line represents median profile. Errors were obtained from 100 Monte Carlo samples. Right: DEM profile for the surrounding streamer (the signal was averaged over the red box in figure above).

25 Fig. 20. 20 March 2012 cavity: DEM maps for two temperature ranges, 2.2–2.5 MK (left) and 2.5–2.8 MK (right).

Cavities are ? lled with hotter material than their surroundings (Fig. 19). These results are consi- stent with most other observational studies. DEM maps show that cavities dominate over the sur- rounding corona in the temperature range 2.2–2.8 MK (Figure 20). This is particularly evident du- ring solar minimum. The temperature of the cavi- ty may differ in diffrent parts of the cavity. Usually it is slightly hotter above the centre and difrences can reach up to 0.1 MK. Cavities exhibit more thermal variability than streamers. In all 33 studied cases cavity tempera- tures were higher than streamer temperatures at a similar coronal height (Fig. 21). Diffrences bet- ween these temperatures are in the range of Fig. 21. Average temperature of analysed cavities (black) 0.11–0.32 MK, with an average value of 0.21 MK. and surrounding streamers (red). Cavities observed during solar maximum have average temperatures in the range 1.85–2.15 MK, while those observed during solar minimum have temperatures in the range 1.67–1.88 MK. (M. Stęślicki)

R&D collaboration with industry National Centre for Research and Development In 2019, researchers from the Zakład Fizyki Słoń- in 2017, and the project received funding in 2019. ca (ZFS) coordinated work on a new generation Work began in October. The CBK PAN is a leader of gaseous radiation detectors for pico- and in the MGEM Consortium, which also includes nanosatellite platforms, within the framework of Wrocław University of Science and Technology the Modular GEM Detectors (MGEM) project. and partners from industry (the Technology Tran- We hope to develop on-ground applications for sfer Agency TECHTRA and the Wrocław Tech- these detectors. A proposal for funding to work nology Park). on these detectors was submitted to the Polish (The ZFS team)

26 OTHER PROJECTS (18–21 and 35–40 µm) will allow us to interpolate the background level of radiance in the middle MIRORES band, which varies as a function of incidence

In 2019, ZFS team work focused on the MIRO- angle, emission angle, atmospheric H2O and other RES (Martian far-IR ORE) spectrometer, factors. Our biggest challenge is the small field of shown in Figure 22. MIRORES is a new instru- view, and the high resolution required for our ment that can take measurements in the 18–40 µm study (10–20 m/ px), which in a small space can range of the far infrared spectrum. The middle only be achieved by the use of the Cassegrain band is 23–28 µm, where we expect see an absorp- optical system. The instrument is equipped with tion peak for ore minerals. The other two bands three Pyroelectric Laser Detectors (Model 420).

Fig. 22. The MIRORES infrared spectrometer and the Cassegrain optical system. (J. Bąkała, the ZFS team and the Mars group)

Cubesat 3U sphere physics, geophysics and high energy char- Figure 23 shows Cubesat 3U, which is a ged particle physics (cosmology), based on obser- Polish–Ukrainian satellite instrument equipped vational data collected for the Sun, seen as a star in with three, multi-channel X-ray detectors (each X-rays. The MiRA_ep is a particle detector that with 256 energy channels) and a CMOS matrix measures electrons and protons in the 0.2–40 imager (a pin-hole detector). Two of the detectors MeV range. This miniaturized recording analyser and the pin-hole imager will operate in the soft will study the nature of charged particle micro- (0.8–15 keV) and a harder (5–150 keV) energy bursts at LEO, verify the existence of an additio- domain. A silicon drift detector (SDD) and a nal, inner electron radiation belt at L ~ 1.6 for CdTe detector will be oriented towards the Sun. particles with energies ranging from tens of keV The third SDD detector will measure particle to ~0.5 MeV. It will determine the energy spectra background and ambient soft X-ray emissions of stationary particles, together with those in within Earth's ionosphere (auroral X-ray emis- radiation belts and in microbursts outside the sions) or atmosphere (solar X-ray induced Argon belts, and the degree of anisotropy in electron fluorescence). The pin-hole detector will take velocities and in the midpoint of the radiation. images of the solar disc and the surrounding Furthermore, it will search for, and identify, the corona with spatial resolution of 2048 x 2048 distinctive features of microbursts of electrons pixels. The main scientific aim of the project is to generated by magnetospheric, solar and interpla- investigate carefully-selected fundamental pro- netary activity, and bursts correlated with seismic blems in the field of heliophysics, Earth atmo- activity.

27 Fig. 23. The Cubsat3U standard satellite equipped with a solar spectrometer and particle detector.

(J. Bąkała, the ZFS team and O. Dudnik)

STIX The Spectrometer Telescope for Imaging X-rays In 2019, our work aimed to develop an image (STIX) is an X-ray imaging spectrometer opera- reconstruction algorithm that was unconstrained ting in the 4–150 keV range. It is installed onboard by analytical simplifications or restrictions. We the Solar Orbiter mission. It is equipped with 30 abandoned Fourier's approach to image recon- pairs of grids and pixelized Caliste-SO detectors struction, and instead used the number of counts that can measure the Fourier components of solar recorded in each detector pixel. We used this data flare HXR emissions. These measurements make to reconstruct each image using a classical Ri- it possible to reconstruct images with an angular chardson–Lucy (R–L) algorithm. Knowing the resolution of the order of 7 arc sec. Given that the instrument's geometry, we were able to calculate perihelion distance for the Solar Orbiter will be the detector's response for point sources. We assu- 0.3 au, these HXR images will have an unpre- med a point source of a 1x1 arc sec pixel on the cedented spatial resolution of 1000 km. Sun. Once we had calculated the point source re- The STIX imaging concept is based on pairs of sponse for a grid covering the entire solar disc, we grids that have already been used in several ins- were able to iteratively combine point source res- truments (Fourier imagers). The main characte- ponses with varying weights until the best match ristic of Fourier imagers is that the image is not between reconstructed and observed detector obtained directly. Rather, the imager consists of responses was achieved. pairs of grids with various pitches and orien- We performed tests on various emission source tations. Each pair of grids modulates the inco- configurations, and compared the results with ming radiation depending on source size and CLEAN-Vis. The test configurations were: location. When sets of intensities are measured • Two Gaussians with a dynamic range 3 : 5; with dozens of grid pairs, we can reconstruct the • Two Gaussians with a higher dynamic range spatial distribution of X-ray emissions. In pre- 1 : 5; vious experiments the front and rear grids were shifted in phase while the slats were parallel. In • Two Gaussians, low signal. The total number STIX, the front and rear grids are slightly tilted, of counts recorded by all 30 detectors was less producing a characteristic Moiré pattern in the than 1000; detector plane. • Faint structure, small sources located close to each other, each source was smaller than the

28 instrument's angular resolution; • Typical flaring geometry: two foot points, loop-top source, above loop-top source. Figure 24 presents simulated configurations (first column), images reconstructed with the CLEAN- Vis algorithm (middle column), and the results of the reconstruction based on the R–L algorithm (right column). The images reconstructed with the two algorithms show the same number of so- urces. The exception is a fine structure, but in this case, the size of the model's sources were below the STIX angular resolution. Our algorithm is the most straightforward ap- proach to the image reconstruction problem. Despite its simplicity, it is very well-suited to de- tailed photometry of solar HXR sources. Pre-li- minary tests show that is can reproduce high-qua- lity images. Our main conclusions are as follows: • The algorithm gives stable results, with a slight tendency towards over-resolution. This can be easily avoided by using the stopping parameter related to the rate of χ2 change. • Although it is slow, the result is comparable to that obtained using Clean-Vis within 20–50 iterations; the computation takes less than 2 se- conds on typical portable computer. • Sources are very accurately reconstructed. Location, size and intensity are very similar to Fig. 24. Simulated emission source configurations (left simulated ones. The algorithm appears to be very column), images reconstructed with the CLEAN-Vis well-suited to detailed photometry of solar HXR (middle column), and R–L (right column) algorithms. sources. (M. Siarkowski, T. Mrozek)

TESS (the Transiting Exoplanet Survey Satellite) In 2019, ZFS team began work with the Astrono- The survey is divided into 26 observation sectors, mical Institute (University of Wroclaw) on a pro- and each sector will be observed during two, 13.7- ject to search for stellar flares in observations of day orbits. light curves recorded by TESS (the Transiting TESS will conduct high-precision photometry of Exoplanet Survey Satellite). TESS is the successor 200 000–400 000 stars at a cadence of approxima- to the Kepler mission and is mainly intended to tely 2 minutes. Such a high cadence can be very search for non-solar planets using the transit useful for studying stellar flares, but such a large method. This mission will conduct high-precision number of stars requires the automation of se- photometric observations of the entire sky in the arch procedures. We are currently preparing and spectral band 6000–10000 Å. testing the code for automatic detection of flares, Starting in August 2018, for a planned period of and procedures for the classification of stars for two years, the satellite will survey 85% of the sky which such flares have been observed. using four, wide-field cameras (telescopes and Figure 25 shows an example of flares found on associated Charge Coupled Device detectors). the ~27 day light curve of the star TIC 25132999

29 measured during the transit of Sector 1. The that virtually all observations are publicly available enlarged profile of one of these flares is shown in as soon as they are completed. Figure 26. The advantage of the TESS mission is

Fig. 25. TESS light curve for TIC 25132999, observed Fig. 26. The enlarged profile of one of the flares from during Sector 1. Flare maxima are indicated by red Figure 25. The green line denotes mean star flux. asterisks. (M. Siarkowski) The SolpeX pin-hole soft X-ray imager-spectrophotometer Proper operation of Solpex's Rotating Drum Spe- cal/ EUV emissions. A filter made of aluminized ctrometer requires timely information about any polyimide will transmit in the range E > 0.35 keV; X-ray activity that might be occurring on the solar this spectral range is similar to that covered by the disc. Such information can be obtained from a XRT Ti-poly filter on Hinode. The X-ray image of simple pin-hole telescope/ imager/ spectrometer the solar disk is formed behind the pin-hole on a (PHI) equipped with a thermal filter that trans- square 2k × 2k CMOS (Gpixel Inc.). mits solar soft X-rays and rejects thermal/ opti-

Laboratory tests and simulation In 2019, we carried out several thermal and mechanical simulations. Figure 27 presents a static, thermal simulation. The CMOS that is expected to be used in the PHI is characterized by good energy resolution, provided that single X- ray photons strike the pixel. The energy resolution of the CMOS pixel is illustrated in Figure 29. With a frame read-out time of 1/8 s, a single photon/ pixel scenario will take place most of the time, except for the most powerful flares, when double strikes/ pixels are expected. An amplitude analysis of the signal from individual CMOS pixels will be used to discriminate solar X-ray photons from those due to secondary fluorescence or energetic particles. The brightness profile can be created for selected energies that are representative of individual spectral bands. The spatial resolution is presented in Figure 30. Fig. 27. PHI - thermal simulation. The power source (2 W) is on the CMOS chip (yellow). The temperature at the end of the heat pipe (dark blue) is - 30 °C.

30 Figure 28 presents the results of resonance tests for three PHI locations. Simulations were perfor- med for frequencies in the range 100Hz to 2300Hz.

Fig. 29. Histogram of energy spectra recorded by the CMOS detector in laboratory conditions.

Fig. 28. PHI resonance test. Figure 29 presents X-rays reflected from a multi- metal foil system consisting of Al, Ti, Fe, Cu and Mo recorded by the Gpixel Inc. CMOS (GSEN- SE400 BSI). It shows escape peaks from Cr and Ti. Foils were illuminated by an X-ray lamp set at 35 keV. Individual peaks, due to characteristic Kα emission are easily discernible. The ambient temperature during measurements was 20 °C. To avoid pileup, measurements were taken 120 times Fig. 30. Part of the image recorded by the CMOS CCD illuminated by the X-ray lamp, through a steel mesh. The with 8 ms single exposition. The CMOS matrix pixel shown here is 11 µm x 11 µm in size. was shielded from direct illumination coming from the X-ray lamp itself. The readout and control system for this CMOS readout was based on a FPGA Spartan 6 XCFSLX9. (M. Kowaliński, J. Bąkała)

HIPERO

HIPERO (the High Performance Reconfigurable As part of my doctoral thesis, I developed the On-Board Computer) is shown in Figure 31. This underlying concept of the SEMICAP module. onboard computer is designed for microsatellites. This module ensures HIPERO's reliability in the Size, weight and power limitations mean that, un- case of soft errors, by continuously scrubbing the like state-of-the-art large missions, payload data configuration memory and enabling its dynamic processing and command & control functions are reconfiguration. The HIPERO demonstration implemented on a single platform. At the same tested the computer's basic functionalities, and time, the machine must meet demanding requi- implemented the first version of SEMICAP. The rements in terms of computing power, and it is system was launched as part of the Xilinx KCU therefore based on one of the newer families of 105 Evaluation Kit. It was necessary to thorou- FPGA systems (Kintex Ultrascale). However, ghly analyse the FPGA system configuration in such systems rely on SRAM memory, which is vul- the Xilinx Kintex Ultrascale family. To do this, a nerable to soft errors in the radiation environ- configuration file parser, and a preliminary ment. Consequently, it is necessary to use techni- version of a tool that makes it easier to test the ques that mitigate the impact of such events. functionality of the SEMICAP computer (by injecting errors) were developed.

31 An initial version of the re- liability model, based on the Kintex Ultrascale system with the SEMICAP module was also developed. Ultima- tely, the model will make it possible to analyse the vul- nerability of a specific im- plementation to soft errors, and generate data that will help to increase the relia- bility and availability of the Fig. 31. Components of the HIPERO demo model (the SEMICAP module is system. highlighted). (D. Ścisłowski)

Participation in NASA projects The CubiXSS Project in a wide temperature range, will test chromo- spheric evaporation and direct coronal heating Together with its American partners, the ZFS models of hot plasma formation in solar ? ares group prepared an updated proposal for a new, over timescales as short as a few seconds. The solar X-ray instrument The CubeSat Imaging X- technology question is: How do elemental abun- ray Solar Spectrometer (CubIXSS, pronounced dances vary within and across active regions (AR)? “cubics”) bridges a crucial, decades-long gap in AR measurements require the definition of a ~0.25–3 keV soft X-ray spectroscopic observa- spatial resolution to quantify the contributions of tions needed to measure many key low- and high- individual ARs to the total SXR spectrum. The FIP ion species across a coronal temperature aim of CubIXSS is to demonstrate and further range ~l to >30 MK simultaneously. CubIXSS is develop new, robust techniques to analyse disper- motivated by a compelling, overarching science sed spectral images. This, in turn, will enable a new question: class of high-sensitivity, spatio-spectral X-ray What are the origins of hot plasma in solar ? ares instruments. An example of simulated CubIXSS and active regions? observations is shown in Figure 32. CubIXSS addresses this issue via two questions. The CubiXSS proposal was submitted to NASA's The measurement question is: How do elemental H-FORT program. The Zakład Fizyki Słońca abundances vary within and across solar ? ares? plans to contribute to camera drive/ readout ele- CubIXSS measurements of coronal composition, ctronics, instrument calibration and data analysis.

Fig. 32. Simulated CubIXSS observations.

32 The FOXSI Project The ZFS group contributed the Spectrometer for In 2019, work was continued on the Focusing Temperature and Composition (STC) to the pro- Optics X-ray Solar Imager (FOXSI) project, in ject. The STC extends FOXSI measurement collaboration with our American partners. The capabilities to softer X-rays. Two of our scientists aim of the project is to develop the first solar are Co-Investigators. The assessment phase instrument with direct imaging capabilities in hard ended in 2018 and, in February 2019 these two X-rays. It addresses the universal science ques- Co-Investigators and an engineer from the ZFS tions of heating and particle acceleration in visited NASA's Goddard Space Flight Center to magnetized plasmas. In particular: present a working prototype of the STC to NASA experts for evaluation. An example of the X-ray 1) How are particles accelerated at the Sun? spectrum measured by the STC prototype is 2) How do solar plasmas get heated to high shown in Figure 33. Although FOXSI scored temperatures? highly in the evaluation it was not, in the end, 3) How does magnetic energy released on the Sun selected by NASA for continuation into the im- produce flares and eruptions? plementation phase.

Fig. 33. Spectrum of 55Fe source measured by the STC prototype at NASA's Goddard Space Flight Center.

(Sz. Gburek, M. Stęślicki, P. Podgórski) The FIERCE Project A FIERCE Spectrometer to Measure • What are the physical origins of space weather Temperature and Composition events? FIERCE is a proposed MIDEX mission concept. • What are the dominant initiation mechani- The planned launch date is mid-2025, with a two- sms for flares and CME? year prime mission. FIERCE's co-optimized X- • What are the origins and properties of ele- ray and EUV observations capture the full emis- ctrons escaping the Sun? sion range in solar flares and CME – from the lar- • How are particles accelerated at the Sun? gest X-class flares, to impulsive energy release in • Where and when do electron acceleration the quiescent Sun. FIERCE links the intricate and local plasma heating occur in coronal evolution of particle acceleration to the dynamics and chromospheric structures? of plasma structures at all significant spatial and • What is the efficiency, and what drives the temporal scales. sustainability of electron acceleration? The science questions that the mission will • How is impulsively-released energy transported address are: in the solar atmosphere?

33 Fig. 34. Fully-deployed observatory.

Fig. 35. FOXSI and STC cutaway view. • How and where do accelerated electrons instruments: lose their energy in the corona and chro- • The Focusing Optics X-ray Solar Imager mosphere? (FOXSI) - the first ever, solar-dedicated, • How is hot flare plasma produced and direct-imaging hard X-ray spectroscopic how does it evolves? imager. • How is the solar corona heated? • A Thermal and Dynamic Imager for the • Is energy release in small flares funda- Sun (THADIS) - a high-angular-resolu- mentally different from that in large fla- tion EUV imager with fast cadence and res? very short exposure times. • What are the properties of unresolvable • The Spectrometer for Temperature and events that heat active regions? Composition (STC) - a soft X-ray spectro- The FIERCE mission will have three onboard meter with high spectral resolution.

Fig. 36. The temperature response of FOXSI ranges from ~2 to >50 MK, making it possible to characterise all relevant heated plasmas.

34 Fig. 37. The combination of FOXSI and STC enables FIERCE to constrain the presence of hot plasmas with high con- fidence, even in the presence of large amounts of cooler plasma. (A) The 'input' temperature distribution (black), or differential emission measure (DEM) from a simulation of AR 11726, and the reconstruction from simulated FIERCE observations (green curve with shading for 90% confidence limits) agrees with the input distribution over 3–25 MK. The comparison with a DEM for a steady-heating model (red) illustrates the dramatic lack of plasma at high temperatures in the absence of nanoflare heating. (B) The simulated count spectra for STC (green) and FOXSI (red) used for the reconstruction take into account realistic uncertainties in calibration and statistical noise in source and background. The CBK PAN contributed the STC instrument FOXSI FOVs remain coaligned, even in the case to the mission. This instrument complements of boom motion and effectively eliminates vignet- FOXSI's and THADIS's images by producing ting for the STC FOV (Fig. 38 ). high-resolution soft X-ray spectra, and provides STC detectors output histogrammed spectra independent measures of solar X-ray flux to aid (photon counts vs. energy) over a configurable FOXSI in selecting appropriate attenuators to energy range (nominally 0.8–20 keV), with 512 manage detector count rates during large flares. channels and 0.5-second cadence. The instrument provides soft X-ray spectroscopy from ~1 keV to ~15 keV, thus extending the FO- XSI temperature response down to ~2 MK and providing access to spectral lines of various ions (Figure 36 and Figure 37). The STC consists of two silicon drift detectors (SDD), their associated readout and interface electronics, and collimating baffles. The two pa- rallel detector channels, STC-Q and STC-F, have effective areas of 1 mm2 and 0.02 mm2, respecti- vely, to span the entire flux-intensity range up to X-class flares. Additionally, the STC FOV is matched to the FOXSI FOV by placing the FOV-defining aper- tures at the FOXSI's Mirror module assemblies Fig. 38. 3D models of the STC detector unit and the Solar and the STC detectors next to the FOXSI detector Aperture Plate (not to scale). board. This configuration ensures that STC and (Sz. Gburek, M. Stęślicki)

35 DATA ACQUISITION

The CBK PAN's Astrogeodynamical Observatory in Borowiec The GNSS BOR 1 station In 2019, the long-term provision of Global Navigation Satellite System (GNSS) data from the BOR1 station, for national and worldwide scien- tific surveying was secured. This permanent GN- SS station is located at the CBK PAN Borowiec Observatory and, since 1996, it has been inte- grated into the International GNSS Service (IGS) and EUREF networks. Data streams from the BOR1 station have been made available through IGS-IP and EUREF-IP Fig. 1. GNSS satellites observed by the BOR1 station. projects. High-quality data files make a valuable contribution to global geodesy and related rese- antenna, which collects signals from GPS, GLO- arch within the IGS framework. Data provided by NASS, GALILEO, BEIDOU, QZSS and SBAS BOR1 are used for precise orbit calculations by systems. many international institutions, such as CODE Since 5 February 2015 the BOR1 station has been (Central Orbit Determination Europe) at Bern, equipped with a multisystem Trimble NetR9 Switzerland, the GFZ-IGS Processing Centre in receiver. This multichannel (440 channel) receiver Germany, the JPL-IGS/FLYNN Processing is capable of gathering signals simultaneously Centre at Pasadena, USA, the Massachusetts In- from GPS, GLONASS, GALILEO, BEIDOU, stitute of Technology in the USA, the Scripts In- QZSS and SBAS constellations. stitution of Oceanography in the USA, and the In 2019 a new computer was bought; this machine National Geodetic Survey in Canada. The BOR1 has been equipped with newer software that is station is one of the reference stations within the dedicated to the conversion of raw data into for- multifunctional, precise satellite positioning sys- mats required by the IGS (i.e. RINEX 2.11 and tem established by the Head Office of Geodesy RINEX 3.02). This seemingly small change has and Cartography in Poland. All of the station's significantly improved the station's stability (Fi- data are provided in two formats: RINEX 2.11 gure 3). and RINEX 3.02. All data are gathered by a Trimble Dorne Margolin with choke ring antenna

Fig. 2. Current constellations of GNSS satellites.

36

Fig. 3. The influence of the new hardware/ firmware configuration on BOR1's stability. The time of the update is marked by the red line. (P. Lejba) The BORL satellite laser ranging station From an observational point of view, 2019 was a med. Information about the position and successful year for the CBK PAN's laser ranging behaviour of space debris, such as defunct satel- station, BORL—the station recorded almost lites, is very important from the point of view of 1500 passes of tracked objects. It tracked 88 future debris removal missions (e.g. ENVISAT) as different objects, satellites and space debris, with a the amount of space junk is increasing rapidly. total of 1468 full passes (Fig. 4). Forty-four were Currently there are more than 20000 objects in satellites, 30 were Low Earth Orbit (LEO), and 14 orbit with a diameter ? 10 cm (Fig. 5). We need to were Medium Earth Orbit objects giving1079 know not only where all these objects are, but also passes, 15197 normal points and pass RMS from precise information about their rotation/ tum- 1.20cm to 3.81cm. Thirty-eight objects were bling and orientation in space. Laser measure- typical space debris, such as inactive (defunct) ments recorded by the BORL station support satellites and rocket bodies (boosters) from the global research on the determination of space LEO regime giving 389 passes, 4074 normal debris spin dynamics (ENVISAT, ERS-1, ERS-2, points and pass RMS from 2.04cm to 221.72cm. OICETS, SEASAT-1, TOPEX/ Poseidon and These targets were observed within the others), which is essential to improve theories of framework of the Space Debris Study Group, run the movement of artificial satellites, including by the International Laser Ranging Service (ILRS) space debris. All of the station's results were sent under internal contracts signed with the to the Crustal Dynamics Data Information Sys- European Space Agency (ESA) and the European tem (CDDIS), the EUROLAS Data Center Consortium EUSST (https://www.eusst.eu/). (EDC) and Space Debris databanks. A total of 388 space debris passes were perfor-

37 Fig. 4. Observational statistics recorded by the BORL station in 2019, including active satellites and space debris (green column – the highest number of passes; red column – the lowest number of passes).

Fig. 5. Map of all space objects in orbit with a diameter ? 10cm (Orbitron software, http://www.stoff.pl/). Among the tracked satellites 11 were geodetic- for LAGEOS-1. Mean RMS ranged from 1.55cm geodynamic (AJISAI, ETALON-1, ETALON-2, (for LAGEOS-2) to 3.81 (for AJISAI). GRACE-FO-1, GRACE-FO-2, LAGEOS-1, The quality of the BORL laser sensor is regularly LAGEOS-2, LARES, LARETS, STARLETTE evaluated, based on tracking results for LAGE- and STELLA), which gave a total of 443 passes OS-1 and LAGEOS-2 satellites, in the form of a and 4933 normal points. Table 1 presents a station performance report. As the results given in summary of observational statistics. Figures 6 and 7 show, the BORL station has signi- The highest number of passes (100), returns ficantly improved the quality and effectiveness of (125946) and normal points (923) were obtained its measurements compared to previous years.

38 Table 1. Observational statistics for geodetic satellites.

SATELLITE NORMAL AVG RMS PASSES RETURNS NAME POINTS [cm] AJISAI 62 84860 785 3.81 ETALON-1 3 453 14 3.76 ETALON-2 4 295 20 2.60 GRACE-FO-1 23 9880 564 3.08 GRACE-FO-2 11 5291 285 2.88 LAGEOS-1 100 125946 923 1.76 LAGEOS-2 43 43780 440 1.82 LARES 75 37186 821 1.55 LARETS 56 21245 405 2.16 STARLETTE 53 46889 573 2.31 STELLA 13 7851 103 2.07

Fig. 6. LAGEOS normal point RMS from 2000 to 2019 for the BORL station (https://ilrs.cddis.eosdis.nasa.gov/net work/stations/charts/BORL_LAG_ NPT_RMS.png).

Fig. 7. LAGEOS normal point measurements from 2000 to 2019 for the BORL station (https://ilrs.cddis.eosdis.nasa.gov/network/stati ons/charts/BORL_LAGEOS_NPT_OBS.png).

39 In 2019, staff at Borowiec worked on the development of new software dedicated to the reduction of laser measurements (Figs. 8–10).

Fig. 8. Results of measurement reduction of ENIVSAT data (O-C residuals).

Fig. 9. Results of measurement reduction of TOPEX/ Poseidon data (O-C residuals and normal points).

Fig. 10. Results of measurement reduction of Chang Zheng 4C rocket data (O-C residuals with noise points).

40 This new software is designed to run on the new- an approved subcontractor. The BORL sta- est operating systems (Windows and Linux); it has tion is responsible for laser measurements of a very flexible graphical interface and allows a ran- cooperative and uncooperative targets. The ge of parameters to be determined (O-C residu- project will continue into 2020 and is led by als, normal points, RMS of normal points, RMS Airbus Defence and Space. of observations, time bias, range bias). The code • The European Space Agency project Laser was developed from specifications and require- Ranging Systems Evolution Study – Laramo- ments provided by the International Laser Ran- tions. The CBK PAN is an approved subcon- ging Service (https://ilrs.cddis.eosdis.nasa.gov/). tractor. The project will continue into 2020 At present, the software is in the testing phase. and it is led by the German Space Agency Other work focused on orbital calculations of DLR. space debris (13 targets, Russian and Chinese bo- • An observational contract, within the EUS- osters from the LEO regime). The aim of this ST, coordinated by the Polish Space Agency. analysis was to show how laser measurements The contract will continue into 2020. from one station can improve the identification In 2019, the BORL station focused on the Euro- of orbits of tracked rockets. All calculations were pean Space Surveillance & Tracking programme run using the advanced orbital programme (EUSST), which constitutes one of the pillars of GEODYN-II (2017), based on laser measure- the Space Situational Awareness (SSA) program- ments recorded by the BORL station. Figure 11 me implemented by the European Space Agency presents the results of the comparison between (space safety in future years) and the EUSST Con- input ephemerides and positions obtained from sortium. The EUSST programme is dedicated to laser measurements. monitoring (observation, detection, identifica- Differences for all analysed targets are given in the tion) active and inactive satellites, discarded RSW satellite frame between TLE (initial orbital launch stages and fragmentation debris orbiting elements) and observations recorded by the BO- Earth. The BORL station is responsible for rese- RL station (corrected elements/ positions). Short arch and development in the area of satellite laser observations of rocket bodies from the LEO re- ranging. Poland is an official member of the EU- gime, ranging from a dozen to several dozen se- SST Consortium, and the CBK PAN is one of the conds improve the covariance matrix by 20–40%. members of the Polish SST consortium. In 2019, staff at the BORL station were involved In 2019, BORL staff participated in the ILRS in the following projects: Technical Workshop held in Stuttgart (Germany), • The International Laser Ranging Service 21–25 October. Dr Eng. Tomasz Suchodolski, a (ILRS) project, Special Mission Support. lead engineer at the BORL station, presented the This is an observational campaign dedicated Centre's work on the topic of CBK PAN Borowiec to SENTINEL-3A and SENTINEL-3B Second Satellite Tracking System. Dr Suchodolski is satellites. The CBK PAN was an approved responsible for the development of a second, subcontractor and the project is ongoing. In independent optical-laser setup dedicated to the 2019, the BORL station collected 67 passes SST/Space Safety (ESA) and SST (EUSST) pro- of SENTINEL-3A with 1032 normal po- grammes. The conference proceedings are ava- ints, and 69 passes of SENTINEL-3B with ilable at https://cddis.nasa.gov/. 1105 normal points. In 2019, the Centre's researchers prepared ano- • The European Space Agency's WebPlan pro- ther paper titled Optical, Laser and Processing Ca- ject, is part of the framework of the Polish pabilities of the New Polish Space Situational Industry Intensive Scheme. The CBK PAN Awareness Centre. This was published in the Pro- is an approved subcontractor. The project ceedings of the Advanced Maui Optical and Space will continued into 2020. The project is led Surveillance Technologies Conference (AMOS), by the Polish company, Sybilla Technologies. 17–20 September 2019 (https://amostech.com/ • The European Space Agency's project SST 2019-technical-papers/). This paper, among Sensor Data Acquisition. The CBK PAN is others, outlines the current situation at the BORL station with respect to its SST activities.

41 Fig. 11. Comparison of TLE ephemerides and laser measurements. (P. Lejba) The Global Navigation Satellite System (GNSS) Observatory in Warsaw The observatory is involved in the following pro- - monitoring the quality of EGNOS corre- jects: ctions in the context of the EGNOS Service - the GALILEO global navigation system, Performance Monitoring Support (SPMS) - positioning measurements and defining the project, national reference frame with GNSS techno- - the Galileo Reference Centre – Member Sta- logy, tes project.

GALILEO Each week, the European Space Research and Te- In 2009, a new GESS+ (Galileo Experimental chnology Centre (ESA-ESTEC) generates repor- Sensor Station) was installed at the CBK PAN. ts of the status of stations and observation data After few months of testing observed data quality, quality for GPS and Galileo signals. In the context the station was included in the global monitoring of monitoring the Galileo system, the CBK PAN network of Galileo In-Orbit Validation Element is participating in the GSA project known as the (GIOVE) satellites. Galileo Reference Centre – Member States.

Fig. 12. The new GALILEO GESS+ station (GWAR) at the CBK PAN, Warsaw.

42 GNSS PERMANENT STATION system as the CBKA station. In 2015, a GNSS Trimble NetR9 receiver was installed at the sta- Since February 2003, a permanent GPS station tion. Currently, the CBKA station also provides operated in Warsaw, as part of the pilot project observational data for two GSA projects related to known as the Active Geodetic Network for monitoring the quality and availability of EG- Poland (ASG-PL). Since December 2007, that NOS corrections, and monitoring of the Galileo station has been included in the ASG–EUPOS system.

The European Geostationary Navigation Overlay Service (EGNOS)

Fig. 13. The EGNOS Ground Segment.

The CBK PAN in Warsaw is the location for a In addition to the RIMS station, the CBK PAN is Ranging and Integrity Monitoring Station (RIMS cooperating with European institutions on rese- WRS). This station is part of the EGNOS System, arch based on the EGNOS System. Specifically, it which is designed to broadcast correction signals is participating in the EGNOS Service Moni- in Europe to improve GPS performance (Fig. 13). toring Support project. (L. Jaworski, A. Świątek) The LOFAR4SW project: improving space weather research The LOFAR for Space Weather (LOFAR4SW) observing window. LOFAR4SW officially started project is a part of the Horizon 2020 Work Pro- in December 2017 and, since then, rapid progress gramme. As a final result it will deliver the techni- has been made. The Centrum Badań Kosmicz- cal and conceptual design of a facility which pro- nych PAN is one of the leading partners in the duces unique research data that will have a key project, being responsible for the coordination impact on advanced predictions of space weather and execution of Work Package 8 (Dissemination events. The project is based on existing LOw Fre- and Exploitation), and providing scientific input quency ARray (LOFAR) infrastructure, already related to ionospheric studies with the LOFAR the world's leading telescope for radio astronomy instrument. research in the low-frequency 10–240 MHz

43 In the course of the project so-called 'Science Use monitoring in the imaging and dynamic spectrum, Cases' were defined describing scientific topics Faraday rotation measurements using observa- where significant progress can be achieved with tions of pulsars, Interplanetary Scintillation (IPS) the fully-operating LOFAR4SW infrastructure. monitoring and ionosphere monitoring using The project will focus on processes observed at dynamic spectrum, and all-sky imaging. the Sun, in the solar wind and in the Earth's iono- In September 2019, the Mid-Term Review was sphere. This can provide new insight into the held in Brussels. The project was very well complex interactions that drive observed space received, and the EC Project Officer and External weather conditions. Reviewer were “impressed by the excellent science The preliminary version of the LOFAR4SW use cases, smooth management and positive design, which will be developed and tested before attitude within the project-team”. the end of the project, aims to provide solar (B. Matyjasiak, H. Rothkaehl)

44 INTERPRETATION AND MODELLING SPACE PHYSICS ximum likelihood algorithm. In addition to the stronger lines, which have already been identified Solar Physics in previous work, a number of weaker lines are al- so clearly visible in the average spectrum, and (Wrocław Solar Physics Division) - belong to higher transitions in the He-like Si XIII Zakład Fizyki Słońca ZFS ion. This is the first time these weaker lines have An analysis of Diogeness data been observed and identified in astrophysical pla- smas. Diogeness (DIOG) is a soft X-ray spectrometer We also reduced spectra obtained in DIOGE- that has operated aboard the Russian CORO- NESS channel 2. In this case, a Beryl monocrystal NAS-F satellite since 2001. The instrument has was used as a dispersive element for Bragg refle- collected hundreds of high-resolution spectra ctions. The average spectrum in the spectral range from a period of high solar activity, including 6.3–6.8 Å is shown in Figure 2. X5.3 on 25 August 2001. In 2019, we ran an analysis of DIOG spectra in channels 2 and 3. This involved the removal of all spectral data disturbed by telemetry or detector problems, and the averaging of the spectrum over the entire flare duration (a total of around 30 scans).

Fig. 2. Logarithmic plot of the average spectrum in DIOGENESS channel 2 (black) together with the spectrum (violet) after deconvolving the instrumental profile (rocking curve of the Beryllium crystal). The Lorentzian rocking curve profile is shown (in blue) under the resonance line (w) of the He-like ion of Si XIII. The dotted vertical line represents the position of the Si absorption jump. Fig. 1. Logarithmic plot of the average spectrum in DIOGENESS channel 3 (black) together with the Like Figure 1, the violet line represents the spectrum (violet) after deconvolving the instrumental spectrum after removing the instrument profile profile (rocking curve of the ADP crystal). The (shown in blue). In addition to the strongest, Lorentzian rocking curve profile is shown (in blue) under the resonance line (w) of the He-like ion of S XV. known lines of He-like Si XIII, tens of weaker lines are present in this spectral range. All of these An example of the results of the analysis for lines are observed for the first time, and identified channel 3 is presented in Figure 1. In order to using atomic data from CHIANTI and Kelly decrease the influence of statistical noise, we re- spectral line tables. These weaker lines belong to moved (deconvolved) the instrumental profile the H-like Mg XII ion and represent spin doublet due to the finite width of the ADP rocking curve. transitions. It is possible that a few lines of highly- The flat ADP monocrystal was used as a disper- ionized Fe can also be seen in this spectral range. sive element. Deconvolution was performed We are preparing a paper describing our results for using the Withbroe–Sylwester (WS) Bayesian ma- submission to The Astrophysical Journal. The Bent Crystal Spectrometer The Bent Crystal Spectrometer (BCS) flew on- craft. During that time, it observed X-ray spectra board NASA's Solar Maximum Mission space- of numerous solar events during the periods

45 February to November 1980 and 1984–1989 in regions around the highly-ionized resonance lines of He-like Ca (Ca XIX) and Fe (Fe XXV). This enabled the diagnosis of plasmas with respect to temperature, turbulence, mass motion, etc. As, to date, there has not been a comparable spectro- meter with similar spectral resolution over such a long observation period, there is continued inte- rest in BCS data analysis. In 2019, we performed a precise analysis of spec- tra obtained during a scan carried out in No- vember 1980. This analysis highlighted anomalies in the crystal curvature of channel 1 (viewing lines of He-like Ca, Ca XIX and associated Ca XVIII dielectronic satellites), and helped to explain a longstanding anomaly in the intensity ratio of the Ca XIX intercombination lines x and y. We also carried out an in-flight estimation of the BCS collimator extent, which provides a better esti- mate of the absolute intensity of BCS spectra. An important implication of our work is that it con- firms the result of an earlier analysis of BCS Ca XIX spectra that implies a time-variable flare abundance of Ca. In Figure 3, we present the path scheme of Bragg reflected X-rays from the BCS channel 1 Ge cry-

Fig. 4. Time history of GOES, BCS channel 1 (Ca XIX spectra), and spectral line shifts for the 6 November 1980 flare (22:02–22:59 UT). Top panel: Channel 1 spectra plotted on a red temperature intensity scale (yellow for high intensities, blue low) with wavelengths in the channel 1 range (3.165–3.231 Å) on the vertical scale, increasing upwards. Second panel: BCS channel 1 photon count rates in the bin range 33–220 (wavelength range 3.174–3.227 Å for an on-axis flare) in units of 104 s-1 with GOES 0.5–4 Å (blue, multiplied by 2 x 105) and 1–8 Å (red, multiplied by 6x 104) light curves. Third panel: temperature (MK, red) and emission measures (multiplied by 1.2, units of 1048 cm-3, blue) derived from the emission ratio of the two GOES channels. Fourth panel: Channel 1 spectra (like those in the top panel, but normalized to the BCS total count rate in the 3.167–3.224 Å range). Bottom panel: wavelength shifts of spectra, expressed as relative bin number, determined from the two approaches. Fig. 3. Ray path schema for BCS channel 1 (Ca XIX) (courtesy of Jarosław Bąkała). X-rays from the Sun (up- stal. The mission's spacecraft performed raster- per left) pass through the 6 x 6 arcmin multi-grid colli- like scans over the active region AR2779, while the mator (front and rear grids are shown) and a thermal fil- M3.5 flare was occurring. This enabled line shifts ter, to the Ge 220 cylindrically-bent crystal wafer. Diffra- cted rays, incident on the bent crystal at angle θ, have in BCS spectra to be precisely related to spatial slightly different wavelengths as a function of their posi- shifts. The scanning motion of the spacecraft cau- tion along the crystal; radiation received by the position- sed line positions to “drift” in a wavy motion (illu- sensitive detector over a data-gathering interval forms a complete spectrum over a limited wavelength range strated in Figure 4). Each normalized spectrum in (3.165–3.231 Å for an on-axis flare in BCS channel 1). this bin range (3rd panel of Figure 3) was compa-

46 Fig. 5. Correction matrixes for wavelength and intensity to be used when reducing the BCS bin-spectra observed in channel 1 to linear units. Provided that the curvature of the Ge 220 monocrystal wafer has an ideal cylindrical shape, the white lines in the left panel should be straight, as should the corresponding background colour. In such a case, the right panel should be a uniform red colour, equal to 1.00. The patterns that are shown indicate the non- cylindrical profile of the Bragg-reflecting crystal surfaces. red with a normalized, reference spectrum to de- spectral bins to wavelengths, and to correct for termine an optimum shift in BCS bins. The me- intensity distortions caused by the non-ideally- thod was broken down into two steps: firstly, a cylindrical surface of the Ge monocrystal wafer multiplicative approach (black points) was app- used to Bragg-reflect the X-rays illuminating it lied; the shift corresponding to a maximum in the through the triangular profile of the collimator. product of the analysed and reference spectra was Figure 5 illustrates the bin-wavelength and offset- obtained; and secondly (red points), the shift cor- intensity correction matrixes that should be used responding to where the traditionally-defined χ2 in the future to reduce archived BCS spectra difference was minimal. For all phases (except C, (around 100 000) that have not, as yet, been pro- where no BCS spectra were observed), red points perly reduced. coincide with black points to within 0.05 bin. After introducing the recommended corrections, The analysis of line positions (offsets) during spa- spectra were averaged over Phases A, B & D and cecraft scans made it possible to determine the were found to correspond to modern atomic the- respective correction to be applied to convert ory. This is illustrated in Figure 6.

Fig. 6. Spectra (in black) averaged over Phase A, Phase B, and Phase D after introducing the necessary corrections. Reduced average spectra are best-fitted; the most-recent atomic theory counterparts (in red) contain not only the contribution of lines formed in Ca ions, but also in Ar (blue) falling in the spectral range of BCS channel 1. It should be noted that there is near-perfect agreement.

47 Fig. 7. Pattern showing the location of the source (green), for 67 consecutive time points representing start & stop times of spectra collections in Phase B, at a time when the spacecraft performed scanning along both E–W and N–S tracks. The transmission profile, shown in the background, is represented by a regular pattern that is triangular along E–W and N–S lines. Based on the ratios of total signal measured in BCS channel 1, and those observed by GOES in its 0.5–4 Å and 1–8 Å ranges, a detailed pattern of spacecraft scans emerges. This shows the location of the flaring, compact source within the field of view of the collimator. This pattern is presented in Figure 7. We are in the process of finalising a paper on the results of our work for submission to The Astro- physical Journal. (B. Sylwester, J. Sylwester)

Bent Crystal Spectrometer particle distribution maps We prepared a map based on X-ray spectra from For each observed spectrum in a given year, the the Bent Crystal Spectrometer/ Solar Maximum position of the satellite above the Earth's surface Mission device. This data was stored in 1042 bda was calculated, and the arithmetic means of maxi- files (several million spectra), covering the years mum spectral values were recorded. We found 1980, and 1984–1989. The particle distribution that these results were distorted by the appearance was examined separately for each year. of high-value detections in the studied areas when An array of 360x60 elements was determined, co- solar flare spectra were recorded. To remove this vering longitudes in the range 0–360º, calculated effect, we developed a method to automatically positively to the west, and latitudes from - 30– eliminate spectra during flare periods. 30º, i.e. the area covered by the Mission's orbit. (Z. Kordylewski)

Properties of crystals used in the Bent Crystal Spectrometer

XOP software (Xcrystal and Xcrystal_bent) was used to determine the theoretical properties of crystals used in the Bent Crystal Spectrometer (BCS) instrument flown onboard the Solar Maxi- mum Mission. Also the trial to determine the exact geometry of the BCS detector units was done but without success (so far), because of a lack of data. XOP software was also used to check the theoretical properties of Resik crystals for calculation integral reflectivity, peak reflectivity and FWHM for three orders of reflection. Calcu- lations were done for linearly polarized and unpo- larized light. Fig. 8. Integral reflectivity of Resik crystals for three orders of reflection, calculated using XOP software (Si 111 and Qu 10-10: first order; Qu 20-20: second order. No reflection of Si 111 in the second order; Si 333 and Qu 30-30: third order). (Ż. Szaforz)

48 SphinX sion measure EM. The temperature was obtained In 2019, we extended, revised and deepened the by fitting the observed spectrum to the theoretical scope of the analysis of spectra from the Polish one, in the statistically important range (1.2 keV< spectrophotometer SphinX, recorded during E < 2.7 keV). The emission measure was estima- periods of minimum activity, based on much-im- ted based on the total number of photons detec- proved instrumental data. Specifically, we sub- ted above 1 keV. The best fit isothermal spectrum tracted the average background spectrum, ob- to the average spectrum is shown in blue in Figure tained by summing a total of around 34 hours of 10. spacecraft night-time observations. These obser- vations concerned regions that avoided passages through the South Atlantic Anomaly, polar auro- ral regions and times when there were no magne- tic sub-storms. Background spectra (typically at energies ≤ 2 keV) include electronic noise, parti- cle emissions and fluorescence from the alumi- nium that makes up the bulk of the instrument's structure. These were subtracted from every ana- lysed spectrum, and for daytime observations for periods of at least 5 minutes when the D1 detec- tor count rate was less than 140 s-1. We identified 576 such intervals (non-active, NA), which are marked in red in Figure 9. Additionally, we selec- ted 40 small brightenings (B, shown in green) and 16 micro-flares (F, shown as blue vertical lines).

Fig. 10. SphinX NA spectra in the 1–6 keV range (thin- line histograms) for 576 time intervals when there was no discernible solar activity, and their average (thick black histogram). Spectra times can be roughly distinguished by the colours used in the histogram (blue = early in the mission, red = middle, yellow = late in the mission). For all spectra, the background spectrum was subtracted (the novel element in our analysis). The best fit isothermal spectrum is shown by the thick blue curve (corresponding temperature and emission measure values are also shown) and the thick green line shows the fit by folding the Fig. 9. X-ray emissions recorded by the SphinX D1 differential emission measure solution. detector (photon count s-1), plotted logarithmically for the period 20 Feb. to 9 Oct. 2009 (after these dates, solar Our initial analysis found poor agreement above activity increased and data were excluded). Red points 2.5 keV; a high temperature component is needed indicate the times of the 576 non-active (NA) intervals to account for emissions above this energy. There- when the count rate was < 140 s-1; green lines indicate the 40 brightenings (B). Times of the 16 micro-flares (F) are fore, in a second step, we analysed spectra in the indicated by thin, vertical blue lines beneath the light 576 intervals, with the assumption that the plasma curve. The GOES 1–8 Å lower threshold is indicated by is multi-temperature (differential emission mea- the horizontal dashed line, and GOES A1, B1, C1 levels, and S1 and Q1 levels (based on our SphinX data analysis) sure distributions were calculated adopting the are indicated by horizontal dotted lines. Withbroe–Sylwester algorithm). The results are presented in Figure 11, together with differential Spectra for all 576 intervals, together with the ave- emission measures calculated for an average spec- rage spectrum (black histogram) are shown in Fi- trum (the thick red histogram). The spectrum cal- gure 10. Spectra in these intervals were analysed culated for this distribution is shown in green in by isothermal approximation, which determined Figure 10, and this highlights much better agree- the average corona temperature T, and the emis- ment compared to the isothermal approach.

49 Fig. 11. Differential emission measures (cm-3 MK-1) Fig. 12. Distribution of differential emission measures for plotted against the logarithm of temperature (in K) average spectra for NA intervals (red), brightenings B derived for each of the 576 non-active intervals (shown in (green) and sub-flares F (blue). Uncertainties are indicated various colours), together with measures calculated for the by error bars in appropriate colours. average of the 576 spectra (thick red histogram). tenings (B) and 16 micro-flares (F). Isothermal fit These differential emission measures indicate the to averaged NA, B and F spectra was evaluated, at presence of a hotter plasma component at around increasing temperatures (1.69 MK, 1.81 MK and 2.4 MK, in addition to a cooler component at 1.86 MK). However, as fit to observed spectra was around 1.6 MK and the bulk of plasma present unsatisfactory for energies above 2.5 keV, dif- for all spectra. The hotter component has an emi- ferential emission measures were calculated. The ssion measure that is almost three orders of ma- results revealed a two-temperature component for gnitude smaller than the cooler one. A similar ana- the source plasma. In all cases, the bulk of the pla- lysis was run for brightenings and sub-flares, and sma has a temperature of around 1.6 MK. A small the cooler component was evident in both cases, amount (2–3 orders of magnitude less) of higher- although the temperature of the hotter compo- temperature plasma (~2.4 MK for NA periods nent is around 3.2 MK. This is illustrated in Figure and 3.2 MK for B and F) is necessary to account 12. for observed spectra above 2.5 keV. A paper des- To sum up, we carried out a reanalysis of SphinX cribing the results of this study is currently in print data for 576 intervals, lasting from 5 to 30 minutes in the journal Solar Physics. with extremely low intensity levels (NA), 40 brigh- (B. Sylwester, J. Sylwester)

RHESSI – SphinX

Background subtraction in RHESSI data. estimate background levels using one, average value, and do not include changes during the flare. The RHESSI instrument observed the Sun during Since 2009, the SphinX instrument, developed by the years 2002–2018, in the energy range 3 keV– the Centrum Badań Kosmicznych PAN's (CBK 17 MeV. Its detectors were not shielded against PAN) Solar Physics Division has been observing side illumination and, so, measured signals co- the Sun in the X-ray range. In 2009, solar magnetic ming from all directions. The instrument was in a activity was very weak. SphinX detected many low-Earth orbit, and periodically passed through events below B class flares; in particular, we found radiation belts and the South Atlantic Anomaly. 36 weak flares that were observed by both This makes it difficult to estimate the orbital back- RHESSI and SphinX, which constituted a great ground level, which is a key element in reliable, opportunity to carry out a precise, physical analy- solar flare analyses, especially for very weak flare sis of phenomena. Unfortunately, 24 of the 36 events. Most popular subtraction methods only were detected by RHESSI as it passed through a

50 radiation belt. This highlighted the need for a precise method to better determine the back- ground level and changes during an event. The RHESSI instrument was equipped with 9 germanium detectors, and each detector was divi- ded into a front and rear segment. The front seg- ment stopped photons and particles with energy below approximately 150 keV. Weak events are characterised by energies below 20 keV. This means that photons from weak flares are only de- tected by the front segment, while the rear seg- ment, which detects the energy range 3–150 keV only measures the orbital background. We used this fact to develop our background subtraction Fig. 13. Ratio of rear to front segment signals for the energy range 3–100 keV. method. During the satellite's night each segment measu- red signals coming from the orbital background. As we knew the relation between rear and front segment detection during this time, we were able to estimate the background level for each flare moment using rear segment counts. Our initial results were presented at the conference “Pro- gress on spectroscopy and imaging III”. Speci- fically, for the flare observed on 8 September 2009, we determined the flux ratio between rear and front segments based on signals from detec- tors numbered 4, 6, 8 and 9 (Figure 13). Figures 14 and 15 show the results of our backg- round estimation. In a second step, we ran a basic Fig. 14. Change in flux over time for a flare (red line) and analysis in OSPEX software. In this case, the ana- estimated background (blue line). lysis was run for the same flare, but with the back- ground subtracted, using the pre-flare average value. Although the results were similar, we found that the background estimated from the rear segment was more reliable. In the next phase of our work, we will calculate the background for all 36 weak flares observed by both SphinX and RHESSI. Flares will be analysed for each detector separately, to avoid any distortion due to the cha- racteristics of the detector – this will also increase the precision of the method. We plan to deter- mine physical parameters for each event, for both RHESSI and SphinX data, and compare results. This will be the continuation of our work des- cribed in the paper Solar Microflares Observed by Fig. 15. Spectrum of the 8 September 2009 flare (red line) and background estimated from the rear segment SphinX and RHESSI. (blue line).

(M. Litwicka, T. Mrozek)

51 Basic research on coronal and photospheric activity during the SphinX mission In 2019, we continued our comparison of solar ges were used for this purpose. Our initial results photospheric and coronal activity. Images from indicate that stronger coronal activity can develop the X-Ray telescope, operating on the Hinode sa- without any sign of increased activity in the pho- tellite, measurements from the Polish Solar Pho- tosphere. tometer in X-rays (SphinX), Debrecen Photohe- (Sz. Gburek) liographic Data catalogue and SOHO/MDI ima- The Bent Crystal Spectrometer archive, catalogue and events In 2019, we continued working on a new version The BCS recorded millions of solar spectra. Un- of the catalogue of Bent Crystal Spectrometer fortunately, many are now unavailable. Our new (BCS) observations. The BCS, which flew aboard catalogue is based on existing bda data files that the Solar Maximum Mission satellite (1980–1989) are formatted to the Solar Soft standard and use was a unique instrument that observed X-ray solar new calculations of the instrument's effective spectra in the ranges 1.769–1.947 Å and 3.165– area. The catalogue is available online at http:// 3.231 Å with unprecedented temporal and spec- www.cbk.pan.wroc.pl/body/sbcs/catalogue/. tral resolution. New calculations of the instru- We examined observations from the first year of ment effective area (Rapley et al., 2017) have ma- the Mission (1980), when the maximum of the 21st de it possible to interpret recorded spectra much solar cycle occurred. In this year, the BCS obser- better than before. Thanks to this work, all availa- ved 110 flares, five of them in the X GOES class. ble archival observations can now be interpreted Two examples of flares registered by the BCS are (or re-interpreted) in order to fit theoretical spec- shown below. The most interesting events were tra, and determine flaring plasma temperatures, presented at the 2nd China–Europe Solar Physics emission measures, chemical composition (Ca & Meeting, CESPM 2019, held in Croatia. Fe), velocities and turbulent motions.

Fig. 16. Two examples of flares registered by the BCS. (A. Kępa, B. Sylwester, J. Sylwester)

52 RESIK: The application of the differential evolution algorithm to the analysis of X-ray spectra In 2019, we continued our work on applying the mental abundances. Our initial results, obtained differential evolution (DE) method to the analysis for the flare on 21 January 2003, confirmed that it of X-ray spectra. DE is a stochastic, evolutionary is possible to simultaneously determine the DEM algorithm used for global optimization. This distribution and the abundance of the most im- population-based algorithm, like other genetic portant elements contributing to the spectrum. algorithms, uses similar operators: crossover, mu- This approach has never been used before in spe- tation and selection. ctra analysis. We presented these initial results at a We evaluated the potential application of the DE seminar, and an article is currently being prepared. approach to the determination of differential emission measure (DEM) distributions. Our tests confirmed the stability of solutions, and its ability to reconstruct synthetic DEM distributions. The method was then applied to the analysis of RE- SIK spectra. We found that DEM distributions obtained using this method were very similar to those calculated using the Withbroe–Sylwester approach. For the 15 April 2002 flare, the obtai- ned DEM distributions were always two-compo- nent independent in the evolutionary phase. A small amount (the third component) of hotter plasma (25–30 MK) is seen at the beginning (rise and maximum) of this long-duration event. Based on the time coincidence with harder X-rays, this component may be attributed to the presence of suprathermal electrons. The results of the analysis were presented at the Fig. 17. Comparison of differential emission measure conference “Progress on spectroscopy and ima- distributions calculated for the decay phase of the flare on 21 January 2003 (max. 15:26 UT) obtained using the ging III” held in Wrocław, and published in Solar Withbroe–Sylwester approach (red) and the differential Physics in the article titled A Multiwavelength evolution (DE) method (blue). Analysis of the Long-duration Flare Observed on The DE method is used to obtain DEM distribu- 15 April 2002. tions simultaneously with abundances for selected We also studied the possible application of our elements contributing to RESIK spectra. The ob- method to the determination of coronal ele- tained abundance values differ from those ob- tained by other methods by only a few percent.

An analysis of RESIK and RHESSI observations for the 20 September 2002 flare We investigated the flare that occurred in the spectra to determine the distribution of non- southwest hemisphere in the active region NOAA thermal electrons involved in the flare process. 10126 (S23E69) on 20 September 2002. This flare Starting with RHESSI and SOHO EIT images, we was classified as an M1.8 GOES flare. The event estimated geometrical parameters of flaring lo- was observed by a few instruments, including the ops. Next, we added these non-thermal electrons SOHO/ EIT telescope, the RHESSI satellite and into the top of the observed loop where, in the the RESIK spectrometer. frame of a 1D-HD model, they fall, heat and eva- We compared the results of a plasma analysis ba- porate in the chromosphere, and fill the loop with sed on a hydrodynamic model (HD) of the flaring hot, dense plasma that glows in soft X-rays. Total loop with observations of spectra in the X-ray electron energy was controlled by comparison of range. We used observed, RHESSI hard X-ray observed and calculated fluxes in the 1–8 Å chan-

53 nel from GOES data. We determined the tempe- rature and density at each point in the flaring loop at all times during the flare, and calculated thermal spectra that should be observed. This found that RESIK spectra for the 20 September 2002 flare were consistent – within a factor of two – with ob- served spectra for most of the flare duration. This result is related to the cross-calibration of RESIK and RHESSI instruments.

Fig. 18. From top to bottom: X-ray fluxes recorded by GOES in the 0.5–4 Å and 1–8 Å energy bands (red and blue dashed lines) and GOES fluxes synthesized using the numerical model (red and blue solid lines); temperatures derived from GOES data (light-blue dashed line), GOES temperatures synthesized using the numerical model (dark-blue solid line) and average temperature from RESIK DEM distributions (black circle); emission measures derived from GOES data (light-blue dashed line), GOES emission measures synthesized using the numerical model (dark-blue solid line) and emission measures from RESIK DEMs (black circle).

Fig. 19. Plots of RHESSI and RESIK energy spectra for two time intervals during the analysed event.

(A. Kępa, M. Siarkowski, R. Falewicz)

54 Heliospheric physics (Laboratory for Solar System Physics and Astrophysics - LSSPA) The hypersonic, ionised solar wind carves out a sizes. This cloud is one of many similar clouds wi- cavity in the interstellar matter, called the helio- thin the Local Interstellar Medium-an astro- sphere. The size of the heliosphere is determined physical object spanning approximately 200 pc by a balance between the pressures of the solar across that is a remnant of a series of Supernova wind and the interstellar gas, both of which are explosions that happened a few million years ago. magnetised. The heliosphere is bounded by a The Sun moves through the Local Interstellar contact discontinuity layer called the heliopa- Cloud from right to left as shown in , emitting the use,which separates the solar wind and interstellar solar wind-an ever-evolving, omnidirectional, lati- plasmas. While the interstellar plasma is deflected tudinally-structured, hypersonic outflow of solar and flows past the heliopause, the neutral com- plasma. Subjected to the ram pressure of the ponent of interstellar matter, mainly hydrogen ambient interstellar matter, the solar wind slows and helium, penetrates freely into the heliosphere, down through a shock wave-the solar wind termi- where it can be directly observed. An artist's nation shock-and eventually flows downstream, impression of the heliosphere is shown in Fig. 20. forming a contact discontinuity surface called the The figure shows the Sun embedded in the local heliopause, which separates the solar and interstellar cloud of interstellar matter composed of ionised plasmas, and an elongated heliotail (bottom-left and neutral atoms, and dust grains of various corner of Fig.20). The heliopause, impenetra-

Fig. 20. 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.

55 ble for charged particles except for cosmic rays, is turbed plasma flow past the heliopause and the transparent for neutral atoms, which thus freely slightly perturbed interstellar neutral atoms. Some enter the heliosphere. Inside the heliosphere, the- of the atoms that are the product of this reaction se interstellar atoms become the seed population also enter the heliosphere, and are detected as the for energetic neutral atoms (ENAs). ENAs are so-called secondary population of neutral inter- formed everywhere in the heliosphere due to the stellar gas. Together with all the other populations charge exchange reaction between the ions from of neutral atoms, they provide an important local plasma and the neutral interstellar atoms. means for analysing the physical state of the dis- Once created, they travel with-out being ionised tant regions that they originated from. or absorbed at large distances, comparable to the During recent years, a very important insight into size of the heliosphere. the heliosphere, Local Interstellar Medium, and The charge exchange process operates both in the processes responsible for the coupling of these supersonic solar wind and in the inner heliosheath astrophysical objects was obtained based on ob- (centre-left in Fig. 20), i.e., in the region between servations by the NASA space probe Interstellar the termination shock and the heliopause. Some Boundary Explorer (IBEX). This mission was of the ENAs created in these regions freely escape developed and is being led by the Southwest Re- from the heliosphere and, due to eventual colli- search Institute in San Antonio, Texas under the sions, slightly modify the inflowing interstellar NASA Small Explorers program. It is managed by gas. Others run in the opposite direction and the Goddard Space Flight Center for the NASA reach detectors located in the Earth's orbit (in Fig. Science Mission Directorate in Washington, DC. 20, schematically drawn close to the Sun). The research facilitated by IBEX is carried out by Neutral atoms from the interstellar matter (whose the IBEX Science Team of researchers from the streamlines are marked by the short arrows in Fig. United States, Poland, Switzerland, Germany, and 20) typically have energies of between a few dozen Russia. CBK PAN has participated in the IBEX and about 150 eV. Due to interaction between the effort since the planning phase, at the Co- heliosphere and the interstellar medium, a distur- Investigator level. bed region called the outer heliosheath (the green In 2019, scientists from the Laboratory for Solar haze in the figure) is formed in front of the helio- System Physics and Astrophysics (LSSPA) carried sphere. In this region, the flows of interstellar out studies of various aspects of the heliosphere plasma and interstellar neutral gas decouple from and the surrounding interstellar medium. Our re- each other. This leads to the formation of another sults were reported in seventeen scientific papers, population of neutral atoms through charge published in international, peer-reviewed jo- exchange reactions between ions from the per- urnals. Some of these results are presented below.

Structure of the heliosphere revealed by the spectrum of energetic neutral atoms Energetic Neutral Atoms (ENAs) are an impor- stigated the hypothesis that these ENAs are tant tool for investigating the structure of the he- created by charge exchange of solar wind pickup liosphere and for diagnosing the enigmatic pro- ions that have been accelerated at the solar wind cesses of acceleration of charged particles in the termination shock, and subsequently advected heliospheric boundary region. Observations of with the plasma flow beyond the termination ENAs with energies below ~50 keV by the Cas- shock. sini space probe, performed at the Saturn orbit, The research team simulated a directional distri- showed that ENA fluxes from the upwind and bution of ENAs within a wide energy range, from downwind regions of the heliosphere are similar 3 to 88 keV, i.e., almost the entire energy range in strength. This led the authors of these obser- covered by available observations from IBEX, vations to hypothesise that the heliosphere is Cassini, and SOHO space probes (IBEX-Hi, bubble-like rather than comet-like (i.e., it has no INCA, and HSTOF instruments, respectively). extended tail). An international team of scientists, The calculation of ENA fluxes was performed led by A. Czechowski from the LSSPA inve- using a multi-tier simulation scheme. The global

56 structure of the plasma flow inside and outside the termination shock was obtained using MS- FLUKSS – one of the most sophisticated global heliosphere models currently available. The PUI flux at the termination shock was calculated using the Warsaw Test Particle Model (WTPM) to si- mulate the spatial distribution of ISN H filling the space between the Sun and the termination shock, forming the seed population for PUIs. The PUI flux at the termination shock was calculated based on this density distribution and the most recent version of the LSSPA model of ionisation factors Fig. 21. A model spectrum of ions used to simulate the observed ENA flux. The model has three components: in the heliosphere (developed by the LSSPA du- bulk solar wind (orange), pickup ions reflected off the ring the past decade, see below). termination shock (red), and pickup ions transmitted across the shock (blue). The three components add up to An essential element of the simulation was a make the total spectrum (purple). This spectrum agrees model of the acceleration of pickup ions at the very well with the spectrum of suprathermal ions termination shock. The research team applied a measured by the Voyager 2 spacecraft in the corresponding energy ranges. Note that the energy of the theory of acceleration developed several years reflected component is shown after energisation of these ago by one of the team members (Gary Zank ions and their resulting penetration of the termination from the University of Alabama, Huntsville, shock. Source: Czechowski et al., Ap. J. 888:1, 2020. USA) and his collaborators. In this theory, a frac- tion of the pickup ion population with energies below the electric potential threshold at the shock cannot penetrate this threshold and is reflected upstream of the solar wind. These ions are picked up and accelerated by the inflowing solar wind plasma, thus gaining energy. The reflection/ energisation cycle repeats until an ion has a suf- ficient energy to penetrate the potential threshold and enter the inner heliosheath. The energised ions are subsequently carried by the solar wind plasma in the inner heliosheath. While the kinetic energy of individual ions is large, the mean flow speed of their population is close to that of the bulk plasma, which leaves them enough time to exchange charge with ambient H atoms and pro- duce a sufficiently large amount of ENAs. The sequence of models used in the simulation drew upon the most-credible, currently-available values for relevant parameters obtained from observations. Equally important was adopting a proton spectrum just downstream of the termi- nation shock, which on the one hand was in agree- ment with solar wind measurements and the Zank Fig. 22. Model of ENA flux (solid lines) for four energy PUI acceleration theory, and on the other hand bands (top–bottom panels), compared with actual agreed with the Voyager LECP in situ measure- observations from IBEX-Hi (first), INCA (second and third), and HSTOF (fourth). The data are presented by ments of the ion spectrum and of the termination dots, and measurement uncertainties by error bars. There shock strength (Fig. 21). is relatively little difference between simulations performed separately for a maximum and a minimum of solar activity (red and black lines, respectively). Source: Czechowski et al., Ap. J. 888:1, 2020.

57 This successful reproduction of the observed flux distribution and spectrum by a simulation using a model of the heliosphere with a long tail strongly suggests that there is no need to deviate from the classical paradigm of the heliosphere. In other words, the heliosphere is not round! The results of this work by the team led by Dr A. Czechowski from LSSPA, including Dr M. Bzow- ski, Dr J. M. Sokół, Ms M. A. Kubiak, and Ms J. Grygorczuk from the LSSPA, and researchers from Princeton University, the University of Ala- bama in Huntsville, the University of New Hamp- Fig. 23. Spectra of ENAs for the upwind (red) and downwind (blue) regions of the heliosphere, obtained shire, and the Max Planck Institute for Solar Sys- from observations (points with bars) compared with the tem Research were published in The Astrophysi- corresponding spectra obtained from simulations cal Journal 888:1, 2020, in a paper by Czechowski (diamonds). Horizontal bars mark the energy bands of the respective energy channels. Vertical bars represent et al. (https://doi.org/10.3847/1538-4357/ab 5b uncertainties in observations. Source: Czechowski et al., 14). Ap. J. 888:1, 2020. (A. Czechowski, M. Bzowski)

Density of interstellar He+ ions and the ionisation state of the Very Local Interstellar Medium The physical state of the interstellar medium sur- the magnetised interstellar plasma. Interstellar rounding the Sun is the subject of extensive re- neutral atoms mediate the interaction via charge search. The Sun is penetrating a cloud of warm, exchange. The interstellar plasma is composed partly ionised gas, but the ionisation state, tempe- mostly of protons and He+ ions. While the num- rature, and other physical parameters of this ber abundance of He+ ions in the plasma is on the cloud are believed to be controlled to a large order of 10%, its contribution to the plasma ram extent by ambient EUV radiation emitted by pressure acting on the heliosphere is fourfold several relatively nearby stars that are very bright bigger, because He+ ions are fourfold heavier than in this spectral region. Differential absorption, protons. Therefore, determining the absolute and the resulting ionisation of various ions of density of He+ ions in the unperturbed interstellar interstellar species and heating of interstellar medium is important for heliospheric studies. matter by radiation from these stars make it However, up to now it has proved challenging challenging to determine the physical state of because of the lack of available observables. interstellar matter near the Sun. The ionisation The flow of neutral interstellar helium through state and mean density of interstellar neutral and the perturbed interstellar plasma in the outer ionised components can be approximately de- heliosheath (OHS) results in the creation of a termined by averaging over lines of sight to secondary population of interstellar He atoms, nearby stars, i.e., on spatial scales exceeding the the so-called Warm Breeze, which is due to charge size of the heliosphere by many orders of ma- + exchange with perturbed He ions. This secondary gnitude. However, to understand the interaction population brings an imprint of the OHS con- of the solar wind with the interstellar medium, an ditions to the IBEX-Lo instrument, and was di- understanding of the local interstellar conditions, scovered in 2010 by a research team led by CBK within several thousand au from the Sun is PAN scientists M. Bzowski and M. A. Kubiak. necessary. This insight was discovered in 2019 by an international team of researchers led by Dr M. In 2019, an international team of researchers led Bzowski from the LSSPA. by Dr M. Bzowski, including Ms M. A. Kubiak, Dr J. M. Sokół, Dr A. Czechowski and Ms J. Grygor- The heliosphere is created as a result of a pressure czuk from the LSSPA determined the number balance between the magnetised solar wind and

58 density of the interstellar He+ population in the gree of H was found to be equal to 0.26 and that unperturbed interstellar medium in front of the of He to 0.37. These conclusions agree with Sun. This finding was based on IBEX-Lo obser- estimates of the parameters of the Very Local vations (for the years 2010–2014) of neutral He Interstellar Matter obtained from fitting observed atoms fitted using a global simulation of the spectra of diffuse interstellar EUV and the soft X- heliosphere, and a detailed kinetic simulation of ray background. the filtration of He in the OHS. This density was These results were published in The Astrophy- found to be (8.98±0.12) ×10- 3 cm- 3. From this, sical Journal, in a paper by Bzowski et al. (Ap. J. they obtained the absolute density of interstellar 882:60, 2019, https://doi.org/10.3847/1538- H+ as 5.4×10- 2 cm- 3 and that of electrons as 4357/ab3462). 6.3×10- 2 cm- 3. Consequently, the ionisation de- (M. Bzowski)

Interstellar neutral gas species and their pickup ions inside the heliospheric termination shock The expected distribution of interstellar neutral heliosphere. The team focused on modulations (ISN) gas and PUI density of H, He, Ne, and O with heliocentric distance, heliolatitude and time inside the heliosphere has been revised. Dr over the last three solar cycles. Three reactions: Justyna M. Sokół and Dr Maciej Bzowski from the charge exchange with solar wind particles (pro- LSSPA, together with Dr Munetoshi Tokumaru tons and alpha particles), photoionisation, and (ISEE, Nagoya, Japan) overviewed the current electron impact ionisation were considered. Simi- state of knowledge about solar ionisation rates for larities and differences between ionisation pro- heliospheric atoms inside the termination shock. cesses for the given species, as well as a compa- They compiled a list of ionisation processes rison of the total ionisation rates between the four relevant for the ISN H, O, Ne, and He inside the species in the ecliptic plane and in the polar

Fig. 24. Time series of ionisation rates of neutral hydrogen, oxygen, neon and helium at 1 au in the ecliptic plane, presented for the time interval 1985–2019, with a time resolution corresponding to the solar rotation period (upper row). Red corresponds to the total ionisation rate, which is a sum of the rates of charge exchange (grey), photoionisation (dark blue), and electron impact ionisation (pale blue). The lower row presents the percentage contribution of the three reaction rates to total rates for the four species, and its variation with time. Source: Sokół et al., Ap. J. 872:57, 2019.

59 regions were presented. The ionisation rates were source, depending on the phase of solar activity considered within a consistent and homogeneous and long-term changes in the solar wind. Total system of calculation, based on multi-source data ionisation rates are highest outside the ecliptic from direct and indirect measurements of the plane for O. Solar ionising factors act differently solar wind and the solar EUV flux. on different heliospheric particles, which results The study showed that ionisation at 1 au is the in different modulation of these particles thro- strongest for H and O and, thus, the resulting ughout the heliosphere. Total ionisation rates for modulation of the H and O fluxes of heliospheric He and Ne vary in time with solar activity, whereas particles is expected to be strongest. Modulation the rates for H and O follow variation in the cyclic due to solar factors is weakest for He – it is almost solar wind outside the ecliptic plane, and aperiodic an order of magnitude smaller than that for H and variations within it. This has important conse- O at 1 au in the ecliptic plane. For He and Ne, the quences for the study of heliospheric particles main source of ionisation losses is photoioni- such as ISN gas, PUIs and ENAs, as well as phy- sation. Consequently, modulation for these sical processes in the inner and outer heliosphere. species is well correlated with variation in the solar These results were presented in a paper by J.M. activity. ISN H atoms are prone to solar wind Sokół, M. Bzowski and M. Tokumaru published variations both in time and in latitude. In the case in The Astrophysical Journal 872:57, 2019 of ISN O, both charge exchange and photo- (https://doi.org/0.3847/1538-4357/aafdaf). ionisation losses can be a dominant ionisation

Fig. 25. The density distribution of H+ pickup ions in the ecliptic plane is shown as a background for the locations of the maximum pickup ion densities of H+ (black), He+ (orange), Ne+ (blue), and O+ (green) in 1996 (full circles) and 2001 (empty circles). The upwind direction is shown on the right-hand side. For comparison, orbits of Venus, Earth, Mars, and Jupiter are shown as broken lines. Also shown are portions of the trajectories of selected spacecraft: Ulysses, Voyagers 1 and 2, New Horizons, and Cassini. The boundary of the cavity in the density distribution of ISN H in 1996 is marked by the grey dotted line. The yellow dotted line marks a region where the He+ PUI density exceeds by a factor of 50 the upwind density of He+ at the termination shock. Source: Sokół et al., Ap. J. 879:24, 2019.

60 These revised solar ionisation rates were used by solar minimum detection is optimal at 1 au, while scientists from the LSSPA (Dr J. M. Sokół, Dr M. during the solar maximum the peak is shifted Bzowski, and Ms M. A. Kubiak) to study the almost to Jupiter's orbit, with a density reduction spatial distribution of ISN gas density for H, He, of over 50%. Although O+ PUIs can be searched Ne, and O and the PUI density for H+, He+, Ne+, for in both upwind and downwind regions (as and O+ in the region between 1 au and the intensities are expected to be similar), acceptable termination shock of the solar wind, both in and locations are found at distances starting from the out of the ecliptic plane, during minimum and Jupiter orbit, up to a few tens of au. The upwind maximum solar activity. The study focused on hemisphere is confirmed as the best location to similarities and differences in the large-scale detect H+ PUIs. structures of ISN gas and PUI densities between The research team identified the location of the various species that formed in the heliosphere. cavity in ISN gas density for the four species, and These results show that different species have variation of the size and shape of the cavity with different ISN and PUI density structures. This is time. The greatest cavity is expected for ISN H, due to differences in modulation by solar ionising while the smallest cavity is expected for ISN He. factors, even though the inflow direction, speed The study also discussed relative abundance ratios and temperature of these species are identical of Ne/O, H/He, Ne/He, and O/He for ISN gas (except for H). The latitudinal anisotropy of the and PUIs densities, together with their variation ionisation rates causes anisotropy in ISN gas and with location in the heliosphere, and their PUI densities measured along the ecliptic plane. modulation along the TS. For relative abundance Because this anisotropy is different for different ratios of ISN gas densities of the species in species, relative abundance ratios of ISN and PUI question, the distribution at the TS is uniform up densities vary non-uniformly in space and time. to about 40° off the downwind direction, where The study, performed for the first time for a an increase in the ab solute density is expected. homogeneous system of ionisation rates for the For PUIs, the variation at the TS is not uniform in species in question, showed that while the ISN time and is a function of the angle off the upwind- density maxima are expected outside 1 au, the PUI downwind axis and heliolatitude; it also varies density maxima are expected to be found closer to with the phase of solar activity. the Sun. The PUI densities, throughout the These results were presented in a paper by Sokół heliosphere, are expected to be highest for He+ et al. published in The Astrophysical Journal PUIs, then H+ PUIs, Ne+, and O+ PUIs. The 879:20, 2019 (https://doi.org/10.3847/1538- optimal location for the detection of He+ PUIs is 4357/ab21c4). downwind, within 1 au. For Ne+ PUIs, during the (J. M. Sokół) Science opportunities from observations of interstellar neutral gas with an adjustable detector boresight direction The interstellar neutral (ISN) gas that has entered ration of this mission. In particular, Dr M. Bzow- the heliosphere can be detected at a few au from ski, Dr J. M. Sokół, and Ms M. A. Kubiak are Co- the Sun, as demonstrated by Ulysses and the Investigators in the IMAP Science Team. During Interstellar Boundary Explorer (IBEX) space 2019, LSSPA scientists were deeply involved in probes. Ulysses observed the ISN gas from a set the science development of the IMAP-Lo instru- of vantage points distributed along its solar polar ment, which draws its heritage from the IBEX-Lo orbit from 1994 to 2007, while IBEX has been detector. One of the significant improvements in observing from the Earth's orbit in an almost this new instrument will be an ability to vary the fixed direction relative to the Sun since 2009. A angle of the boresight relative to the Sun. This follow-on mission for IBEX will be NASA's capability will enable IMAP-Lo to track ISN flux Interstellar Mapping and Acceleration Probe in the sky during almost the entire year and, con- (IMAP), which will be launched in 2024. Resear- sequently, significantly lengthen the observation chers from the LSSPA are involved in the prepa- time.

61 Fig. 26. Graphic representation of science opportunities for a study of the local interstellar medium by direct sampling of interstellar neural H, He, Ne, O, and D using a scanning instrument located at the Earth's orbit that is able to vary the angle between the Sun and the instrument boresight. This configuration is similar to that planned for the IMAP-Lo experiment. Source: Sokół et al., Ap. J. S. 245:26, 2019. A team of LSSPA scientists (J. M. Sokół, M. A. Kubiak, M. Bzowski) in collaboration with the IMAP-Lo Lead Professor N. Schwadron and Professor E. Möbius from the University of New Hampshire studied Fig. 27. Timeline for science opportunities stemming the science opportunities afforded by this new from the ability to adjust the boresight in the planned capability. This study identified alternative advan- IMAP-Lo experiment (lower panel). Alternative schedules tageous ISN gas observation geometries for the are presented in the upper panel. The ?FOV angle is the angle between the spacecraft's rotation axis, directed detector moving along the Earth orbit over the towards the Sun, and the boresight of the mounted course of a year, and suggested a multi-choice, an- instrument. Source: Sokół et al., Ap.J.S. 245:26, 2019. nual ISN observation scheme. Science opportu- nities provided by these alternative schemes were metries, primary and secondary populations can identified as a function of time of year and phase be fully separated. Additionally, they showed that of solar activity. Observation geometries and atoms of ISN gas on indirect trajectories can be seasons were determined separately for various detected, and pointed out the impact of this ISN species and populations. capability on the study of ionisation rates of ISN species. The researchers found that using an adjustable viewing direction allows to perform sampling The results of this study, which may be regarded ISN gas in the upwind hemisphere, where the as a yearly observation plan for such an experi- signal is not distorted by gravitational focusing. ment, were published in a paper by Sokół et al. in However, ISN species can be sampled almost The Astrophysical Journal Supplement Series 245:26, throughout the year, which enables improving the 2019 (https://doi.org/10.3847/1538-4357/ observation statistics. They demonstrated that ab21c4). with appropriately-adjusted observation geo- (M. Bzowski)

A “forgotten” population of neutral gas inside the heliosphere Interstellar neutral H penetrates the heliopause pickup ions and the heliospheric backscatter glow. and continues its flow towards the Sun. On the The globally distributed flux (GDF) of ENAs, way, it is strongly depleted inside the termination created by charge exchange in the inner helio- shock. Nevertheless, fractions of both primary sheath, has been sampled directly by the Inter- and secondary populations of this gas reach the stellar Boundary Explorer for almost a full cycle Earth's orbit. In these regions of the heliosphere, of the solar activity. Usually, these ENAs are trea- ISN H is the source population for interstellar

62 ted as test particles bringing information on remo-te regions of the heliosphere. However, in fact, these atoms form a separate non-thermal popula-tion of neutral H atoms deep inside the helio-sphere. The energy spectrum of ENAs measured by IBEX is approximately described by a power law function, i.e., partial densities of atoms with energies corresponding to increasing energy channels of IBEX detectors rapidly decrease. Therefore, to assess the total density of ENAs at the Earth orbit, it is sufficient to analyse observa- tions from the low-energy part of the spectrum, observed by the IBEX-Lo detector. Based on available measurements from IBEX-Lo, Dr M. Bzowski from the LSSPA and Dr A. Galli from Bern University, Switzerland, calculated the number density of the GDF ENA population at the Earth's orbit. They found that this density is between 10- 4 and 10- 3 cm- 3, i.e., comparable in magnitude to the density of ISN H in the down- wind portion of the Earth's orbit. Half of this atom population has energies less than ~80 eV. Fig. 28. Partial densities of H ENAs observed by IBEX- Consequently, this GDF population of neutral Lo in its eight energy steps (upper panel) and a plot of hydrogen is likely to provide a significant contri- cumulative density of the H ENA population from bution to the intensity of heliospheric glow in the highest to lowest energies (lower panel). Densities are marked with a black line, and their uncertainties by grey downwind hemisphere. It may also be the seed shading. Most of the atoms forming the ENA population population for the ambiguous inner source of at 1 au from the Sun have energies less than 0.1 keV. hydrogen pickup ions, and may be responsible for Consequently, their speeds relative to the Sun are the excess production of pickup ions found in the sufficiently low to locate their Doppler shifts inside the analysis of magnetic wave events induced by the spectral range of the solar Lyman-α line. Hence, these atoms are illuminated by solar Lyman-α radiation, which proton pickup process in the downwind region 1 they re-emit by the fluorescence mechanism. This ENA au from the Sun, which was discovered in 2018 by glow is one of the components of the Lyman-α helioglow a research team that included scientists from the observed from Earth-orbiting spacecraft. Source: Bzowski LSSPA. & Galli, Ap. J. 870:58, 2019. Fig. 29. Comparison of mean ENA density at 1 au (the thick orange line) with the density distribution of ISN H along the Earth orbit, simulated using the WTPM model for four dates in the solar activity cycle. While in the upwind portion of the Earth orbit (ecliptic longitudes 165–345°) the ENA density is lower than the ISN density by almost an order of magnitude during all phases of the solar cycle, in the downwind hemisphere they become comparable and, in certain years, ENA density may exceed that of ISN H gas. Source: Bzowski & Galli, Ap. J. 870:58, 2019.

63 The uncertainty of this density is high, and the deserve further analysis. These results were pu- spatial distribution of GDF ENAs density re- blished in The Astrophysical Journal in a paper by mains to be established. However, the analysis Bzowski & Galli (870:58, 2019, https://doi.org/ performed by Bzowski and Galli clearly suggests 10.3847/ 1538-4357/aaf1b2). that GDF ENAs, treated as a gas population, (M. Bzowski)

Uncertainty of the cross section for charge exchange in the outer heliosheath Models play an important role in our under- standing of the global structure of the solar wind and its interaction with the interstellar medium. A critical ingredient in many types of models is the charge-exchange collisions between ions and neu- trals. Some ambiguity exists in the charge-ex- change cross-section for protons and hydrogen atoms, depending on which experimental data is used. The differences are greatest at low energies and, for the plasma-neutral interaction in the outer heliosheath, may exceed 50% (Fig. 30). The charge-exchange cross-section is important because it directly affects the intensity of coupling between neutral gas and plasma in the outer helio- sheath. A larger cross-section implies stronger heating and a slowdown of the plasma, on the one hand, and more intense production of the secon- dary H component and attenuation of the pri- mary component, on the other hand. A smaller Fig. 30. Measurements of the charge-exchange cross- section between protons and H atoms shown as a cross-section implies weaker mass-loading of the function of the kinetic energy of particle collision (black plasma, less intense production of the secondary dots), compared with various model formulae. The component, and a different ratio between thermal selected measurement data were chosen based on a review of the literature. Three models are in a very good and ram pressures in the plasma. agreement with the selected dataset, while two others are Dr M. Bzowski from the LSSPA and Dr J. not. Model LS05 agrees with a different subset of experimental data (not shown) and has been widely used Heerikhuisen from the University of Waikato, in the modelling of the heliosphere, becoming a de facto New Zealand, assessed a number of existing standard. It seems, however, that it is not appropriate in datasets and formulae for proton–hydrogen the context of the outer heliosheath. Source: Bzowski & charge-exchange. They used a global simulation Heerikhuisen, Ap. J. 888:24, 2020. of the heliosphere to quantify differences bet- ween the currently-favoured cross-section (the

Fig. 31. Comparison of density profiles of neutral H in model heliospheres, simulated assuming two alternative cross-sections for charge exchange (LS05 vs Ba90), and different densities of interstellar plasma. Simulations based on identical plasma densities and different cross- sections are shown by green and blue lines. The purple line corresponds to the case where the preferred cross- section (Ba90) was used, and the density of interstellar plasma was adjusted. This figure illustrates the level of uncertainty in the model's results (or, in other words, the model's sensitivity) to the magnitude of the adopted charge-exchange cross-section. Source: Bzowski & Heerikhuisen, Ap. J. 888:24, 2020.

64 green line in Figure 30) and suggested a formula report. They found that in order to make the for the charge-exchange cross-section that most resulting two model heliospheres the same size, closely matches the majority of available data. interstellar proton and hydrogen densities needed The two researchers also sought to identify uncer- to be adjusted by 10%–15% (Figure 31). This tainty in the model of the heliosphere stemming observation provides a way to link uncertainty in from different cross-section models. To do this, the cross-section to uncertainty in the parameters they performed simulations of the heliosphere of the pristine interstellar plasma. that only differed with respect to the adopted This study was reported in a paper by Bzowski & cross-section. They used the same model of the Heerikhuisen published in The Astrophysical Journal heliosphere that was used in the determination of (888:24, https:// doi.org/10.3847/1538-4357/ the density of interstellar He+, presented in this ab595a).

Distribution function of neutral helium in the heliospheric boundary region Interactions between the solar wind and inter- solutions of the production and loss equations for stellar matter involve, among other processes, secondary atoms due to charge-exchange colli- charge exchange between interstellar neutral sions in the outer heliosheath. This simulation atoms and plasma, which results in the creation of method was developed by the LSSPA in 2017, and a secondary population of interstellar neutral has been successfully used in the determination (ISN) atoms. These secondary atoms are former of He+ density in the very local interstellar me- interstellar ions from the perturbed plasma, dium (these results are presented in this report). flowing around the heliosphere. They inherit the Results of the simulation, performed using the kinematic parameters of their parent ions and aforementioned secondary population synthesis move freely across large distances as they are no method, are shown in Figure 32. The intensity of longer tied to the plasma by electromagnetic the secondary population increases when going forces. from the outside to the inside of the outer The secondary population of interstellar helium heliosheath. A left-right asymmetry of the secon- was detected by IBEX. However, the interpre- dary population appears approximately 300 au tation of these measurements was mostly based from the Sun and attains maximum magnitude on an approximation which assumed that in the between 200 and 115 au, where production of the outer heliosheath, the primary interstellar neutral secondary population is most intense. Moving atoms and the secondary atoms form two non- closer to the Sun, inside the heliopause, the interacting homogeneous Maxwell–Boltzmann distribution function narrows but maintains a populations. Although this approximation is certain level of asymmetry, which is a signature of incorrect from the fundamental viewpoint, it was the presence of the secondary population in the able to explain observations with surprising sample. At 1 au, the only remaining asymmetry is fidelity. LSSPA scientists M. A. Kubiak, M. at the fringe of the distribution function, in Bzowski and J. M. Sokół investigated this appa- qualitative agreement with IBEX observations. rent contradiction and sought to understand the These results were compared with those obtained distribution function of interstellar neutral he- using the approximation of two Maxwell– lium in the boundary region of the heliosphere, Boltzmann populations. The researchers found based on information about the physical state of that the two-Maxwellian approximation for the interstellar matter in this region. distribution function of neutral He is poor within The researchers adopted the global model of the the outer heliosheath, but reasonable inside the heliosphere used in the study of He+ density in the termination shock. This is due to a strong sele- VLISM, and simulated the distribution function ction effect: He atoms able to penetrate the termi- in the outer heliosheath and inside the heliopause nation shock are a small, peculiar subset of the using the method of characteristics. The statistical entire secondary He population. Nevertheless, weights used in this method were obtained from the two-Maxwellian approximation is a good

65 Fig. 32. Maps of the full distribution function of neutral He obtained from simulations for locations distributed along the direction of the Sun's motion through the interstellar medium (i.e., along the so-called upwind line). It starts from 700 au and 300 au, where the He population consists almost solely of primary interstellar atoms, runs through 200, 150 and 115 au, where the production of secondary atoms is most intense, ending at 100, 10 and 1 au from the Sun, where there is no secondary atom production and an increasing effect of ballistic selection is visible. The reference frame is based on the so-called B-V frame. The horizontal axis is the angle off the upwind direction along the plane defined by the upwind direction and the direction of the vector of the unperturbed interstellar magnetic field (the B-V plane). The vertical axis is the elevation angle with respect to this plane. This figure shows full distribution functions of neutral He, integrated over atom speeds and normalised to the peak value at 1000 au. Unperturbed interstellar atoms flow in from the centres of the panels and are represented by yellow disks. Secondary atoms are represented in blue and white. Source: Kubiak et al., Ap. J. 882:114, 2019. reproduction of the density distribution of ISN representative of those of the secondary popula- He inside the termination shock, and provides a tion in the region where it is produced, or for the realistic reproduction of the orientation of the plasma in this region. plane defined by the Sun's velocity vector through These conclusions were published in The Astro- the local interstellar matter and the vector of the physical Journal in a paper by Kubiak et al. (882: 114, unperturbed interstellar magnetic field. Its tempe- 2019, https://doi.org/ 10.3847/1538-4357/ rature and velocity parameters, however, are not ab3462). (M. Bzowski)

66 Trajectories of dust particles around stars The motivation for this work was observations of rotating star, the outer limit of the trapping region excessive infrared emission in the vicinity of some contracts, consequently, the hypothetical trapped stars. One proposed explanation is that the emis- dust would have to survive the extreme conditions sion comes from small dust grains trapped by the inside the stellar corona. These theoretical sug- stellar magnetic field. In the case of the Sun, trap- gestions were confirmed by numerical calcula- ped small dust particles (ranging from a few to a tions performed using simplified models of the few ten nm) was theoretically predicted by A. stellar wind and the magnetic field for Vega and Czechowski from the LSSPA and I. Mann. Fomalhaut. These conclusions were published in In 2019, this hypothesis was tested. An interna- a paper by Stamm et al. in Astronomy & Astro- tional team of researchers, including A. Czecho- physics (626, A107, 2019, https://doi.org/ 10. wski, applied the theory to the cases of Vega and 1051/0004-6361/201834727). Fomalhaut. Vega and Fomalhaut are young, hot An additional chapter in this paper discusses the stars of the A spectral type, with high rotation effect of corotation of the coronal plasma (not rates (20–40 times faster than that of the Sun). included in earlier models developed by Cze- Theoretical arguments put forward by Czechow- chowski and Mann) on the process of nanodust ski and Mann imply that trapping of nanodust trapping. The conclusion is that including plasma grains around these stars is unlikely, for two corotation in dust trajectory simulations does not reasons. First, for a hot star, the high radiation affect trapping, provided that the magnetic field pressure acting on dust grains overcomes the gra- and the plasma flow satisfy freezing-in equations. vity force. Consequently, the attractive force, This observation lends credence to earlier con- which is necessary for trapping, is absent and dust clusions. grains cannot be trapped. Second, for a rapidly (A. Czechowski)

Studies of the intermittent nature of the turbulence in magnetospheric plasma and solar wind out of the ecliptic plane

The solar wind is considered as a natural plasma decreased efficiency of intermittency drivers with laboratory to study turbulence and its intermittent distance from the Sun. Additionally, the analysis nature. One approach uses the multifractal forma- showed that the greatest differences between lism, which is a generalisation of the fractal descri- magnetic field components are found close to the ption and allows us to classify processes and data Sun, where intermittency is the strongest. More- with a high level of heterogeneity. over, it was observed that the slow solar wind Dr Anna Wawrzaszek from the LSSPA, in coo- during the maximum of solar cycle 23 has a lower peration with scientists from Belgium and Italy level of multifractality (intermittency) than the conducted a multifractal analysis of magnetic fast solar wind, which can be related to the idea of field measurements obtained by the Ulysses space the existence of a new type of Alfvénic slow solar probe during two solar minima (1997–1998, 20 wind. 07–2008) and one solar maximum (1999–2001), These results were published in The Astrophysical separately within the fast and slow solar wind Journal in a paper by Wawrzaszek et al. (876:153, regimes. These studies were based on a much 2019, https://doi.org//10.3847/1538-4357/ larger number of cases than previous research, ab1750). and showed that outside the ecliptic plane, the To better understand the process of hydroma- degree of multifractality/ intermittency slowly gnetic convection in space plasma, Dr Anna Waw- decreases with distance from the Sun (regardless rzaszek and a PhD student, Ms Agata Krasińska, of the component or reference system). The performed systematic studies of the dynamics of researchers concluded that this radial dependence a four-dimensional generalised Lorenz system. may be explained by the slower evolution of This model, which was proposed in 2010 by other turbulence outside the ecliptic plane, and the scientists from the LSSPA (W. Macek and M.

67 Strumik), was supplemented by a fourth variable that magnetic field control parameters signifi- that described the profile of the magnetic field cantly influence the linear stability regime of the induced in a convected magnetised fluid. Analy- generalised Lorenz model. Moreover, the study tical and numerical analyses of this system were showed the existence of several windows of non- performed in 2019. chaotic variation (windows of order). In parti- They revealed several types of dynamical states, cular, period-3 windows were observed, at the including nondegenerate and subcritical Hopf edge of which the researchers identified new cases bifurcation, and forward and backward bifur- of type I intermittency. cation structures (tangent, pitchfork, period-dou- These results were published in a paper in the bling). Moreover, they determined an analytic International Journal of Bifurcation and Chaos (29 No formula for control parameters at which Hopf 14, 1920042, 2019, https://doi.org/10.1142/S0 bifurcation exists. This advance makes it possible 218127419300428). to control the linear stability of the considered (A. Wawrzaszek) system. In particular, the two researchers found

Ionospheric and magnetospheric group (Plasma Physics Group) Comparison of the Disturbances in the Ionosphere Registered by DEMETER and Swarm Satellites during Geoma- gnetic and Thunderstorms Lightnings and particularly TLEs (sprites, jets, elves, halos) are associated with the electro- magnetic connections and interactions between atmosphere, ionosphere and magnetosphere and with strong thunderstorm activity. The geoma- gnetic storms are known as a source of strong disturbances in the ionosphere. Analysis of the data from DEMETER and Swarm shown some similarities and diferencies between effects of both types of events. Fig. 37 shows dynamical spectra of the magnetic field and electron density variations on March 26 2016 registered during flight over African center of the thunderstorm. The diamonds indicate time of strong strokes registered by WWLM system. Similarities: Presence of energetic electrons. Strong variations of the electron density and tem- perature, Turbulence seen in the electric and magnetic fields as well as in plasma parameters. Differences: Globality vs. Locality.

Fig. 33. Configuration of DEMETER satellite and 3 satellites creating Swarm mission. (courtesy of ESA).

68 Fig. 34. Magnetic storm November 2004.

Fig. 35. Disturbances in the ionosphere registered by DEMETER during main phase of geomagnetic storm.

Fig. 36. Registrations of the HF emissions associated with fluxes of energetic electrons in the ionosphere during thunderstorm.

69 Fig. 37. Location of tracks and lightnings for a thunderstorm in Africa on March 26, 2016.

Fig. 38. Dynamical spectrograms (δB - top panel, δNe – bottom panel) for selected passes of Swarm A over active African thunderstorm center. (J. Błęcki, J. Słomiński, R. Wronowski, E. Słomińska, R. Iwański, M. Parrot, R. Haagmans)

70 Connections between electromagnetic signals generated by Mesoscale Convective Systems, observed by an ELF ground station and DEMETER satellite In recent days intensified thunderstorm activity in Europe is observed, both for the number of ap- pearances and intensity. It is especially visible in summer time, when there is an advection of warm maritime air from west. The advection of air mas- ses is enriched by water vapour, which source can be found over the Mediterranean Sea. In propi- tious atmospheric conditions, thus mentioned above thermal conditions and significant convec- tion, atmospheric instability or strong vertical thermal gradient lead to the development of strong thunderstorm systems. In this paper, Mesoscale Convective Systems (MCS) (Bonner 1968, Banta i in. 2002, Houze 2014), cases are discussed it is believed that they belong to the strongest storm phenomena that have been ever registered on Earth. Their genesis can be found in Fig. 39a. Composite radar map of Poland during strong developed Cumulonimbus clouds, which development of the Mesoscale Convection system on 2 23rd of July 2009. may cover up an area above 100 000 km . MCSs are able to generate strong atmospheric dischar- meters are responsible for positive verification of ges or significant precipitation of rain and/or hail. this phenomenon. CAPPI belongs to this para- (Chomicz, 1951) and significant wind blows, meters - cloud reflectivity. This product is based often exceeding 150 km/h. Identification of the on satellite data in IR spectrum (Maddox, 1980), MCS is a complex process, due to many variables, atmospheric soundings or measurements from which have to be taken into account. These para- PERUN system based on detectors in VHF range

Fig. 39b. Spectrograms of the magnetic (upper panels ) and electric (bottom panels) fields in VLF range. Both figures contain 1sec interval of measurements and correspond to 20:05:33- 20:05:34 UT.

71 (Very High Frequencies 113.5 – 114.5 Hz). Men- ween DEMETER flybys and measurements from tioned tools allowed to identify two MCSs, that the ELF (Extremely Low Frequencies) Hylaty had happened in Poland in 23th of July 2009 and station, placed in Bieszczady mountains (Kulak et 24th of May 2010. We would like to emphasise, al., 2014). that selection of these cases is not random. Both (J. Błęcki, K. Martyński, A. Kulak, J. Młynarczyk, of them were designated due to correlation bet- R. Wronowski, R. Iwański)

Interaction of an interplanetary shock wave with the solar wind Among the physical processes in the solar wind parameters: particle flow velocities, pressure, and (SW) plasma, the processes that take place in the the accompanying magnetic field in the vicinity of vicinity of the front of the interplanetary shock the front have been derived for both models. Two wave, and on the front itself are of particular important facts have been established in the interest. In 2029, we prepared a paper that presen- interaction of the solar wind with a shock wave. ted an analytical description of such processes, The magnetic energy of the shock front is based on the solution of a system of nonlinear absorbed by the solar wind and increases its speed. equations of magnetohydrodynamics in a thin In the case of model II, this process is much more layer surrounding the front of the interplanetary intensive than with model I. The kinetic energy of shock wave and the use of Rankine-Hugoniot the shock front, in the case of model I, on the conditions in the frontal zone. We considered two contrary, takes energy from the solar wind, which shock waves models: one that does not takes into leads to a decrease of the velocity of the solar account the thickness of the front (the surface of wind particles. For model II, this effect is discontinuity), and another that take into account practically absent. These results of this work are its finite thickness and fine structure. The influ- analytically proven and evaluated quantitatively. ence of both models on the solar wind parameters The article has been submitted for publication in are compared with each other. Explicit formulas the Journal of Atmospheric and Solar-Terrestrial describing the changes of the main solar wind Physics. (I. A. Molotkov and B. Atamaniuk)

Current activities related to the Polish LOFAR PL610 station and LOFAR data studies The LOFAR interferometer is an international infrastructure designed by the Dutch institute AS- TRON. It consists of 51 stations situated across Europe. One of the three Polish LOFAR stations, PL610 located at Borówiec, belongs to the Cen- trum Badań Kosmicznych PAN. The infrastru- cture has been operating since 2015 with a obser- vation schedule divided between working in inter- ferometric mode (as part of the International LOFAR Telescope) and working in local mode, where it operates as a single instrument (inter- national station owners are guaranteed about 10% of annual observing time for local mode observ- ations). During this time, station PL610 observa- dedicated software developed by CBK PAN tions are mainly focused on monitoring iono- researchers, which enables semi-automatic spheric conditions, Sun and Jupiter observations scheduling of observations in local mode. Target and, on request, observations for selected pro- observations can be manually selected for a jects. specific time. For example, this takes place for the Routine PL610 observations are managed by international project where every two months

72 observations of the pulsar B1508+55 are per- method, including multiple scattering and refrac- formed. For the remaining time slots, a scheduler tion, we try to untangle the information contained searches for available visible radio sources (e.g. in the full rane (time, space, frequency) of Cas A, Cyg A, Tau A, Vir A, the Sun, Jupiter) and LOFAR data and verify a number of hypotheses fits them into four possible beams. All LOFAR about the local structure of the ionosphere and its data are made open access after one year, which evolution. allows wider scientific community to use them in - Development of analysis methods for detec- their research. tion of different scales (small and medium) iono- The current analyses being carried out at CBK spheric irregularities based on astronomical cali- PAN, based on LOFAR data, can be divided into bration data. For testing purposes, calibration so- three main topics: lutions from one of the key scientific LOFAR - Measurements of ionospheric scintillation at projects are used (Epoc of Reionization KSP), radio frequencies, and calculation of GNSS equi- providing sensitivity levels around three orders valent of the S4 index. This work is based on the higherthan those achieved using GNSS. observations made by the polish LOFAR station Pl610. (B. Matyjasiak, H. Rothkaehl, K. Budzińska, - Analysis and modelling of ionospheric irre- D. Przepiórka, M. Pożoga, M. Grzesiak, gularities from LOFAR scintillation data. Based R. Wronowski, Ł. Tomasik) on scintillation simulations using the phase screen

Ionosphere structural and temporal variation derived from a LOFAR calibration routine One of the key issues determining the quality of In 2019, we ran an analysis of ionospheric calibra- radio astronomy observations in the low frequen- tion solutions that are routinely calculated as part cy regime is the influence of the ionosphere on of the aforementioned project. These solutions transmitted electromagnetic signals. The proper cover many hours of winter, night time observa- removal of the ionospheric effect is especially tions (each observation lasts 6–8 hours) in the important when retrieving faint signals, such as HBA frequency range (110–250 MHz). This the 21 cm redshifted emission line of neutral found differential Total Electron Content values hydrogen from the Epoch of Reionization. The between LOFAR network stations (specifically, latter is the focus of the EoR project, based on the core and remote stations located in the Nether- use of the LOw Frequency ARray (LOFAR) lands), which, in turn, provided insight into interferometer. horizontal TEC gradients and structures existing in the ionosphere. The high temporal and spatial resolution, as well as the long time span of obser- vations gives us an insight into the morphology and dynamics of this ionized layer with respect to different geomagnetic conditions. This, in turn, may lead not only to a better understanding of the various processes that take place in the iono- sphere, but also to improvements in the calibra- tion technique itself and, therefore, the sensitivity of radio astronomy observations at low frequ- encies. (K. Budzińska, M. Grzesiak)

Fig. 40. Normalized auto-correlation function of differential TEC values between remote LOFAR stations and the reference, core station.

73 LOFAR as a new tool for ionospheric model validation The LOFAR (Low-Frequency Array for radio astronomy) radio interferometer is located in Europe, and observes radio signals in the frequ- ency range 10–240 MHz. It consists of multiple stations that can work as a part of a bigger radio telescope (in so-called ILT mode), as well as separately (in local mode), but with limited capa- bility. The unprecedented sensitivity of the LO- FAR to ionosphere electron concentration distri- bution enables us to monitor the dynamics and structure of large-scale irregularities such as traveling ionospheric disturbances (TID), as well as small-scale ionospheric structures. It provides measurements of electron density irregularities using ionospheric scintillation and differential total electron count (TEC), calculated between Fig. 41. Scatter plots of short time variation in TEC stations. LOFAR has proven to be a useful tool for values obtained from joint observations using HF radio monitoring and analysing the dispersion of the and GNSS monitoring techniques for a 2017 event. measured radio signal caused by the ionosphere. LOFAR network instrumentation can cover the ficantly increase existing space weather services mid-latitude and auroral region with scintillation capabilities. For this purpose analysis of iono- diagnostics at a level of sensitivity unavailable spheric conditions using LOFAR measurements, with GNSS diagnostics). The ability to simul- in both single station and ILT mode was used. taneously monitor solar activity, solar wind pro- (M. Pożoga, B. Matyjasiak. M. Grzesiak, perties and ionospheric conditions can signi- H. Rothkaehl, Ł. Tomasik, K. Budzińska)

Asymmetry in mid-latitude trough manifestation for northern and southern hemispheres The mid-latitude trough (MIT) manifests itself as • the impact of geomagnetic activity on trough a significant depletion in electron density and characteristics (position, width, depth and electron temperature increase in the sub-auroral gradients); region of the topside ionosphere. The region of • asymmetry between the northern and the main ionospheric trough is an unique area of southern MIT; the Earth's ionosphere, where different type • case studies related to geomagnetic storms instabilities and impact from bottom part of and other short-term and local processes that atmosphere and remote region of magnetosphere may impact the MIT's behaviour. can meet. It is well-known that the trough is highly A particular focus of our work is electron density sensitive to dynamic geomagnetic conditions. A data, mainly drawn from DEMETER and particularly distinct feature is that the trough's SWARM missions. properties change according to the phase of geomagnetic storms. In particular, it moves equa- Table 1 shows, in numbers, how MIT detections torward with the storm onset and, as the storm may differ according to the hemisphere. In gene- develops, it narrows and deepens. In 2019, our ral, local winter seems to be the most favourable work focused on the following points: period for MIT detection.

74 Table 1. DEMETER data relating to detection of the main ionospheric trough for different years.

(D. Przepiórka, B. Matyjasiak, H. Rothkaehl)

Modelling and analysis of LOFAR scintillation data Scintillation of beacon satellite signals or distant cosmic radio emissions can provide interesting information on the cosmic medium itself, its inter- nal spatial structure and basic evolution characte- ristics. The Low Frequency Array (LOFAR) is an excellent astronomical instrument as well as the very useful tool for studying irregularities in the ionosphere. Due to its operational frequency ran- ge (10-270 MHz, LBA range), LOFAR is very sensitive even to very small changes in iono- spheric electron density. The interferometric na- ture of the instrument allows for the multi-point observations, and, thus gives the possibility for ionospheric scintillation measurements over dis- tances ranging from tens of meters to hundreds of kilometers. The project for scintillation monitoring over the LOFAR stations has been carried out for several years and a large amount of data has been collec- ted and stored in the Long Term Archive (LTA). Available data contain signal amplitude for a few strongest radio sources (A Team) measured at all

Fig. 42. Correlations for zero time lag as a function of station position difference (left column) with the estimated quadratic form ellipse overlayed. Geometry for all three cases seem to be well-defined. The right column shows the time shift of the maximum cross-correlation in the separation function and the determined velocity vectors (red strip) as well as the isotropic estimate (blue strip). Black strip means vector with speed magnitude successively: 100 m / s, 1000 m / s, 1000 m / s.

75 core and remote stations. Based on the LTA data, umptions and compute diffraction pattern velo- correlation analysis between stations can be made cities for three different geophysical conditions. in order to obtain information about the chara- The results allow to attribute estimated quantities cteristics of ionospheric structures. to ionospheric irregularities. We take frozen-in assumption of scatter evo- To resolve this inconsistency we proposed double lution and derive simple formulas for characte- scattering scenario, where the incident wave ristics of spatio-temporal correlation function of undergoes two successive scattering by distinct observed diffraction pattern. Using Low Frequ- ionospheric layers with different plasma drift ency Array (LOFAR) Cassiopeia intensity obser- velocities what is shown in Figure 44. vation we are able to validate qualitatively the ass-

Fig. 43. Cut of the time lag vs. position dependence along plane containing mean gradient. First panel reveal unexpected nonlinear behavior while the other two follows frozen-in drift relation.

Fig. 44. Panel a) depicts the idea of forementioned scenario, panel b) shows the amplitude of scintillation on the ground formed by doubly scattered wave with superimposed receiving stations as black dots and panel c) gives cut of the time lag vs. position for simulated data and the observed by LOFAR on the right.

(M. Grzesiak, M. Pożoga, B. Matyjasiak, K. Budzińska, H. Rothkaehl)

76 PHYSICAL AND GEODETIC STUDIES OF SOLAR SYSTEM BODIES AND EARTH Planetology and Solar System Dynamics (Solar System Dynamics and Planeto- recorded by the OSIRIS camera of the freshly- logy Group) exposed subsurface after the Aswan cliff collapse. We find that the hypothetical subsurface blocks

Comet 67P/Churyumov-Gerasimenko should have |∆ εr'|≥ 0.15, setting an upper limit from Rosetta mission of ~ 1 m on the size of 67P/CG's primordial building blocks if they exist. Our analysis is VIRTIS – Rosetta measurements of 67P/C- consistent with a purely thermal origin for the ~3 G. The new analysis and modelling of spec- m surface bumps on pit walls and cliff faces, trometric measurements of the comet 67P/C-G hypothesized to be high-centred polygons formed were restarted. The additional geometric cali- from fracturing of the sintered shallow ice- brations were performed and presented at EPSC bearing subsurface due to seasonal thermal ex- 2019 by the first author D. Kappel. (“Geometric pansion and contraction. Potential changes in preprocessing for Rosetta/VIRTIS-M measurements of 67P/CG's radar reflectivity at these at X- and S- comet 67P/CG”). bands can be associated with large-scale structural The article is scheduled for 2020. changes of the nucleus rather than small-scale (D. Kappel, G. Arnold, L.V. Moroz, A. textural ones. Monitoring changes in 67P/CG's Raponi, M. Ciarniello, F. Tosi, S. Erard, C. Leyrat, radar properties during repeated close-ap- M.I. Błęcka, G. Filacchione, F. Capaccioni, and the proaches via Earth-based observations can con- Rosetta/VIRTIS Team) strain the dynamical evolution of its cometary Post-rendezvous radar properties of comet nucleus. 67P/CG from the Rosetta Mission: under- This paper was published in October 2019 in ding future Earth-based radar observations Monthly Notices of the Royal Astronomical Society. and the dynamical evolution of comets (E. Heggy, E. M. Palmer, A. Hérique, W. Kofman, Radar observations provide crucial insights into M. R. El-Maarry) the formation and dynamical evolution of co- Homogeneity of 67P/Churyumov-Gerasi- mets. This ability is constrained by our knowledge menko as seen by CONSERT: implications of the dielectric and textural properties of these for composition and formation small bodies. Using several observations by Ro- setta as well as results from the Earth-based Are- Context. After the landing of Philae, CONSERT cibo radio telescope, we provide an updated and probed the nucleus of 67P/Churyumov-Gerasi- comprehensive dielectric and roughness descrip- menko (67P) and observed no heterogeneities at tion of Comet 67P/CG, which can provide new metric scale within the probed part of its small constraints on the radar properties of other nu- lobe. Further studies have since quantified the clei. Furthermore, contrary to previous assum- observed homogeneity in terms of maximum per- ptions of cometary surfaces being dielectrically mittivity contrast versus the typical size of he-te- homogeneous and smooth, we find that they are rogeneities. Aims. The aim of this article is to interpret the dielectrically heterogeneous (εr'»1.6–3.2), and are rough at X- and S-band frequencies, which are sensitivity limits of CONSERT measurements in widely used in the characterization of small terms of composition, and to provide constraints bodies. We also investigate the lack of signal on the maximum variability in composition, broadening in CONSERT observations through porosity, and local dust-to-ice ratio. the comet head. Our results suggest that primo- Methods. The sensitivity of CONSERT measu- rdial building blocks in the subsurface are either rements to local variations in density, dust-to-ice absent, smaller than the radar wavelength, or have ratio, and composition was analysed using permit- a weak dielectric contrast (∆ εr'). To constrain this tivity modelling of mixtures. ambiguity, we use optical albedo measurements Results. We interpret the maximum detectable

77 heterogeneity size and contrast in terms of by adjusting the dielectric properties of the composition and porosity of the nucleus. The cometary interior, the position of the lander being sensitivity to porosity is ±10 percent points for fixed and exact. Based on this, we were able to heterogeneities with a characteristic length scale determine rays, their travel, their lengths and of a few meters; the sensitivity to local variations depth of propagation, as a function of the closest in the composition is limited. distance to the surface, and places from which The results of our research were published in signals left the comet and propagated to the Astronomy & Astrophysics (October 2019). spacecraft. (A. Hérique, W. Kofman, S. Zine, J. Blum, In our presentation, we discuss the dielectric pro-

J.-B. Vincentand V. Ciarletti) perties obtained for all rays – some of them pro- Revisiting CONSERT results taking into pagated from deep inside the comet and some account the exact lander position on the co- close to the surface. The main result of the pre- met sent analysis is observed variability in dielectric The CONSERT experiment measured the signals properties with the depth of the cometary inter- that propagated through the small lobe of 67P/C- ior. We conclude that close to the surface (on ave- G between the lander and the ROSETTA rage within 15 m depth), permittivity is between spacecraft (Kofman et al., SSR, 2007). The main 1.5 to 1.86; at greater depths, it is between 1.27 observed parameters are the propagation time and 1.4. This is an indication that the material and amplitude of the signal at given orbital posi- varies from higher density (denser dust or a higher tions of the Rosetta spacecraft. The exact posi- dust–to–ice ratio close to the surface), to a more tion of Philae lander was not known until Sep- icy interior (i.e. average density decreases inward). tember 2016 util then we only knew roughly There is also the possibility that porosity increases where it landed (Herique et al., PSS, 2015). As a with depth, but this is difficult to conclude based consequence, we were only able, by minimizing only on CONSERT measurements. This conclu- the error between the measured and simulated sion seems less plausible, compared to an incre- signal propagation time, to determine the average ase in the ice–to–dust ratio with depth, which is dielectric properties of the interior (Kofman et certainly possible. We discuss these results as a al., Science, 2015). Our work uses 3D modelling function of the comet's potential composition of propagation (Kofman et al., Science, 2015; and their influence of the materials on the model Herique et al., MNRAS, 2017) to exactly deter- of the cometary interior. mine rays propagating through the comet, and These results were presented at the AGU General which propagation times have the best match with Assembly, San Francisco 2019. those of measured signals. Matching is obtained (W. Kofman, S. Zine and A. Hérique)

Long-period and interstellar comets – their activity, dynamics and statistics Discovery statistics and the 1/a-distribution cometary reservoir (named the Oort Cloud) play of long-period comets for the period 1801– an important role in the dynamical evolution of 2017 long period comets and injecting them into the Our work was described in the 2018 Annual observability region of the Solar System. The aim Report, and a paper was published in February of our work was to discuss two cases in which 2019 in Monthly Notices of the Royal Astronomical orbits based on observational data were used, and Society. stellar perturbations of cometary motion (M. Królikowska and P. A. Dybczyński) (C/2002 A3 LINEAR and C/2013 F3 PAN- STARRS) were detected. Using the available data First stars that could significantly perturb from the Gaia DR2 catalogue, and some other comet motion are finally found sources, we searched for close stellar passages near Since 1950, when Oort published his paper on the the Sun. Our study took into account that some structure of the cloud of comets, it has been be- stars are part of multiple systems. Over 600 stars lieved that stars passing near this hypothetical or systems that approached, or will approach, the

78 Sun at distances closer than 4.0 pc were found. very similar results. However, a detailed analysis Once we obtained a complete list of perturbers, of the radial velocity uncertainty of Kruger 60 we studied their influence on a sample of 277 showed that the probability that this binary star is Oort spike comets that have been observed since a home system of 2I/Borisov is low. Finally, the 1901. We discovered that two comets might have use of a new, unpublished radial velocity for the had their orbits fundamentally changed due to a Kruger 60 system effectively ruled out this possi- close stellar encounter. Our results show how dif- bility. ferent the dynamical evolution of comets would These two stages of our research were published look if their motion is only considered in the Ga- in arXiv.org (in September and November 2019). lactic potential. Uncertainties both in stellar and (P. A. Dybczyński, M. Królikowska, cometary data were fully taken into account. Our analysis indicates that perturbations of cometary and R. Wysoczańska) motion due to passing stars are very rare, and the Non-gravitational effects change the original uncertainties of these effects are hard to estimate. 1/a-distribution of real near-parabolic co- The results of our work were published in the mets January 2020 volume of Monthly Notices of the Royal Seven decades ago, Oort (1950) postulated the Astronomical Society (published online: November existence of a huge cloud built from billions of 2019). kilometre-sized bodies or larger. His hypothesis (R. Wysoczańska, P.A. Dybczyński was based on a very small number of near-para- and M. Królikowska) bolic comets that visit the inner part of the Solar System. Since then, the number of such detected Kruger 60 as a home system for 2I/Borisov – a comets has increased tenfold, but we still know case study very little about the number and distribution of At the end of August 2019, the second interstellar the objects that constitute the Oort Cloud. Our comet, 2I/Borisov was discovered at a time when knowledge is poor, largely because so few para- it was 2.99 au from the Sun, and 3.72 au from the meters can be derived from the observational Earth. A month later, we searched for a candidate data. The only relatively reliable information we for its home system, using an orbital solution have is a distribution of the original 1/a for the based on 548 positional measurements spanning near-parabolic comets discovered so far. More- over about one month. Although we will never be over, to interpret this distribution realistically, we sure which star or stellar system this comet comes need to be able to dynamically separate new from, we obtained a very small relative velocity comets (that visit the inner Solar System for the and a promisingly small miss-distance for a star first time) from old comets, because the latter have when tracing motion of 2I/Borisov back in time distorted orbits due to their earlier passages through space; it suggests that this body can be a through the planet zone, during which planetary good candidate of origin of comet Borisov. In the perturbations changed their semi-major axes. context of our long-standing study of Oort spike Our work is part of a long-standing research comets' dynamics, we recently updated a list of project on the origin of Oort Cloud comets. In potential stellar perturbers of cometary motion one of our previous papers (Królikowska & (using the Gaia DR2 catalogue). This list was Dybczyński, 2017, KD17, see the Annual Report checked against a past, close and slow encounter 2017), we investigated the dynamical evolution of with 2I/Borisov. Only one of of the 647 stars or Oort spike comets (original semimajor axes grea- stellar systems in our list – a double star Kruger 60 ter than 10,000 au) with perihelion distances – appeared as a potential candidate for the origin exceeding 3.1 au. This selection minimized the of this comet. Later archival research unearthed potential effects of nongravitational (NG) forces some prediscovery positions of 2I/Borisov, and on comet motion. In a sample of 100 such objects, we therefore repeated our calculations using more only 16% showed some degree of deviation from 2I/Borisov data (1711 observations from the purely gravitational (GR) motion within the ob- period 13 Dec 2018 –2 Nov 2019). This found served arc.

79 Fig. 46. Upper panel: Distribution of original 1/a based on preferred orbits for the whole sample of small- Fig. 45. Strength of NG acceleration acting on cometary perihelion LPCs, of which 64% are NG orbits. For nuclei at perihelion for the sample of Oort spike comets. comparison, the lower panel shows the original 1/a- Solutions obtained in KD17 are shown in light red ( the distribution for purely GR orbits. NG orbit is based on the standard g(r)-function), and blue dots (g(r)-like function adequate for CO-sublimation). By obtaining a sufficiently large sample of NG The solutions presented here are shown by green squares, orbits for small-perihelion LPCs, it was possible to magenta triangles, and red dots, all of which represent preferred solutions based on the standard g(r)-function. construct a distribution of 1/aori for an almost The two solutions marked as cyan dots represent models complete sample of these comets, 64% of which for comets C/2012 S1 and C/2002 O7 based on the CO- were based on NG orbits. The resulting distri- driven formula. bution is shifted by about 10- 5 au- 1 to higher values

Our current work considers a sample of 122 long- of 1/aori compared with the distribution that is period comets (LPCs) with small perihelion obtained when NG effects are ignored (Fig. 46). distances (q < 3.1 au) and original 1/aori < Additionally, we found differences in 1/aori-distri- - 1 0.000100 au for purely GR orbits. They form an butions between LPCs with q < 3.1 au and those almost complete sample of such objects disco- with q > 3.1 au. These findings indicate the impor- vered in the period 1885–2012. In this sample, the tant role of NG acceleration in the motion and NG effects play an important role. We determined origin of kpng-period comets, and in the for- NG orbits for the majority (78) of these small- mation of the Oort Cloud. perihelion comets. Figure 45 presents a statistical The results of this work was appeared in the analysis of the magnitudes of NG acceleration January 2020 volume of Astronomy & Astrophysics for about 100 Oort spike comets. (published online: December 2019). (M. Królikowska)

Use of production rate curves and a non-gravitation acceleration model for long-period comets

I selected the sample of long-period comets for mation about outgassing as a function of helio- which photometric data and production rate mea- centric distance, r. Production rate detections can surements, as well as astrometric data were good be supplemented by far more numerous bright- enough to determine both the outgassing profile ness measurements at different orbital positions. and non-gravitational effects. The detected However, these measurements must first be production rates of volatile components (mostly converted into the gas production rate. I derived

H2O and CO) of cometary nuclei provide infor- empirical correlations between visual magnitudes

80 and gas production rates for each comet separa- the proposed non-gravitational force model relies tely. Magnitudes measured by different observers on observed production rates (a g-like function). with different instruments can differ by several Non-gravitational perturbations in the orbital units of magnitude. Thus, a special effort was ma- motion of comets were investigated based on de to construct high-quality cometary light curves positional observations and modified, g-like func- with a slight dispersion. tions. Additionally, the derived non-gravitational In the standard formalism, the orbital calculation acceleration and gas production rates were used to of non-gravitational effects is based on a special estimate masses of studied comets. function, g(r) that simulates the water production Preliminary results were presented at the ACM rate. However, the shapes of cometary produc- 2012 conference by S. Szutowicz, and reported in tion rate curves differ from g(r) function. Thus, 2012. This research is ongoing. (S. Szutowicz) Outer solar system dynamics in a stellar cluster Hans Rickman led a research project that aimed to discussed and developed techniques for com- clarify the role of the Sun's birth cluster in shaping municating the cluster simulation results into the most remote, small body populations of the Solar System integrations. Solar System – generally referred to as the Oort One, novel technique is to use a dense time series cloud and the Inner Oort cloud. This required the of cluster outputs to derive a smooth, analytic development of dedicated tools to simulate the formulation of the stellar tide as a function of dynamics of the stellar cluster, and the dynamics distance from the centre, by fitting to numerical of small bodies orbiting a solar-type cluster mem- estimates of the force function, based on the ber at large distances, under the influence of gra- positions of individual stars. The template for vitational scattering by giant planets. these formulae is a generalisation of the Plummer The team included Drs Paweł Wajer and Tomasz model that is used for the initialisation of the Wiśniowski. Hans Rickman provided ideas, kno- cluster. This offers a way to elucidate the cluster wledge and inspiration; Paweł Wajer developed evolution based on the initial virialisation and the and ran simulations of gravitational scattering in expansion caused by gas loss. Papers discussing the outer Solar System by the RA15 integrator; both the evolution of young stellar clusters and and Tomasz Wiśniowski implemented and tested the roles of cluster tide and close stellar enco- the open access NBODY6++GPU code deve- unters in populating the outskirts of planetary loped to simulate gravitational, many-body sys- systems by small bodies are under development. tems with the initial aim of study the evolution of This project is ongoing. new -born, embedded clusters. The whole team (H. Rickman, P. Wajer, T. Wiśniowski and an international team)

The long-term evolution of Main Belt Active Asteroids Solar System small bodies are conventionally cal- activity. The latter category are known as active led comets or asteroids, depending on their obser- asteroids; they have semi-major axes below 5 AU, vational and dynamical properties. Objects with a Tisserand parameter larger than 3, and show unbound atmospheres and a Tisserand parameter evidence of mass loss (as they have a comae or a (a dynamical parameter measured with respect to tail). Jupiter's orbit) below 3 are known as comets, Most currently-known, active asteroids are loc- while objects lacking such atmospheres, and with ated in the Main Belt, where their dynamics is a Tisserand parameter above 3 are called asteroids. driven by mean motion resonances (MMRs) with However, it is difficult to consider this standard Jupiter and Saturn, and υ6 secular resonance. Yar- classification as complete, as we can observe bo- kovsky and YORP effects are other important dies on cometary orbits with no activity, and ob- factors impacting small body dynamics in this jects on asteroidal orbits that exhibit cometary

81 region. Unfortunately, both of the latter factors cometary type activity. We then compare their strongly depend on physical parameters (surface influence on the long-term evolution of the inve- and bulk thermal conductivity, surface heat capa- stigated small bodies. Our research should allow city, surface density, spin, shape of a body, etc.), us to draw some conclusions about ejection me- which are hard to determine. Recent papers have chanisms in different parts of the Main Belt, and indicated detections of non-gravitational acce- the influence of models on the observed struc- leration for most active asteroids. ture of the NEO population. Our work focuses on the dynamics of active aste- So far, we have developed the code needed for our roids in two, distinct models of non-gravitational computations. Initial results will be available in forces: the first uses Yarkovsky effects; the second 2020. uses the standard model of non-gravitational (R. Gabryszewski, P. Wajer and M. Królikowska) Missions to solar system objects GALAGO: the highland terrain hopper – a trometer orbiting Mars, CRISM (the Compact cutting-edge planetary locomotion system Reconnaissance Imaging Spectrometer for Mars) This project, carried out in cooperation with As- onboard the Mars Reconnaissance Orbiter tronika, aims to develop GALAGO, a light and (MRO), struggles to detect sulfides on the Martian robust jumping locomotion system designed to be surface; spectral interference with silicates impede dropped anywhere on the surface of a celestial sulphide detection in the 0.4–3.9 µm CRISM body that has reduced gravity compared to Earth. range. In contrast, at least four common sulphides After quickly analysing its surroundings, it will found on Earth and Mars (pyrite, chalcopyrite, hop, leap or crawl to wherever investigators want marcasite, pyrrhotite) have prominent absorption it to work, within a maximum single jump distance peaks in a narrow, far-infrared (FIR) wavelength of several meters (depending on the gravity) range of 23–28 µm. Providing global distribution vertically and horizontally. Its low mass makes it and chemical composition of sulphide ores would possible to simultaneously launch several hoppers help in choosing useful targets for future Mars that can work as a fractionated explorer at a very exploration missions. Therefore, we have begun competitive price. After reviewing their potential work on the design of a relatively cheap and sim- payload, we illustrated the scientific capabilities of ple pyroelectric detector-based Martian far-IR hopper and hopper networks in carrying out basic ORE Spectrometer (MIRORES) measuring three, geologic observations at distinct study sites in a wide spectral bands limited with filters, including variety of geological environments, obtaining da- the main 23–28 µm band, and two reference bands ta along steep, geological cross-sections, sur- at 18–21 µm and 35–40 µm. Focusing only on sul- veying geophysical anomalies in the subsurface, phides will make it possible to reduce the instru- prospecting for resources, monitoring micro- ment's dimensions to microsatellite size. The environments, or characterizing dust activity on largest challenge related to this design is the small the Moon. Finally, we have selected the payload field of view conditioned by the high resolution and proposed experimental scenarios to be exe- required for this study (10–20 m/px), which, in cuted during the test campaign. limited space, can only be achieved by the use of the Cassegrain optical system. The probe could be (J. Gurgurewicz, D. Mège and A. Nicolau-Kuklińska) launched as a piggyback mission with a larger Design of the Martian far-IR ORE Spectro- satellite (for example, the Japanese Martian meter MIRORES Moons Exploration) during the 2024 or 2026 Sulphide ores are a major source of noble (Au, Mars launch window. Ag, Pt) and base (Cu, Pb, Zn, Sn, Co, Ni, etc.) Our preliminary results were presented at the metals, and will, therefore, be vital to the self- COSPAR conference in Herzliya, Israel. sustainment of future Mars colonies. Martian (J. Ciążela, J. Bąkała, J. Barylak, M. Ciążela, meteorites are rich in sulphides, which reflects in M. Kowaliński, S. Płocieniak, J. Gurgurewicz, recent findings from Martian rovers. However, D. Mège, B. Pieterek, Ż. Szaforz, P.-A. Tesson, the only high-resolution (18 m/px) infrared spec- M. Giuranna, F. Pirajno)

82 A Low Frequency Radar to Fathom Asteroids moonlet in 2026. This paper presents the scien- from the Juventas Cubesat on HERA tific rationale, the mission and the radar that is Despite several, asteroid-orbiting missions, an expected to explore the interior. asteroid's internal structure has never been obser- The HERA mission was accepted by the Mini- ved directly. However, this question is crucial for sterial Conference in November 2019 and is pre- science, planetary defence and exploration. Wit- sented in EPSC Vol. 13, EPSC-DPS2019-807-2, hin the context of the HERA mission, the LFR 2019. on the Juventas Cubesat will fathom Didymos's (A. Herique, D. Plettemeier, W. Kofman, Y. Rogez, Ch. Buck and H. Goldberg) Mars

MoMo: a new empirical model of the Mars This research was published in the Journal of ionospheric total electron content based on Mars Space Weather Space Climate (October 2019). Express MARSIS data (N. Bergeot, O. Witasse, S. Le Maistre, P.-L. Blelly, Aims: Several scientific landers and rovers have W. Kofman, K. Peter, V. Dehant and J. M. Chevalier) reached the Martian surface since the 1970s. A new method for determining the total ele- Communication between the asset (i.e., the lander ctron content in Mars' ionosphere based on or rover) and Mars orbiters or Earth antennas Mars Express MARSIS data uses radio signals in UHF to X-band frequencies passing through the Mars' ionosphere. It is We present a new method for determining the to- consequently necessary to take into account tal electron content (TEC) in the Martian iono- electron density variation in the ionosphere to sphere based on the time delay of radar pulses re- correct the refraction of the signal transmitted. ceived by the Mars Advanced Radar for Subsur- face and Ionospheric Sounding (MARSIS) on- Methods: We developed a new empirical model of board the Mars Express spacecraft. As previous the Mars' ionosphere called MoMo. It is based on studies of the same dataset have produced dif- the large Total Electron Content (TEC) database fering results for the day-side ionosphere, it is derived from the subsurface mode of the Mars useful to have an alternative way to compute TEC Express MARSIS radar. The model provides in this region. Our method iterates a model iono- vertical TEC as a function of solar zenith angle, sphere, in order to simultaneously match iono- solar activity, solar longitude and location. For spheric delays in the signals received by the radar's validation, the model is compared with Mars Ex- two channels. It does this by finding the model press radio occultation data as well as with the nu- that minimizes the root mean square error bet- merical model IPIM (IRAP Plasmasphere-Iono- ween measured and simulated delays. Topo- sphere Model). graphical information is obtained from data from Results: We discuss the output of the model in the Mars Orbiter Laser Altimeter (MOLA) instru- terms of climatology behaviour of the Mars' ment. The model parameters are held constant for ionosphere. The output of MoMo is then used to a given orbit, and very good agreement between quantify the impact of the Martian ionosphere for simulated and measured delays is obtained. TEC radio-science experiments. From our results, the can then be inverted from the ionospheric model. ? 3 ? 1 effect is of the order of 10 mm s in Doppler Matching the delays of the two channels simu- observables, especially around sunrise and sunset. ltaneously introduces an additional constraint into Consequently, this new model could be used to the model, which has not been made in previous support the data analysis of any radio-science studies. The model is additionally validated by experiment and, especially, for present InSight matching simulated pulses with raw range-com- RISE and future ExoMars LARA instruments pressed measurements for one orbit. Finally, typi- that aim to develop a better understanding of the cal model parameters are compared to those ob- deep interior of Mars. tained by previous studies, which are also

83 simulated. The method is applied to orbits during the first 9 months of imaging with CaSSIS was moderate solar activity, and our results show very presented at the 50th Lunar and Planetary Science good agreement with previous studies. Conference and the 9th International Conference The results of these studies were published online on Mars. in December 2019 in Planetary and Space Science. (An international team led by N. Thomas, including M. (P. Conroy, G. Quinsac, N. Floury, O. Witasse, M. Banaszkiewicz, W. Kofman, P. Orleański, P.-A. Tesson, Cartacci, R. Orosei, W. Kofman, B. Sánchez-Cano) P. Wajer and P. P. Witek from CBK PAN) The Colour and Stereo Surface Imaging Sys- Trace gases on Mars tem (CaSSIS) for the ExoMars Trace Gas Or- In 2019, the studies on measurements recorded by biter the stereoscopic camera CaSSiS (The Colour and This investigation was partly described in the Stereo Surface Imaging System) and the NO- Annual Report 2016. MAD spectrometer were continued. Both instru- The CaSSIS camera, which operates onboard the ments are part of the payload Trace Gas Orbiter ExoMars Trace Gas Orbiter (TGO), was designed (TGO) of the ExoMars ESA mission. to acquire colour and stereoscopic images of the The CaSSiS camera gives the opportunity of Martian surface and provide geological context to analysis the locations and structure on the surface potential trace gas sources. Since the beginning of of Mars possible sources of trace gases e.g. me- the TGO's Science Phase in April 2018, members thane. From the orbiter identification and moni- of the ZDUSiP (notably the EXOMHYDR team) toring of minor species in the atmosphere are per- have proposed potential targets in several areas of formed by spectrometric instruments (e.g. NO- interest using the CaSSIS Suggestion Targeting MAD, ACS). (CaST) web tool. CaSSIS images are planned Various types of features on the Martian surface weeks in advance, based on the predicted space- may be associated with trace gases release. It craft trajectory provided by the European Space seems likely that the processes that enable me- Agency. Image acquisition is planned based on thane emission were created in different ways, one earlier suggestions and potential targets that the of which is production from serpentinized rocks. TGO flies over during a specific orbit. Our models provide estimates of spectral In March 2019, P.-A. Tesson and, in April–May reflectance/emittance and total radiance from the 2019, P. P. Witek planned observations based on Martian surface and the atmosphere in the mid- suggestions provided by colleagues, taking into infrared spectral range. For selected locations the account potential targets and technical con- various surfaces were spectrally described using straints. presumed reflectance or emissivity of minerals Images planned by P.-A. Tesson were acquired by CaSSIS in May 2019 and were made available by staff at Bern to the Science Team. Planning ses- sions identified several areas of interest for the EXOMHYDR project; this included zones such as Tharsis volcanoes summit calderas and tecto- nic features on Valles Marineris floor. Images planned by P.P. Witek were acquired by CaSSIS in July 2019. These acquisitions were severely limited by the lack of stereo and targeting capability. Consequently, he mainly chose targets with rich stratigraphy and varied composition, such as layered deposits of different colours, and Fig. 47. The results of our numerical simulations. The nadir measurement of the surface and atmosphere of deposits of sulphates and chlorides. Mars showing radiance at the top of the atmosphere in Another CaSSIS data acquisition planning session the spectral region of strong absorption of methane. Calculations include: constant reflectance of the surface was held in December 2019 by P.-A. Tesson for equal to 0.3 and four concentrations of CH4 in the images to be taken in March 2020. An overview of atmosphere.

84 and rocks (e.g. serpentinized rocks) calculated compare the data obtained by the spacecraft's from optical constants (n, k) with Mie and Hapke instruments to describe the lower boundary con- theories. The physical properties of the atmo- ditions (at the surface) that we need for our atmo- sphere were characterized by its thermodynamic spheric photochemical model. This research is parameters, and absorption and scattering pro- ongoing. cesses. The common influence of optical spectral (P. Wajer, P.P. Witek, W. Kofman features of the surface and atmosphere contai- and M. Banaszkiewicz) ning trace gases in various physical conditions on Evidence for thermal-stress-induced rock- simulated radiance spectra were analysed. falls on Mars impact crater slopes Our conclusions regarding visibility of spectral Recent rockfalls in impact crater slopes on Mars features of trace gases (methane) in total radiance display a slope aspect and latitudinal trends spectra were discussed during meetings of the (equator-facing rockfalls are more numerous than Martian group at CBK PAN, and were presented pole-facing ones between - 50° and+40°). A com- at the IUGG General Assembly 2019 in Montreal parison with insolation patterns indicates that (“Study of the influence the composition and tex- thermal stress plays an important role in Mars tures of Martian surface on detection the atmo- rockfalls. spheric methane – the numerical simulations” This topic was described in the Annual Report M.I. Błęcka). 2018 and a paper describing our results was The examples of the result of our numerical published online in Icarus (October 2019). modelling are shown in the Figure 47. (P.-A. Tesson, S.J. Conway, N. Mangold, Our work goes on, and we plan to submit a paper J. Ciążela, S.R. Lewis, and D. Mège) presenting our findings in 2020. (M. I. Błęcka) Deep-seated gravitational slope deformation scaling on Mars and Earth: the same fate for Modelling the transport of trace gases in the different initial conditions and structural evo- Martian atmosphere lutions The European-Russian ExoMars Trace Gas Or- We investigated the topography of selected para- biter (TGO) has been in scientific orbit since glacial, deep-seated gravitational slope deforma- 2018. The orbiter furnishes data on the abun- tion (DSGSC) scarps on Mars, and in the Tatra dance of trace gases, as well as colour and stereo Mountains. Starting from different initial condi- images of the surface that are useful in characte- tions, the final ridge geometry was found to be rizing sources and sinks of certain atmospheric similar. Because DSGSD scarps are expected to trace gases. One of the most interesting subjects have become inactive in both regions, their com- of investigation is the appearance and disap- parison suggests that whatever the initial ridge pearance of methane (Ch4) on short timescales. morphology, DSGSD proceeds until a mature We have developed a single-column model of the profile is attained. The longer activity of the Martian atmosphere to compute its steady-state Martian faults may be correlated with a long suc- chemical composition. All constituents of the cession of climate cycles generated by the un- atmosphere are subjected to solar radiation and stable Mars obliquity. react with each other in the presence of This topic was described in the Annual Report atmospheric aerosols. Taking this as a starting 2018 and a paper presenting our work was publi- point, we will study the release, propagation and shed in Earth Surface Dynamics (April 2019). loss of trace gases such as methane, other (O. Kromuszczyńska, D. Mège, K. Dębniak, J. hydrocarbons, together with sulphur and chlorine Gurgurewicz, M. Makowska and A. Lucas) species. In a second phase, we will compare our simulations with data acquired by the probe. Dynamic accretion beneath a slow-spreading ridge segment: IODP Hole 1473A and the This model will help us to better-understand the Atlantis Bank Oceanic Core Complex origin and evolution of trace gases, especially The 809-m-deep IODP Hole U1473A at Atlantis CH4. We also plan to use simulations of gas tran- sport from the subsurface to the surface, and Bank, SWIR, is 2.2 km from the 1,508-m Hole

85 735B and 1.4 km from the 158-m Hole 1105A. of cumulate gabbroic rocks and an upper layer of Mapping has provided the first 3-D view of the differentiated basalts. The thicknesses and pro- upper levels of a 660-km2 lower crustal batholith. portions of the gabbroic and basaltic layers in dif- The batholith is laterally and vertically zoned, ferent oceans are largely controlled by spreading representing a complex interplay of cyclic intru- rate, magma supply, and magmatic differentiation sion and ongoing deformation, with kilometre- processes. Evaluating the effects of complex scale upward and lateral migration of interstitial magmatic differentiation as a function of the melt. Transform wall dives over the gabbro-peri- spreading rate on Ca isotope composition is criti- dotite contact found only evolved gabbro intru- cal to understanding whether the Ca isotope com- ded directly into the mantle near the transform. positions of oceanic crust from different oceans There was no high-level melt lens, rather the are homogeneous and, thus, whether the obser- gabbro crystallized at depth, and then emplaced ved considerable variation of δ44/40Ca in basalts into the zone of diking by diapiric rise of a crystal (up to 0.4‰) results from magmatic differen- mush followed by crystal-plastic deformation and tiation or mantle source heterogeneity. faulting. The residues to mass balance the crust to To address the question, we present δ44/40Ca mea- a parent melt composition lie at depth below the surements of a series of gabbroic rocks (n=38) centre of the massif-likely near the crust-mantle and mineral separates from the 810-m-long boundary. Thus, basalts erupted to the seafloor U1473A hole drilled into the gabbroic lower crust from >1,550 mbsf. In contrast, the Mid-Atlantic at the ultraslow-spreading Southwest Indian Ridge lower crust drilled at 23°N and at the Atlan- Ridge (SWIR), along with 12, mid-ocean ridge tis Massif experienced little high-temperature basalts (MORBs) from the slow-spreading South deformation and limited late-stage melt transport. Mid-Atlantic Ridge (SMAR) and the fast- They contain primitive cumulates and represent spreading East Pacific Rise (EPR). Although the direct intrusion, storage, and crystallization of gabbroic rocks of the SWIR reflect several events parental MORB in the thinner crust below the of magma supply and strong magmatic differen- dike-gabbro transition. The strong asymmetric tiation (bulk rock Mg# of 64–79 for each event), spreading of the SWIR to the south was due to their δ44/40Ca values (0.85±0.09‰, 2sd, n=37) fault capture, with the northern rift valley wall are uniform. The results are consistent with limi- faults cut off by a detachment fault that extended ted inter-mineral Ca isotope fractionation bet- across most of the zone of intrusion. This caused ween plagioclase (Pl) and co-existing clinopy- rapid migration of the plate boundary to the roxene (Cpx) in the accumulated gabbro (average north, while the large majority of the lower crust 44/40 ∆ CaPl-Cpx=- 0.10‰, n=5). This indicates that spread south, unroofing the Atlantis Bank and no measurable Ca isotope fractionation occurs uplifting it into the rift mountains. during the formation of ultraslow-spreading Most of our research was conducted in 2018 and, oceanic crust. in 2019, a paper presenting our work was MORBs from the SMAR and EPR show published in the Journal of Geophysical Research: Solid 44/40 consistent δ Ca values (0.82±0.08‰ (2sd, n=4) Earth. and 0.86±0.09‰ (2sd, n=8), respectively), regar- (H. J. B. Dick, C. J. MacLeod, P. Blum, N. Abe, dless of the degree of fractional crystallization. D. K. Blackman, J. A. Bowles, M. J. Cheadle, K. Cho, On the whole, the ultraslow-, slow- and fast- J. Ciążela, J. R. Deans, V. P. Edgcomb, C. Ferrando, spreading gabbroic cumulates and MORBs L. France, B. Ghosh, B. M. Ildefonse, M. A. display indistinguishable δ44/40Ca within analytical Kendrick, J. H. Koepke, J. A. M. Leong, C. Liu, uncertainty, suggesting a homogenous Ca isotope Q. Ma, T. Morishita, A. Morris, J. H. Natland, composition for the global igneous oceanic crust T. Nozaka, O. Pluemper, A. Sanfilippo, J. B. Sylvan, (δ44/40Ca=0.85±0.09‰, 2sd, n=49) even if they M. A. Tivey, R. Tribuzio, and G. Viegas) experience complex magmatic differentiation. Calcium isotopic compositions of oceanic Comparison with values for fertile mantle rocks crusts at various spreading rates (δ44/40Ca=0.94±0.10‰) reveals that partial mel- The oceanic crust consists mainly of a lower layer ting triggers only slight Ca isotope fractionation

86 (0.09±0.02‰, 2se). In this light, the considerable The preliminary results of our work were publi- variation in previously-reported δ44/40Ca values for shed in LPSC Abstracts (March 2019). basalts may result from their different mantle (D. Mège, J. Gurgurewicz, S. Douté, F. Schmidt and sources, and is probably attributable to the R.A. Schultz) recycling of crustal materials. ExoMars TGO/CaSSIS colour imaging of This research was mainly conducted in 2018 and, late lava flows and hydrothermal alteration in in 2019, a paper was published in Geochimica et the Ladon Basin, Mars Cosmochimica Acta. The CaSSIS colour stereo camera onboard Exo- (C. Chen, J. Ciążela, W. Li, W. Dai, Z. Wang, Mars/TGO views the surface of Mars with 4 fil- Z. Jin, S. F. Foley, L. Ming, Z. Hu, and Y. Liu) ters in the range 0.4–1.2 µm and pixel size 4.6 m. Shear tectonics in Valles Marineris Its colour capabilities for geological interpre- tations are explored in the Ladon impact basin, The presence of a dense swarm of dikes, several and reveal a surprising diversity of terrains that tens of meters thick on the floor of Ophir Cha- CRISM, CTX, and HiRISE data help in inter- sma, which do not cut the surrounding Interior preting further. It is most likely that the surface is Layered Deposits, indicates that kilometres of capped by a rather fresh, thin mafic or ultramafic bedrock must have been eroded or are missing in flow, dated middle Amazonian, underlain by a this part of Valles Marineris. We report on the exi- serpentinized flow of similar composition. These stence of brittle-plastic, NE-SW-oriented dextral results indicate that a long time after formation, shear zones similarly exposed in the deepest parts the Ladon basin underwent volcanic and hydro- of Ophir Chasma (Fig. 48), as well as Hebes Cha- thermal activity, and reveals the exceptional po- sma. We discuss their identification, kinematics, tential of CaSSIS for geologic mapping. age, the nature and mineralogical composition of the deformed rock, and their role in the tectonic, These preliminary results were published in Geo- erosional, and geomorphological evolution of physical Research Abstracts (April 2019) and Valles Marineris. EPSC Abstracts (September 2019). (D. Mege and J. Gurgurewicz) Very-high-resolution ground magnetics cha- racterisation of hydrothermal processes in the Danakil depression Understanding hydrothermal processes in salts has applications on Mars, where thick salt (sul- phate) sequences are common, and past or pres- ent hydrothermal systems are likely to be wide- spread. Hydrothermal circulation alters rock magnetization due to dissolution. High-resolution magnetic surveying is therefore able to distinguish between areas of strong and weak hydrothermal activity, as well as associated structural discon- tinuities. Preliminary results from very-high-reso- lution magnetic surveying at unprecedented reso- lution were obtained in Lake Asale, in the Danakil depression, near Dallol. Hydrothermal circulation patterns are correlated with geologic evidence at the surface, such as open fissures, hydrothermal pools, noise generated by subsurface bubbling, and moist ground. Our preliminary results were published in EPSC Abstracts (September 2019). Fig. 48. Tectonic map of the main shear zone exposure in Ophir Chasma in Valles Marineris, Mars. (D. Mège, H. Choe, J. Dyment, H. Tsegaye, B. Ayele, B. Tadesse, H. Hansen)

87 Chains of cones on Martian Isidis Planitia several types depending on their conformation In 2019, we continued our research from 2018. (Fig. 49). Although we see a type of residual volca- We are examining the volcanic system of cones on nism, we do not know if it is related to the Syrtis Isidis Planitia. Many of these chain forms have a Major area in any way. We are currently working characteristic furrow through the centre, sug- on determining the duration of this volcanism gesting that linear volcanism dominated in the and its age, and determining the size of the Isidis area. The cones have dimensions ranging magmatic chamber that was once under Isidis. from 300 to 500 m and a height of about 30 m. The mathematical algorithm developed by Mał- This type of volcanism is seen in Iceland. Some of gorzata Jenerowicz will help to identify the conical the Isidis cones are arranged in concentric circles structures in this area. that keep the cone shape, but without a furrow. The spatial distribution map of cones is now This type of volcanism is seen on the archipelago almost complete. of the Canary Islands and, in particular, Lan- (N. Zalewska, M. Jenerowicz, zarote. The cones on Isidis have been divided into L. Czechowski, J. Ciążela)

Fig. 49. HiRISE images. An example of dividing cones into types. Chain-shaped cones – type A PSP_009375_1935 (Lanzarote), and chain-shaped cones with a characteristic furrow – type B-ESP_019291_1965_RED (Icelandic). Courtesy of Mateusz Kuzaj. The cones system on the border of Acidalia show a number of individual volcanoes along the and Chryse tongue borders. We suggest that these are, ho- In 2019, we continued work that began in 2018 on wever, volcanic deposits and not lava tongues, determining the genesis of the arrangement of although we do not exclude the origin of ground- tongue with concentric forms of small cones on water, which would be responsible for mud volca- their surface, on the border of Acidalia and Chry- nism. We observe that the slope of the terrain has se areas. Last year, we suggested a type of rootless characteristic tongues running from west to east, cones volcanism; however, there are some which excludes lava flow in the opposite direction inaccuracies that exclude this type of volcanism. and, thus, rootless cones. An unusual type of vol- Photos from THEMIS V55617012 and CTX canism, unheard of on Earth, is observed. This P22_009485_2187_XN_38N040W (Fig. 50) looks like flat lava domes flowing out of semicir-

88 cular furrows, along which, and at a distance from them, are formed parallel, small volcanic cones with a base of 50 m. An article is being prepared for submission with the working title “Some remarks about the origin of chains of cones in Chryse Planitia”.

Fig. 50. CTX P22_009485_2187_XN_38N040W. Acidalia/ Chryse. Marking of cones on tongue structures and lava flow direction. (N. Zalewska, L. Czechowski, M. Ciążela, J. Kotlarz, P. Witek) Using surface temperature from the PFS/ MEX dataset to track ice distribution on Mars Tracking the surface temperature distri- bution on Mars can provide unique in- formation on thermo-physical surface properties that complement informa- tion from images in the visible range. In the first phase of our work, we genera- ted night-time temperature maps of Mars for 12 time intervals (months) to investigate thermal distribution chan- ges over time. We then calculated thermal inertia maps for the Martian summer (Ls=90°–150°) and winter (Ls= 270°– 330°) using the apparent thermal inertia (ATI) ap- proach: ATI=(1- A)/∆T, where A is albedo and ∆T is the temperature dif- ference. We used the PFS night-time and daytime temperatures database, along with the global NIR 1-micro- meter albedo map of Mars from the same mission. The albedo map is based on reflectance data acquired by the OMEGA spectrometer from January 2004 to August 2010. The presence of Fig. 51. Thermal inertia maps for Ls=90°–150° (top) and ice may also, indirectly, indicate hydrothermal Ls=270°–330° (bottom) following the ATI approach. Black sites on Mars. This method is especially efficient lines indicate the global boundary (along ~ 1000 J m- 2 - 1 - 1/2 at identifying seasonal surface ice, as it shows K s ) between high thermal inertia values interpreted as -2 -1 - polar ice (marked in red) and lower thermal inertia values, highly-enhanced thermal inertia (>1000 J m K s marked with white dashed lines. Martian soils are marked in 1/2 units) compared to Martian soils (<600), due to blue.

89 the higher thermal conductivity and heat capacity submitted to Journal of Geophysical Research: of ice. We are using the PFS/MEX dataset, which Planets. consists of 1,424,366 surface temperature retrie- (J. Ciążela, D. Mège, B. Pieterek, M. Ciążela, vals collected over 18438 Mars Express orbits, J. Gurgurewicz, A. Lagain, P.-A. Tesson) encompassing 9 successive Mars years (Ls=331° Hydrae Cavus: a tectonic basin in the Valles of MY26 to Ls=21°of MY34). Marineris region This research is ongoing. Our previous work revealed dextral brittle-plastic (M. Ciążela, J. Ciążela, D. Mège, M. Giuranna, NE-SW shear zones that affect the deepest parts P. Podgórski, B. Pieterek, J. Gurgurewicz, of Hebes Chasma and Ophir Chasma, (Mège and P.-A. Tesson, and P. Wolkenberg) Gurgurewicz, 2018). These results suggested that the northern part of Valles Marineris is probably composed of large sheared tectonic blocks that Active magma chambers on Mars moved relative to each other, while Valles Mari- In the absence of volcanic activity captured by the neris was being stretched perpendicular to its Mars exploration spacecrafts, or associated ef- main, ESE trend (Schultz, 1995; Mège and Mas- fects such as enhanced surface thermal signatures, son, 1996). Following this work, we have sought to volcanism on Mars may appear to be extinct. Yet identify other tectonic features linked to this shea- Martian volcanic terrains dated from Late Ama- ring episode in the vicinity of Valles Marineris. zonian (2.4 Ma) to Noachian (>3.7 Ga), and Hydrae Cavus is a 20 by 60 km, 1600-m-deep, steep-sided depression located 130km east of atmospheric CO2 isotopic signatures indicate recent volcanic degassing. Volcanism on Mars Candor Chasma. Previous morphological map- could, thus, be dormant rather than extinct. We ping (Marra et al., 2015) suggests a tectonic origin modelled magma fluxes in the two largest Martian for the opening of the basin. Using an available igneous provinces, Tharsis and Elysium, and dataset (CTX imagery and HRSC Digital Eleva- found that the largest volcanoes of Tharsis sho- tion Models), we have mapped the tectonic fea- uld have erupted on average ~150 km3/Myr in the tures bounding the basin and its surroundings, as last 10 Ma. We predict the largest active magma well as the different terrains (early Hesperian lava reservoirs feed Olympus Mons and the Tharsis flows). Montes. An active magma chamber under Olym- Our preliminary results were presented during the pus Mons would explain the 2.4 Ma young lava First National Martian Seminar and the Second flows found on its western flanks. Planetary Mapping and Virtual Observatory This topic was described in the Annual Report Workshop. 2018. In 2019, a paper reporting our work was (P.-A. Tesson, D. Mège, J. Gurgurewicz, M. Ciążela, and J. Ciążela) Comparative planetology Investigation of friction weakening of terre- low as 0.1–0.2. No distinguishable difference is strial and Martian landslides using discrete observed between the behaviour of terrestrial and element models Martian landslides. Understanding what controls the travelling dis- This topic was described in the Annual Report tance of large landslides has been a topic of consi- 2018 and a paper presenting our work was derable debate. We show that the normalized published in Landslides (March 2019). runout distance starts to depend on the volume (T. Borykov, D. Mège, A. Mangeney, P. Richard, J. involved only above a critical slope angle > Gurgurewicz and A. Lucas) 16–19°, as observed experimentally. The em- pirical friction coefficient, calibrated to reproduce Nanotopographic characterization of micro- the observed runout of terrestrial and Martian fractures in rocks by Atomic Force Micro- landslides, is shown to decrease with increasing scopy landslide volume (or velocity), falling to values as Atomic Force Microscopy (AFM) records nano-

90 scale digital terrain models, making it possible to bases and their experiments. Three experiments carry out quantitative, nanoscale structural ana- with NIR and MIR reflectance spectra of tholins, lysis of rocks. AFM coupled with other techni- were released to the public. The SOSYPOL data- ques able to provide some mineralogical infor- base currently includes 18 experiments with over mation, such as Scanning Electron Microscopy, 250 spectra. has huge potential in this field, as it makes it Details of our work are available online at https: possible to put fracture nanotopography into //www.sshade.eu/db/sosypol (December 2019). context. (J. Gurgurewicz and D. Mège) Our work was described in the Annual Report The EXOMHYDR project website 2018, and a paper was published in the Journal of The EXOMHYDR website is updated monthly, Structural Geology (April 2019). and presents objectives, activities, people, and (J. Gurgurewicz, D. Mège, M. Skiścim and J. Pers) latest news from the FNP/ TEAM funded project EXOMHYDR – Magmatic plumbing systems The SOlar SYstem analogues database and tectonic control of hydrothermal activity on POLand (SOSYPOL) Mars revealed by ExoMars/TGO: constraints for The database content was described in the Annual life and resources. Report 2018. This year, new elements have been The website is online at http://exomhydr.eu added to the database infrastructure, which ena- (December 2019). bled the creation of the DOI for SSHADE data- (D. Mege and the EXOMHYDR team)

Earth Rotation and Geodynamical Studies (Department of Planetary Geodesy) In the first part of our work, we computed HAM Geophysical interpretation of polar from the newest (Release 6 – RL06) and older (RL05) GRACE solutions provided by different motion excitation data centres: the GeoForschungsZentrum (GFZ), Polar motion (PM) excitation functions-namely the Center for Space Research (CSR), the Jet Pro- atmospheric angular momentum (AAM), oceanic pulsion Laboratory (JPL), the Institute of Theo- angular momentum (OAM) and hydrological retical Geodesy and Satellite Geodesy (ITSG) of angular momentum (HAM)-describe the impact the Graz University of Technology, and the Cen- of variation in the mass redistribution of Earth's tre National d'Etudes Spatiales (CNES). Series surficial fluids on PM. We know that HAM is the were validated using so-called geodetic residuals main source of uncertainties in PM excitation. (GAO), obtained after removing AAM and OAM HAM can be estimated from either hydrological from GAM. Analyses were performed for sea- models, or observations of temporal variations in sonal and non-seasonal change, with a particular the gravity field, provided by the Gravity Reco- focus on spectral bands with periods of 1000– very and Climate Experiment (GRACE) mission. 3000, 450–1000, 100–450, and 40–100 days (Figs A common method to validate HAM measure- 52, 53). Our work found that the level of agree- ments is to compare them with the hydrological ment between HAM and GAO was a function of signal in observed PM excitation (Geodetic Angu- the frequency band, and was highest for decadal lar Momentum, GAM), derived from precise changes with periods of 1000–3000 days. The measurements of pole coordinates. biggest improvement in RL06, compared with In 2019, we continued our research into: 1) the RL05, was detected for the 100–450-day spectral evaluation of HAM from different GRACE band and for non-seasonal oscillations. solutions for various spectral bands; 2) an analysis In the second part of our work, GAO and HAM of retrograde and prograde circular terms in time series computed in the first phase were de-

HAM; and 3) the determination and evaluation of composed into prograde (χP) and retrograde (χR) HAM from temporal gravity field models circular terms by applying the Complex Fourier obtained from kinematic orbits of low-Earth- Transform. The obtained series were validated by orbit (LEO) satellites. comparison with GAO. We examined temporal

91 HAM and GAO variation in four spectral bands: MetOp-A, MetOp-B and Jason 2), as well as solu- seasonal, non-seasonal, non-seasonal short-term tions obtained from a combination of data from a (with periods shorter than 730 days) and non- few satellites. The validation was performed using seasonal long-term (with periods longer than 730 GAO, and conducted for seasonal and non-sea- days) (Figs 54, 55). Our general findings, arising sonal variations separately. The findings indicated from analyses of χP and χR terms, were consistent a large impact of orbital altitude and inclination with conclusions from the comparison of equa- on the accuracy of derived HAM. Orbit parame- torial components (χ1 and χ2) in HAM studies in ters MetOp-A, MetOp-B and Jason 2 were exclu- previous research. In particular, we showed that ded from further analyses as they provided much the new GRACE RL06 data increased the noisier solutions than other satellites. We showed consistency of different solutions, and improved that HAM series obtained from Swarm data were agreement between GRACE-based HAM and found to be the most consistent with GAO. Visi- GAO. For most of the oscillations considered, ble differences were found in HAM obtained best consistency with GAO was obtained for CSR from GRACE and Swarm orbits and those provi- RL06 and ITSG 2018 solutions. The study also ded by data processing centres. The main reasons revealed that both prograde and retrograde HAM for such differences were found to be different circular terms can be determined by GRACE, processing approaches and background models with similar levels of accuracy. used to develop gravity solutions. Our study In the third phase of our research, we evaluated demonstrated that the Swarm solution provided HAM computed from gravity field solutions by the Astronomical Institute of the Czech based on kinematic orbits of LEO satellites Academy of Sciences provided HAM series that (GRACE, Swarm, TerraSAR-X, TanDEM-X, were most consistent with geodetic observations.

Fig. 52. Comparison of changes in

χ1 and χ2 components of GAO and HAM functions for the period 450–1000 days. HAM+SLAM is a hydrological excitation function computed from the LSDM (Land Surface Discharge Model) hydrological model.

Fig. 53. Comparison of changes in

χ1 and χ2 components of GAO and HAM functions for the period 100–450 days. HAM+SLAM is a hydrological excitation function computed from the LSDM (Land Surface Discharge Model) hydrological model.

92 Fig. 54. Comparison of means and ranges between minimum and maximum

for χR and χP non-seasonal variation in HAM for old and new GRACE solutions. Time series of GAO and HAM from the LSDM model (with SLAM added) are provided for comparison.

Fig. 55. Correlation

coefficients of χR and χP parts of non-seasonal variation between GAO and HAM computed from GRACE solutions and the LSDM model (with SLAM added), and the percentage of variance in GAO explained by HAM functions. The critical value of the correlation coefficient for 25 independent points and a confidence level of 0.95 was 0.34. The standard error of the difference between two correlation coefficients for 25 independent points was 0.30.

Fig. 56. Correlation coefficients between seasonal changes of GAO and HAM obtained from ITSG 2018 GRACE solution and solutions based on kinematic orbits of satellites. As series were different lengths, we considered three periods: 2003–2013, 2011–2016 and 2013–2016. The critical value of the correlation coefficient was: 0.24 for 2003–2013, 0.34 for 2011–2016, and 0.50 for 2014–2016. ITSG solutions were provided by the Institute of Theoretical Geodesy and Satellite Geodesy at the Graz University of Technology, CAS solutions were provided by the Astronomical Institute, Czech Academy of Sciences.

93 Fig. 57. Correlation coefficients between non-seasonal change in GAO and HAM obtained from the ITSG 2018 GRACE solution, and solutions based on kinematic orbits of satellites. As series were different lengths, we considered three periods: 2003–2013, 2011–2016 and 2013–2016. The critical value of correlation coefficient was: 0.31 for 2003–2013, 0.37 for 2011–2016, and 0.50 for 2014–2016. ITSG solutions were provided by the Institute of Theoretical Geodesy and Satellite Geodesy at the Graz University of Technology, CAS solutions were provided by the Astronomical Institute, Czech Academy of Sciences. (J. Nastula, J. Śliwińska)

Comparative analysis of groundwater and total water storage in Poland

Fig. 58. Comparison of TWS time series derived from GRACE with those obtained from GLDAS (a) and CMIP5 models (b). Comparison of GWS time series derived from scaled wells with those obtained from GRACE-GLDAS (c) and GRACE-CMIP5 (d). All data relate to the Vistula basin. In 2019, our work focused on the analysis of va- GRACE observations, in-situ groundwater mea- riation in total water storage (TWS) and ground- surements at well stations, GLDAS (Global Land water storage (GWS) for the two main Polish river Data Assimilation System) hydrological models, basins, the Vistula and the Odra. Data came from and CMIP5 (the World Climate Research Pro-

94 gramme's Coupled Model Intercomparison Pro- GRACE-based TWS. The resulting GWS time ject Phase 5). The analysis was run for the period series were evaluated using in-situ well measu- September 2006 and October 2015. TWS tem- rements (Fig. 58c, d). Our results suggested that, poral variation was obtained directly from GRA- in general, there has been no noticeable increase CE data, and computed as the sum of soil moi- or decrease in TWS or GWS in Poland. Our ana- sture and snow water taken from four GLDAS lyses showed that, when comparing TWS series, (VIC, CLM, MOSAIC, and NOAH) and six better agreement with GRACE data was obtained CMIP5 (FGOALS-g2, GFDL-ESM2G, GISS- for GLDAS than for CMIP5 models. However, E2-H, inmcm4, MIROC5 and MPI-ESM-LR) the GWS comparison revealed that climate models (Fig. 58a, b). The model's TWS series were models were more consistent with well results. validated using GRACE estimates. We also com- (J. Śliwińska, M. Biryło, Z. Rzepecka, J. Nastula) puted GWS by removing the modelled TWS from

Study of 222Rn in the context of tectonic activity in the Świebodzice Depression orogen Researchers have devoted significant time and The CBK PAN's Geodynamic Laboratory is the effort to using radon (the 222Rn nuclide, in parti- only Polish, and one of the few European labo- cular) as a natural radioactive indicator of the va- ratories able to investigate subtle, geodynamic and rious geodynamic processes happening in the geochemical phenomena in tectonic areas. Our lithosphere. Its gaseous state, and relatively low laboratory is located in underground tunnels in chemical reactivity with the environment mean the Świebodzice Depression Unit. The location that radon is widely used to characterize gas ex- of the Świebodzice Unit was specifically chosen change between the lithosphere and the atmo- because of the dense network of faults, which sphere. Research has attempted to apply varia- separate both single blocks and neighbouring tions in 222Rn concentrations in soil, air, ground- geological units such as the Intra-Sudetic Basin water or other geofluids (e.g. crude oil, natural gas (the Struga Fault to the south), the Sowie Range or CO2 streams) to characterize and predict earth- Gneissic Block (the Szczawienko Fault to the quakes, volcanic eruptions and identify active west), the Fore-Sudetic Block (the Sudetic fault zones. Marginal Fault to the east), and the Kaczawa Metamorphic Complex (to the north).

Fig. 59. The AlphaGUARD instrument that measures 222Rn concentrations in the fault zone at Książ. The right-hand photo shows the one meter deep hole drilled in the fault zone, from which the atmosphere is pumped into the instrument's ionization chamber.

95

The Świebodzice Depression is filled with Lower empirically proven that CO2 plays an important Carboniferous and Upper Devonian deposits. It is role in radon transportation from Earth's crust mostly sedimentary rock, including conglo- into the atmosphere. Several hours before earth- merates composed of gneisses, migmatites and quakes, there is an increase in both CO2 concen- granites. These kinds of rock are rich in iron tration and radon activity. The two phenomena are hydroxides (magnetite and hematite) and uranium well-known earthquake precursors. In the case of oxides, which are particularly dense in a nearby the Świebodzice Depression mechanism, CO2 fault zone. The decay of uranium and tor radio- radon transportation is consistent with orogen nuclides are the source of radon in the atmo- kinematic activity (i.e. variation in compression sphere of the laboratory's underground corri- and extension phases). dors. As the density of monatomic radon gas is 3 Ongoing transformation processes, which alter- 9.73 [kg/m ] (about 8 times heavier than the den- nate between compression and extension, pump sity of Earth's atmosphere), radon molecules are out gases from pore spaces and rock fissures into much less mobile than statistic molecules in the the fault zone and the atmosphere of under- atmosphere. ground tunnels. This characteristic is relevant in explanations of Compression–extension sequences are deter- the transportation mechanism of heavy radon mined on the basis of observations of orogen molecules from rock crevices and faults. The half- 222 kinematic activity. These observations are provi- life of the most stable radon isotope ( Rn) is ded by two water tube tiltmeters in the Ksiaz labo- short (3.8224 days), and the process of trans- ratory. Plots of two year series (18 May 2014 to 18 portation ought to be fast enough. It has been January 2016) of four tectonic activity functions

Fig. 60. Two year series (18 May 2014 to 18 January 2016) of multi-plots of four tectonic activity functions from two water tube tiltmeters and changes in 222Rn concentrations registered by five SRDN-3 probes. Bq [one decay/sec] measures the amount of decay as cubic metres per second.

96 from the two tiltmeters, and changes in 222Rn sphere occurs not only through fault zones, but concentrations registered during this time by five, also through all of the underground surfaces: SRDN-3 probes are shown in Figure 60. During floors, sidewalls and roofs. Second, the high con- this time, we observed the relationship between cordance between radon channels confirms the 222Rn activity and variation in orogen tectonic thesis of the existence of a large-scale, homo- activity registered by the tiltmeters. geneous field of stresses that stimulates kinematic Our analyses of variations demonstrated the spa- activity in the whole Świebodzice Depression tial character of changes in 222Rn activity (Figure massif. The problem of the existence of a large- 61). For all measured channels, variation over time scale, well-approximated homogeneous field of was very comparable in all parts of the under- tectonic forces was presented in the CBK PAN ground laboratory. This interesting result sug- Report 2017 (p. 102) and 2018 (p. 92) in the gests two, important conclusions. First, gas context of the seismicity of the Fore-Sudetic migration between the lithosphere and the atmo- Monocline, Upper Silesian and Czech Massif.

Fig. 61. Comparison of plots of variation in radon concentration registered by five gauges in the Książ Laboratory from 17 May to 30 June 2014. (M. Kaczorowski, T. Przylibski, L. Fijałkowska-Lichwa, D. Kasza, R. Zdunek, M. Rudnicki, R. Wronowski, M. Gadomski)

Accelerometers and Inter-Satellite Links in Orbit Determination In 2019, the Centrum Badań Kosmicznych PAN Investigations are now continuing on using new successfully finalised the GalAc project. This types of measurements for orbit determination. project aimed to analyse the feasibility and use- Accelerometer data can be used to directly mea- fulness of equipping second-generation Galileo sure the unmodelled effects of nongravitational spacecraft with accelerometers to improve the perturbations and spacecraft acceleration due to accuracy of the Precise Orbit Determination. on board activity. At the same time, it makes it

97 possible to correct existing empirical models. In parallel, we are carrying out analyses of Inter- Satellite Links (ISL) as this can significantly enhance the orbital solution. ISL provides precise range and range rate measurements (unaffected by the atmosphere) between satellites in a specific constellation, which is one of the key require- ments for improving the reliability of positioning and time transfer. It may also make a significant contribution to on board data processing and could be a step towards autonomous GNSS con- stellations. Our work pays special attention to the analysis of the behaviour of different constellation geo- metries (Galileo and GPS), and links between sa- Fig. 62. Simulated Galileo constellation with Inter-Satellite tellites in various conditions. The outcomes of Links. our investigations include a reduced number of the European Space Agency's Galileo project. It ground stations, more accurate ISL, and a greater has resulted in the development of a bespoke total number of ISL measurements. Another software package that combines recent theory, outcome is significant improvement in the accu- models and data to perform realistic simulations racy of determined orbits and estimated clocks. of GNSS satellites in orbit. We anticipate that the Finally, our research also looked at combining core features of this software will be updated, pa- GNSS and ISL measurements based on weighting ving the way for more advanced GNSS data pro- methods in the context of the least squares cessing, notably near-real-time analyses of obser- approach. Variance Component Estimation was vations and verification of modern techniques analysed with the aim of reducing the influence that can potentially be used in next-generation of systematic errors on the orbit and clocks. positioning and navigation systems. Our research is a key element in the evolution of (T. Kur, M. Kalarus)

SPACE MECHATRONICS (LMRS-Space Mechatronics and Robotics Laboratory) Formation of vesicles within the fusion crust of eucritic meteorites Cosmic objects entering a planetary atmosphere of eucrite meteorites (achondritic stony meteo- reach a very high temperature, as a result of hy- rites of basaltic composition, likely originating pervelocity collisions with air molecules. The from asteroid Vesta-4) by means of microscopic outermost part of these objects completely melts observation, laboratory experiments and nume- and, during cooling, is transformed into a glassy rical modelling. This study will improve our layer, usually between 100 mm and 1000 mm understanding of the interaction of bolides with thick, named the fusion crust. The most chara- the atmosphere, and determine the amount of cteristic feature of stony meteorites' fusion crust volatiles delivered to past and present atmo- is vesicles, which, in microscope images, look like spheres of terrestrial planets by cosmic particle round, empty objects with different size and flux. density. There is a hypothesis that they are formed In order to determine the vesicle formation me- by exsolution of volatile components from the chanism it is necessary to quantitatively determine silicate melts due to high temperatures. the 'level of vesicularity' of the fusion crust. To The aim of this project is to explain the mecha- do this, we have developed Matlab code to iden- nism of vesicle formation within the fusion crust tify vesicles on SEM images and automatically

98 calculate simple statistics (their number, size, guished automatically using the steps presented in percentage area, etc.). Figure 63. The final algorithm is able to quanti- The first step of the algorithm is to determine the tatively determine the level of vesicularity of the boundary of the fusion crust. In SEM images, this fusion crust of the meteorite PCA91007.32 (Figu- boundary is not easy to trace, but it can be distin- re 64, Table 2).

a) b) c)

Fig. 63. a) Select pixels from the melted zone and record their value, b) Find areas with a higher density of pixels within a specific range of values, c) Define the boundaries of areas with a high density of pixels, d) Select the fusion crust area and separate it from the picture for further analysis. d)

Fig. 64. Boundary of the fusion crust (red line) and vesicles (blue points) of the meteorite PCA91007.32, identified by our new Matlab code.

Table 2. Statistical analysis of the vesicles in the fusion crust of meteorite PCA91007.32.

The next step of this project will be to determine the chemical (notably, isotopic) composition of meteorites using different analytical techniques in order to identify the extra-terrestrial matter transfor- mation. (A. Nicolau-Kuklińska)

99 Mathematical model of a landing on Phobos – the LOOP project In 2017, the CBK PAN formed a consortium with laboratory microgravity simulations and mathe- the Akademia Górniczo-Hutnicza (AGH), and matical modelling. The AGH is a pioneer in the submitted a proposal for a project to develop a field of geology, mining, geophysics and engi- mathematical model of a landing process in the neering in general. We believe that the synergy context of the Polish Industry Incentive Scheme. between these two entities is the key to the success The proposal was accepted and, at the end of of the proposed project. 2017, the LOOP project was launched. In 2018, the LOOP team conducted an extensive literature review in order to define requirements for future modelling and testing. The next step was to de- sign, manufacture and test two testbeds: the FBT (Falling Box Testbed) and the FCT (Falling Cone Testbed). Efficient landing algorithms and lander mecha- nical designs are going to be a key element in the success of any future space endeavours. In the scope of past, ongoing and proposed landing missions it is apparent that the landing process itself is crucial for the entire project to succeed. There is no doubt that missions such as Pho- otprint have much to gain from the outcomes of this project, which we have named LOOP (Lan- ding Once On Phobos). The origin of the name lies in the fact that, while working on the REST project (Robotically Enhanced Surface Touch- down, part of the Phootprint mission) the team realised that the empirically-validated mathe- matical model of the contact would be a valuable tool in various projects concerned with landing processes. Such a model should, in our opinion, be developed hand-in-hand with its counterpart in the form of a full laboratory model. As the initial idea derived from a project concerned with landing on Phobos, this tiny celestial body has given its name to the proposed activity. Although the overall project is focused on Phobos, our results will serve the general purpose of landing on other celestial bodies. The mathematical model that we have developed will be adapted to serve two engineering purposes – one is the creation of a simplified engineering Fig. 65. Falling Box Testbed. model that should be easy to implement in the overall control system – and the other will take the In 2019 two devices – the Falling Box Testbed form of a ready-to-use simulation tool in the (microgravity conditions) and the Falling Cone MATLAB/ Simulink environment. Testbed (vacuum condi-tions) – were successfully The project's staff consists of a variety of commissioned by the European Space Agency. specialists from two leading scientific facilities. They will be used in a test campaign planned for The CBK PAN possesses broad experience in the beginning of 2020. (T. Barciński, J. Baran, J. Musiał, A. Sikorski, K. Aleksiejuk)

100 APPLICATIONS

EARTH OBSERVATIONS The Earth Observation Division (ZOZ) of the senting various bio-geographical regions of CBK PAN specializes in remote sensing and Europe. According to rules established in the first geographic information systems. Our Group has part of the project, training samples were derived been active in various European projects (e.g. the from existing LC databases – CORINE LC and 7th Framework Programme, H2020 and ESA High Resolution Layers. The selection of training programmes), as well as domestic research. The samples was enhanced by the introduction of ad- ZOZ is also developing innovative applications, ditional filtration rules between selected databases software and algorithms. and the use of spectral indices (NDWI and NDVI). Additionally, workflow rules for the sele- Sentinel-2 Global Land Cover classifi- ction of time series images were established; these cation rules assume the processing of approximately 20 images, per Sentinel-2 tile, representing all sea- Duration: 1 February sons. The post-processing approach was also mo- 2016 – 31 January 2018 dified and adjusted to fit the European landscape. Continuation: 1 May 2018–30 April 2019 All classifications were carried out on the CREO- DIAS platform. This required the adaptation of The European Space Agency's Sentinel-2 Global all of the previously-created S2GLC algorithms Land Cover (S2GLC) project ran from 2016– to the CREODIAS computing environment. 2019. It was divided into two parts: Over fifteen thousand Sentinel-2 images, Part 1: Development of land cover (LC) representing 815 Sentinel-2 tiles, were processed classification on a global scale (2016–2018). to map the selected area of Europe. The final map was validated using a large dataset of 52 000 Part 2: LC classification of Europe (extension randomly-distributed samples representing 55, of the project) (2018–2019). Sentinel-2 tiles spread across Europe. The The goal of Part 1 was to develop a classification distribution of these tiles made it possible to methodology that could be used for global LC validate the results at both European and country mapping based on Sentinel-2 images. The pro- level. The overall accuracy (OA) of the complete cedure we developed was tested on five areas map, with 13 LC classes, was estimated to be over located in different geographical regions of the 86%. However, as results were poorer for some world. Two were located in Europe (the whole of classes (e.g. grasslands and moors), we merged Germany and Italy), and the other three repre- selected vegetation classes. Although this reduced sented similar areas in China, Columbia and Na- the number of LC classes to 10, OA increased to mibia. Satellite images and auxiliary data were 89%. Country-level accuracy was found to be very processed using dedicated software developed by good, with OA exceeding 80% for the majority of the CBK PAN. countries. The S2GLC classification map of The main objective of Part 2 was to verify the Europe for 2017 is presented in Figure 1. operability of the methodology developed during In general, the continental-scale classification Part 1. This was done by performing LC classifi- confirmed the effectiveness of the S2GLC tool at cation over a large part of the European conti- global/ regional scale. The methodology can nent, based on the CREODIAS infrastructure. automatically generate new editions of European The developed methodology was adjusted to the Land Cover maps at 10 m resolution every year. European landscape and all processes were fully The S2GLC LC map for Europe 2017 was pre- automated. sented at the European Space Agency and Euro- The adaptation of the classification method, in- pean Commission stand during the GEO summit cluding modifications to the legend, was based on in Canberra (November 2019). More information tests conducted on selected Sentinel-2 tiles repre- can be found at the S2GLC project website: http://s2glc.cbk.waw.pl.

101 Fig. 1. The S2GLC LC classification of Europe for 2017.

(St. Lewiński, R. Malinowski, M. Rybicki, E. Gromny, M. Jenerowicz, M. Krupiński, C. Wojtkowski, E. Bilska)

102 BAMS-Mazovia – Build-up Areas Monitoring Service for Mazovia Duration: 18 September 2018–17 September testing phase. Its outcomes will be subject to a 2020 detailed assessment based on a comparison with The BAMS-Mazovia project aims to develop a up-to-date orthophotomaps and field surveys. service platform that provides continuous infor- Once the results of the building classification are mation about newly-detected changes in a set- verified, the service workflow will be imple- tlement network. Regional authorities that are res- mented. ponsible for, inter alia, maintaining and updating In the next phase of our work, the service plat- topographic maps, were identified as the main form will be used to perform spatial analysis that end-user of the service. The project consortium compare the building classification results with consists of GEOSYSTEMS Polska Sp. z.o.o. existing databases (e.g. the Database of Topogra- (project leader) and the Earth Observation Divi- phic Objects [Baza Danych Obiektów Topografi- sion of the Centrum Badań Kosmicznych PAN cznych]). This comparison will enable automatic (research partner). identification of changed areas. The goal is to ac- The service, which is currently being developed celerate the process of updating existing data- uses multitemporal, Sentinel-2 satellite imagery to bases and reduce maintenance costs. The project's detect buildings using highly-automated classifi- case study is based on the area of the Mazovia cation algorithms. The classification workflow, Province, Poland. Ultimately, the service will be which was developed by the CBK PAN, is in the applicable to other provinces in Poland.

Fig. 2. Examples on new biulding detection - Warsaw, Poland.

(R. Malinowski, S. Aleksandrowicz, M, Jenerowicz, M. Rybicki, St. Lewiński, C. Wojtkowski, M. Krupiński)

ACCESS4FI: Automated Crop Classification and yield Estimation online ServiceS for the Food Industry Duration: 15 January 2019–14 January 2021 In 2019, we carried out a systematic and compre- The ACCESS4FI project addresses the challenge hensive analysis of the characteristics of both of the quantification and annual monitoring of SAR and optical remote sensing data (Sentinel-1 agricultural production, from the perspective of and Sentinel-2). Activities included the definition different actors in the agriculture sector. The main and extraction of features in order to develop a objective is to develop a set of user-dedicated fully-utomted method to classify selected crop EO-based tools, namely: types. We evaluated several features that, poten- - an automated crop recognition and clas- tially, could be used in the classification of a speci- sification tool; and, fic crop for a multi-temporal series or the year - an automated, per crop-field, yield 2018 Tests were based on he Polish province of estimation tool. Wielkopolskie Voivodeship. Theyfocused on a

103 combination of spectral values and bands (or a intermediate aim of the analysis is to optimize the pixel-based approach in the case of optical data), classification algorithm and reduce the number of and on the oherence of matrix elements, band inputswithout losing accuracyby selecting the best combination and entropy, and arameters (or a possible features. pixel-based approach in the case of AR data) The (M. Jenerowicz)

Evaluation of the usefulness of multifractal formalism in the processing and analysis of optical remote sensing images Duration: 20 July 2017–19 July 2020 images. The multifractal formalism was applied to The scientific goal of is to analyse optical remote evaluate the scope of applicability of multifractal sensing images using an advanced multifractal features in the image classification domain. The formalism. In 2019, we carried out a systematic results showed that the multifractal parameter, and comprehensive analysis of the multifractal calculated for all conidered scenes, increased for characteristics of different kinds of optical remo- compact structures. The results of this study were te sensing images. In particular: published in the Proceedings of the 2019 IEEE - we ran a preliminary comparison of two International Geoscience and Remote Sensing methods that are based on the mathematical Symposium doi: 10.1109/IGARSS.2019.8898588 approach: Mathematical Morphology and the - we developed a multifractal approach to au- Local Multifractal Description. Tests were tomating information extraction regarding Inter- performed based on selected Brodatz textures nally Displaced Persons/ refugee camps, and exa- and artificially-generated noisy images. Thee tests mined its potential and limitations. Our case study aimed to identify the strengths and weaknesses of used multifractal features to determine the extent the two methods when applied to edge/ object of camps in Kenya and Sudan. The results detection tasks. The results were presented at te showed that the multifractal methodology can be Summer XLIV IEEE SPIE Joint Symposium on usefully applied to an analysis of camp growth, Photonics Web Engineering, Electronics for and help to make a rough, but rapid estimation of Astronomy and High Energy Physics Expe- their extent. This study was published in the riments Wilga 2019 published in the SPIE IEEE Journal of Selected Topics in Applied proceedings doi: 10.1117/12.2536408 Earth Observations and Remote Sensing, doi: - we described a complex terrain based on 10.1109/JSTARS.2019. 2950970 multifractal features. The analysis was run for two These studies were carried out under Opus samples of Internally Displaced Person refugee project no. 2016/23/B/ST10/01151, funded by camps (Ifo and Daadab in Kenya, and Al Geneina the Polish National Science Centre. in Sudan). In both cases, information was derived (M. Jenerowicz, A. Wawrzaszek) from very high resolution panchromatic satellite

Night sky pollution over Warsaw Light pollution can be defined as a situation where set up at the CBK PAN, which is equipped with a “organisms are exposed to light in the wrong sky quality meter (SQM). In 2019, we published place, at the wrong time or at the wrong intensity”, the results of the very first, long-term photome- “an unintended result of electric lighting”, or “an tric survey of NSB over Warsaw. The study cove- excessive or obtrusive artificial light caused by bad red 636 nights between 2014 and 2016, including lighting design”. It has been recognized as one of 475 astronomical nights. the most widely-distributed forms of anthro- Data were collected for all-weather conditions, pogenic pollution, and threatens both biodiversity hence our analyses accounted for clouds (fraction, and human health. One of the most popular indi- base height, layer height), vertical visibility, and cators is known as night sky brightness (NSB), solar and lunar illumination. Furthermore, and which is measured with photometric techniques. also for the very first time, two cloud data sources A dedicated NSB photometric station has been were investigated simultaneously – surface-based

104 observations collected at a meteorological station During the astronomical night, clouds amplified (SYNOP), and satellite-based observations col- NSB by a factor of seven; NSB increased with in- lected by the Meteosat cloud imager. creasing cloud base height and cloud fraction 2 The results of the study showed that average NSB (~0.2 magSQM/arcsec per every 10% of cloud frac- over Warsaw, at the darkest moment of a clou- tion). Our study suggests that analyses based on dless, moonless astronomical night was 18.65± low cloud and low cloud fraction conditions sho- 2 0.06 magSQM/arcsec , which is 15 times higher than uld not use SYNOP-like data, as the mismatch be- an unpolluted sky. This value agrees well with esti- tween the SQM's and observer's fields of view in- mations published in The new world atlas of artificial troduces ambiguities into the data interpretation. night sky brightness. In fact, the average Warsaw Our work has shown that satellite data can be used night was so bright that the phase of the Moon as an alternative to traditional, visual surface-ba- had no effect. Although Sun elevation above the sed observations. When used to derive average horizon was the most important factor influen- NSB, satellite-based cloud estimates result in sta- cing NSB, it became irrelevant when it was 12° tistics that are almost the same as those based on below the horizon. Clouds dominated when the SYNOP information. Sun was ~5° below the horizon. Our study sug- The details of our work were published in an gests that the critical solar elevation angle (i.e. article titled Night sky photometry over Warsaw when the elevation of the Sun becomes irrelevant, (Poland) evaluated simultaneously with surface-based and or when clouds become the dominant factor) can satellite-based cloud observations, which was published in be used as a quantitative measure of light pollu- the Journal of Quantitative Spectroscopy and Radiative tion intensity. Transfer.

Fig. 3. Nighttime imagery of Warsaw taken by an astronaut onboard the International Space Station. Photo: CBK PAN / NASA.

(A. Z. Kotarba)

105 Land cover change detection and classification using very-high-resolution satellite images Automatic change detection is one of the main thods. Images are segmented, and the resulting topics in the field of remote sensing. In 2019, our objects are classified into “change” or “no-chan- work focused on developing a workflow (Fig. 4) ge” classes based on the χ2 layer. “Change” objects for the analysis of bi-temporal images. The are then classified into sub-classes using pre- method we have developed makes it possible to defined rules. In the last stage, false positives (cau- accurately detect and classify changes based on sed by phenological changes in agricultural fields) unsupervised method. are removed. In the first phase, both images were pre- Our tests show that the proposed method is processed. Here, the aim was to eliminate false accurate and provides a high level of automation. positives due to radiometric changes caused by Image pair processing does not require parame- differences in image data collection. A key role in ters or thresholds to be set. It also does not require this part plays the atmospheric correction pro- training samples. Change classification rules can cess. We convert units from digital numbers to be extended based on the results from test data. reflectance values as this enables an initial classi- Our algorithm was developed using a pair of fication of pixels into spectral categories that are WorldView-2 and GeoEye-1 images from the later used for change classification. In the next county of Niepołomice, in Poland. The algorithm phase, images are subject to a Multivariate Altera- was tested on two pairs of WorldView-2 images tion Detection (MAD) analysis, which identifies of the area of Warsaw. Our results confirm the MAD layers and the change probability layer χ2. high accuracy of change detection (up to 89% MAD layers, together with pre-processed image overall accuracy) and of change classification (up data are then analysed using object-based me- to 84%).

Fig. 4. Proposed workflow for change detection and change classification. (S. Aleksandrowicz)

106 The CRISIS INFORMATION CENTRE The mission of the Crisis Information Centre vices and crisis management institutions re- (CIK) is to make rescue operations and crisis ma- garding the use of geoinformation and sa- nagement activities more efficient through the tellite applications; effective use of existing geospatial information • providing geoinformation support to the technologies, and the development of new me- State Fire Service, Polish crisis management thods and tools – in particular, satellite-based ap- institutions and non-governmental organi- plications and the organisation of demonstra- sations; tions and training focused on new solutions. • organising training and simulations focused The CIK combines scientific expertise in the field on the effective use of new technologies; and of satellite applications with an end-user per- • demonstrating and testing the usefulness of spective. The CIK's operational activities include: pre-operational technical solutions via table • providing expert advice to Polish rescue ser- top and field exercises.

DRIVER+ Duration: 1 May 2014 – well as organising the DRIVER+ Final Demon- 30 April 2020 stration. In 2019, two trials were held. Trial 3 was run in DRIVER+ (DRiving InnoVation in crisis mana- Austria on 12–15 September. This scenario was gement for European Resilience +), which is fun- th focused on the consequences of an earthquake ded under the European Union's 7 Framework and subsequent heavy rain. Trial 4 was run in the Programme, is the largest collaborative crisis ma- Netherlands on 22–23 May and concerned an nagement project in the security domain. It brings extremely high coastal tide that coincided with an together 31 partners from 14 countries. expected storm. The Final Demonstration took The main aims of the project are to: place in Warsaw and the Hague on 27–28 Novem- 1. Develop a pan-European Test-bed for ber. This large-scale, forest fire scenario was used Crisis Management stakeholders: to assess how much the newly-developed solu- - develop a common Guidance Methodolo- tions can contribute to situation assessment and gyan tools that support testing (Trials) and the information exchange among team leaders in Eu- consolidation of lessons learnt, ropean Union Civil Protection (EUCP) Modules, - develop an infrastructure to create rele- the EUCP Tea and the Emergency Response Co- vant environments, to enable Trials of new ordination Centre (ERCC). solutions and explore and share Crisis Mana- During the Final Demonstration, the CBK PAN gement capabilities, and DRIVER+ signed a joint declaration on the - run Trials in order to assess the value of establishment of the Centre of Expertise within solutions that address specific needs using the Crisis Information Centre. As a Centre of guidance and infrastructure, Expertise, the CIK at the CBK PAN will continue - ensure the sustainability of the pan- to act as a practitioner-centred organisation and – European Test-bed. whenever relevant and possible – as an inter- 2. Develop a well-balanced, comprehensive mediary between research organisations, solution Portfolio of Crisis Management Solutions. providers, public administration at all levels and 3. Facilitate a shared understanding of Crisis policymakers in the crisis management domain, Management across Europe. with a particular focus on the use of drones and The Crisis Information Centre is responsible for geoinformation. overseeing the preparation and execution of four More information is available on the project's rials that aim to evaluate the guidance metho- website: http://www.driver-project.eu/. dology developed under the project, and to assess (A. Foks-Ryznar, A. Dembińska, A. Gadawska, new solutions for crisis management operations A. Nałęcz-Kobierzycka, J. Ryzenko, in conditions that are as realistic as possible, as K. Trzebińska, J. Tymińska, E. Wrzosek)

107 Sat4Envi The Mobile Centre for Satellite Data Analysis is equipped with hardware and software that ena- Duration: 1 December 2017 – 30 bles the effective and efficient use of digital satel- November 2020 lite data in emergency rescue management, in a location chosen by the user. It is staffed by the Mobile Support Team, who are specialised in The CBK PAN is a member of the project using satellite data and advanced data processing. consortium “The operating system for collecting, In 2019, there were 23 activations resulting in the sharing and promotion of digital satellite infor- generation of over 800 GB of data related to 310 mation about the environment (Sat4Envi)”, information products. Activations were proces- which is a cooperative endeavour with the Insti- sed upon request from MC Users. tute of Meteorology and Water Management – The CBK PAN is also focused on the develop- National Research Institute, the Academic Com- ment and implementation of a Training Program puter Centre Cyfronet AGH, and the Polish Space for statutory users in the field of crisis manage- Agency. The intended end-users of the project's ment and rescue operations, including the acquisi- outputs are security sector units, including entities tion, analysis and use of satellite data. The pro- competent in crisis management, rescue and civil gram is based on eight, thematic modules that re- protection, non-governmental organisations and flect the individual needs of user communities at other entities working in public security. national, provincial and local levels. These modu- CBK PAN researchers are focused on four main les cover the basics of satellite remote sensing, tasks: setting up the Mobile Centre for Satellite operational capabilities and the functionality of Data Analysis (MC); creating the Mobile Support the MC, as well as the editing and processing of Team; preparation and implementation of a data in GIS systems. In 2019, 12 training sessions training program; and support for users of the were conducted. Customer Services System. The project is funded under the Operational Programme Digital Poland 2014–2020.

Fig. 5. Exercises organised by the Silesian Voivodeship Crisis Management Centre, held on 6 November 2019.

(W. Hodowicz, T. Borkowski, K. Dąbrowska, M. Milczarek, A. Dembińska, J. Ryzenko, A. Foks-Ryznar, E. Wrzosek, E. Woźniak, M. Krupiński)

108 The Heliogeophysical Prediction Service Centre The Heliogeophysical Prediction Service Centre of the European web service, provides online (HPSC) is part of the global International Space access to a database of critical frequency F2 iono- Environment Service (ISES). It is responsible for spheric layer forecasts for all sites. Continuous measurements and predictions of solar activity nowcasting of regional ionospheric conditions and related Earth phenomena. over Europe, East Asia and Australia is also avai- The ISES is an international organisation that lable. The HPS Centre provides the W-index over coordinates the rapid exchange of parameters Europe based on European Geostationary Navi- concerning the Sun, the Earth and the Earth's gation Overlay Service ionospheric maps obtai- environment between participating observatories. ned from global navigation satellite system The Warsaw centre has a special status as a (GNSS) measurements. The same analysis can be Regional Warning Centre (RWC). The CBK PAN obtained using data from the Russian System for exchanges data with other Warning Centres, and Differential Corrections and Monitoring mes- receives large amounts of data from national sages via GNSS observations. This will make it observatories in different countries. Data from possible to show plasma flow from the eastern Polish observatories are also collected. Together region, which can be used as a fast warning for with the Geophysical Institute of the PAN, the Polish GNSS users. Warsaw Centre supplies data from the polar In 2019, we carried out an analysis of the region (provided by the Polish Polar Station in correlation between GNSS TEC and foF2 for Hornsund). Ionosonde data is completed by rio- operational purposes used in several projects. meter and scintillation measurements. A special Statistical approaches such as KNN were used to daily bulletin (URSIGRAM Warsaw) is published build foF2 maps from Ionosondes. The results of and broadcast to ISES members. this research have been used to create a new The Ionospheric Despatch Centre, which is part service for civil aviation users. PECASUS The Pan-European Consortium for Aviation MOD) and 50% (severe depression, HF COM Space WeAther User Services (PECASUS) SEV). initiative aims to develop a global space weather As a result of negotiations between three global information centre (SWxC), as specified by the space weather centres for ICAO it was decided to International Civil Aviation Organisation not calculate maps of foF2 or MUF(3000), and (ICAO). The countries forming the PECASUS instead compare depression parameters with 30- consortium are Finland (Lead), Belgium, the day medians. We decided to use foF2 as the main United Kingdom, Poland, Germany, the Nether- parameter as it is most accurately scaled from lands, Italy, Austria, and Cyprus. PECASUS will ionograms, and its databases are more complete in provide the civil aviation with information on comparison with MUF(3000). We are currently space weather that has the potential to affect using the median value of foF2 for the previous communications, navigation and the health of 30 days, estimated for the specified ionosonde, passengers and crew. The consortium was audited together with concrete time as background para- in February 2018 by space weather and opera- meters to calculate the depression. If the number tional management experts nominated by the of numerical foF2 values for the specified iono- World Meteorological Organisation (WMO). sonde is less than 20 for the past 30 days, the me- The CBK PAN provides products related to dian calculated from data in the NeQuick model is changes in high-frequency communication and used instead of the ionosonde location. provides advisory support for users. In the frame- Nowcast maps of warnings, coverage and depres- work of PECASUS activity, we have developed sions are sent in near-real-time in JSON and PNG and implemented techniques for building foF2 formats to the Solar-Terrestrial Centre of Excel- global nowcast maps, as well as global maps of lence (STCE) where the PECASUS control office foF2 depression and warnings about depressions is located. Examples of maps sent to the STCE over 30% (moderate depression, HF COM dashboard are shown in the following two figures.

109 Fig. 6. foF2 depression map.

Fig. 7. foF2 warnings map.

Fig. 8. Lowest usable frequency (LUF) in response to the solar flare model developed by the HPSC. Example for LUF estimated at the level - 5 dB as a result of the X8.2 Solar flare that took place at 16:47 p.m. UT on 10 September 2017.

110 Maximum usable Frequency - model developed in HPSC. It is example of the map calculated.

Fig. 9. Maximum usable frequency model developed by the HPSC. This is an example of a map calculated in the framework of the NeQuick model, corrected with actual ionosonde data.

The CBK PAN's ionosphere model In 2018, the CBK PAN's assimila- ted ionosphere model Helgeo2PT (H2PT) became operational, and has been used as a source of total electron count (TEC) maps for GALILEO monitoring. The mo- del includes global navigation sa- tellite system observations, bot- tom vertical and, if possible, oblique sounding. The H2PT is an empirical model, which means that TEC maps are restricted by data availability and mapping function efficiency. In 2019, the stability and performance of the model were improved by the deve- lopment of a new database sche- ma in the MongoDB environ- ment. Fig. 10. Sample TEC map generated using the H2PT model.

The Ionospheric Weather Expert Service Centre

The Ionospheric Weather Expert Service Centre upper atmosphere weather conditions. Within the provides support to the European Space Agency's framework of the Agency's 'Ionospheric Weather' Space Situational Awareness Space Weather project, the HPS Centre hosts two services – SRC Segment (SSA SWE) network, notably in the form SGIArv and SRC RIO. The current version is of the observation, monitoring, interpretation, being updated to meet users' needs. modelling and forecasting of ionospheric and

111 Fig. 11. Screenshot of the European Space Agency's SRC SGIArv service.

Other projects and activities Within the framework of the EUROPLANET RI compared to Warsaw ionosonde data and H2PT H2020 project, RWC Warszawa began issuing TEC output. warnings using VOEvent technology. The histo- The HPSC provides specific products and rical databases of RWC Alerts can still be acces- expertise to the Polish National Radio Frequency sed via the VESPA service. Agency, power grid operators and other Polish In the context of the Galileo Monitoring project, government institutions about the various effects the HPSC produces quarterly reports of Galileo of Space Weather on technical infrastructure. single frequency ionospheric model performance (Ł. Tomasik)

The Global Navigation Satellite System (GNSS) Observatory in Warsaw MONITORING THE QUALITY OF THE GALILEO SYSTEM Since autumn 2018, the CBK PAN has been parti- cise orbits for Galileo satellites, cipating in the Global Navigation Satellite Sys- - computation of independent ionospheric tems Agency (GSA) project known as the Galileo models for different world regions, Reference Centre-Member States. This project is - computation and monitoring of Key designed to enable monitoring of the Galileo sys- Performance Indicators, tem by research institutes from European Union countries, independent of the system manager. - computation and analysis of the NeQuick-G The main tasks are: model, which is broadcasted as an ionosphere model in the Galileo navigation message. - computation of independent rapid and pre-

112 Fig. 12. Example of results from the analysis of the Galileo SISE and PDOP<6 for July and August 2019.

Fig. 13. Example of analysis results: a Horizontal and Vertical position error performed for the E1 Galileo frequency over the third quarter of 2019. (A. Świątek, L. Jaworski, Ł. Tomasik, M. Pożoga)

113 MONITORING THE QUALITY OF EGNOS CORRECTIONS The CBK PAN is one of the consortium partners cess Service) corrections. The project includes in the GSA's EGNOS Service Performance Mo- analysis and visualization of Key Performance In- nitoring Support scheme. This project performs dicators (KPI) of the EGNOS system, and a com- continuous monitoring of the availability, correc- parative analysis of EGNOS corrections trans- tness, continuity and accuracy of EGNOS-SIS mitted directly by satellite and via the internet. (Signal in Space) and EGNOS-EDAS (Data Ac-

Fig. 14. Example of a visual analysis of EGNOS Signal in Space corrections at the Warsaw site.

Fig. 15. Horizontal and Vertical Position Error in SIS and EDAS data over the last seven quarters.

114 Fig. 16. Horizontal and Vertical position differences for SIS and EDAS data over the last seven quarters. (A. Świątek, L. Jaworski, Ł. Tomasik)

115 PUBLICATIONS

* Total number of publications in 2019: 121 (including 61 in the journals from JCR/Ministerstwo) * Papers in refereed international and national science journals, books, and proceedings: 60

Papers in refereed international and national 4. Bergeot, N., O. Witasse, S. Le Maistre, P. - L. science journals and proceedings (JCR): Blelly, W. KOFMAN, K. Peter, V. Dehant, J. - 1. Acharyya, A., K. SEWERYN and other 480 M. Chevalier; MoMo: a new empirical model of the authors; Monte Carlo studies for the optimisation of Mars ionospheric total electron content based on Mars the Cherenkov Telescope Array layout; Astropar- Express MARSIS data; Journal of Space Wea- ticle Physics, Volume 111, Pages 35-53, DOI: ther and Space Climate Volume 9, Issue 1, 10.1016/j.astropartphys.2019.04.001, 2019 Article number A36, DOI: 10.1051/swsc/ 2. Bąk-Stęślicka, U., S. E. Gibson, M. STĘ- 2019035, 2019 ŚLICKI; Thermal Properties of Coronal Cavities; 5. Bogusz, J., A. BRZEZIŃSKI, J. NASTULA, Solar Physics, Volume 294, Issue 11, Article Research on Earth rotation and geodynamics in number 164, DOI: 10.1007/s11207-019- Poland in 2015–2018, Geodesy and 1554-z, 2019 Cartography, Vol. 68, No. 1, 2019, pp. 65–86 3. Baranets, N., Yu. Ruzhin, V. Dokukin, M. DOI: 10.24425/ gac.2019.126094, 2019 Ciobanu, H. ROTHKAEHL, A. KIRAGA, J. 6. Borykov, T., D. MÈGE, A. Mangeney, P. Ri- Vojta, J. Šmilauer, K. Kudela; Injection of 40- chard, J. GURGUREWICZ, A. Lucas; Empi- kHz-modulated electron beam from the satellite: II. rical investigation of friction weakening of terrestrial Excitation of electrostatic and whistler waves; and Martian landslides using discrete element models; ADVANCES IN SPACE RESEARCH DOI: Landslides, Volume 16, Issue 6, Pages 1121-11 10.1016/j.asr.2019.08.027, 2019 40, DOI: 10.1007/s10346-019-01140-8, 2019

116 7. Bouche, J., S. Bauduin, M. Giuranna, S. Ro- 14. Desai, M. I., M. A. Dayeh, F. Allegrini, D. J. bert, S. Aoki, A. C. Vandaele, J. T. Erwin, F. McComas, H. Funsten, J. Heerikhuisen, S. A. Daerden, P. Wolkenberg, P.-F. Coheur; Retrie- Fuselier, N. Pogorelov, N. A. Schwadron, G. P. val and characterization of carbon monoxide (CO) Zank, E. J. Zirnstein, J. M. SOKÓŁ, M. Toku- vertical profiles in the Martian atmosphere from maru, M. BZOWSKI, M. A. KUBIAK, D. B. observations of PFS/MEX; Journal of Quan- Reisenfeld; Temporal Evolution of the Latitude titative Spectroscopy and Radiative Transfer, and Energy Dependence of the Energetic Neutral DOI: 10.1016/j.jqsrt.2019.05.009, 2019 Atom Spectral Indices Measured by the Interstellar 8. BZOWSKI, M., A. Galli; Energetic Neutral Boundary Explorer (IBEX) over the First Nine Atoms from the Heliosheath as an Additional Popu- Years; Astrophysical Journal Volume 875, lation of Neutral Hydrogen in the Inner Heliosphere; Issue 2, Article number 91, DOI: 10.3847/ The Astrophysical Journal, Volume 870, 1538-4357/ab0f37, 2019 Number 2, Article number 58, DOI: 10.3847/ 15. Dick, H. J. B., C. J. MacLeod, P. Blum, N. Abe, 1538-4357/aaf1b2, 2019 D. K. Blackman, J. A. Bowles, M. J. Cheadle, K. 9. BZOWSKI, M., A. CZECHOWSKI, P. C. Cho, J. CIĄŻELA, J. R. Deans, V. P. Edgcomb, Frisch, S. A. Fuselier, A. Galli, J. GRYGOR- C. Ferrando, L. France, B. Ghosh, B. Ildefon- CZUK, J. Heerikhuisen, M. A. KUBIAK, H. se, B. Joh, M. A. Kendrick, J. Koepke, J. A. M. Kucharek, D. J. McComas, E. Möbius, N. A. Leong, C. Liu, Q. Ma, T. Morishita, A. Morris, Schwadron, J. Slavin, J. M. SOKÓŁ, P. SWA- J. H. Natland, T. Nozaka, O. Pluemper, A. San- CZYNA, P. Wurz, E. J. Zirnstein; Interstellar filippo, J. B. Sylvan, M. A. Tivey, R. Tribuzio, Neutral Helium in the Heliosphere from IBEX G. Viegas; Dynamic Accretion Beneath a Slow- Observations. VI. The He+ Density and the Ioniza- Spreading Ridge Segment: IODP Hole 1473A and tion State in the Very Local Interstellar Matter; the Atlantis Bank Oceanic Core Complex, Journal Astrophysical Journal, Volume 882, Issue 1, of Geophysical Research: Solid Earth, Volu- Article number 60, DOI: 10.3847/1538- me 124, Issue 12, Pages 12631-12659, DOI: 4357/ab3462, 2019 10.1029/2018JB016858, 2019 10. Chen, C., J. CIĄŻELA, W. Li, W. Dai, Z. 16. GALICKI, M.; Optimal sliding control of mobile Wang, S. F. Foley, M. Li, Z. Hu, Y. Liu; Calcium manipulators; Bulletin of the Polish Academy isotopic compositions of oceanic crust at various sprea- of Sciences: Technical Sciences Volume 67, ding rates; Geochimica et Cosmochimica Acta, Issue 4, Pages 777-788, DOI: 10.24425/ DOI: 10.1016/j.gca.2019.07.008, 2019 bpasts.2019.130187, 2019 11. Conroy, P., G. Quins, N. Flourya, O. Witasse, 17. Galli, A., P. Wurz, F. Rahmanifard, E. Möbius, M. Cartacci, R. Orosei, W. KOFMAN, B. N. A. Schwadron, H. Kuchaek H., Heirtzler Sánchez-Canof; A new method for determining the D., Fairchild K., BZOWSKI M., KUBIAK total electron content in Mars' ionosphere based on M.A., KOWALSKA-LESZCZYŃSKA I., Mars Express MARSIS data; PLANETARY SOKÓŁ J.M., Fuselier S.A., Swaczyna P., AND SPACE SCIENCE, DOI: 10.1016/ McComas D.J.; Model-free maps of interstellar j.pss.2019.104812, 2019 neutral hydrogen measured with IBEX between 2009 12. CZECHOWSKI, A., M. BZOWSKI, J. M. and 2018; Astrophysical Journal, Vol. 871, SOKÓŁ, M. A. KUBIAK, J. Heerikhuisen, E. 10.3847/1538-4357/aaf737, 2019 J. Zirnstein, N. V. Pogorelov, N. A. Schwad- 18. Giuranna, M., S. Viscardy, F. Daerden, L. ron, M. Hilchenbach, J. GRYGORCZUK, G. Neary, G. Etiope, D. Oehler, V. Formisano, A. P. Zank; Heliospheric Structure as Revealed by the Aronica, P. Wolkenberg, S. Aoki, A. Cardesín- 3–88 keV H ENA Spectra; The Astrophysical Moinelo, J. Marín-Yaseli de la Parra, D. Journal, Volume 888, Number 1, DOI: Merritt, M. Amoroso; Independent confirmation 10.3847/1538-4357/ ab5b14, 2019 of a methane spike on Mars and a source region east of 13. Derek, M., E. WOŹNIAK, S. Kulczyk, Cluste- Gale Crater; Nature Geoscience, Volume 12, ring nature-based tourists by activity. Social, economic Issue 5, Pages 326-332, DOI: 10.1038/ and spatial dimensions; Tourism Management s41561-019-0331-9, 2019 75, pp. 509-521 DOI: 10.1016/j.tourman. 19. Giuranna, M., P. WOLKENBERG, D. Grassi, 2019.06.014, 2019 A. Aronica, S. Aoki, D. Scaccabarozzi, B.

117 Saggin, V. Formisano; The current weather and ASTRONOMICAL SOCIETY 489, 1667– climate of Mars: 12?years of atmospheric monitoring 1683, DOI:10.1093/mnras/stz2174, 2019 by the Planetary Fourier Spectrometer on Mars 25. Hendricks, R. J., F. Ozimek, K. Szymaniec, B. Express; Icarus, Article number 113406, DOI: NAGÓRNY, P. DUNST, J. NAWROCKI, S. 10.1016/j.icarus.2019.113406, 2019 Beattie, B. Jian, K. Gibble; Cs Fountain Clocks 20. GRYNYSHYNA-POLIUGA, O.; Characteri- for Commercial Realizations-An Improved and stic of modelling spatial processes using geostatistical Robust Design; IEEE TRANSACTIONS ON analysis; Advances in Space Research, Volume ULTRASONICS FERROELECTRICS 64, Issue 2, Pages 415-426, DOI: 10.1016/j. AND FREQUENCY CONTROL, Volume: asr.2019.04.020, 2019 66 Issue: 3 Pages: 624-631 Special Issue: SI 21. GURGUREWICZ, J., D. MÈGE, M. Skiścim, DOI: 10.1109/TUFFC.2018.2874550, 2019 J. Pers; Nanotopographic characterization of micro- 26. Herique, A., W. KOFMAN, S. Zine, J. Blum, J.- fractures in rocks by Atomic Force Microscopy; Jour- B. Vincent, V. Ciarletti; Homogeneity of 67P as nal of Structural Geology, Volume 124, Pages seen by CONSERT: implication on composition and 70-80, DOI: 10.1016/j.jsg.2019.04.010, 2019 formation; Astronomy & Astrophysics, Vol. 22. Hadlera, K., D. J. P. Martin, J. Carpenter, J. J. 630, A6 (5p), DOI:10.1051/0004-6361/2018 Cilliers, A. Morse, S. Starr, J. N. Rasera, K. 34865, 2019 SEWERYN, P. Reiss, A. Meurisse; A universal 27. JENEROWICZ, M., A. WAWRZASZEK, W. framework for Space Resource Utilisation (SRU); DRZEWIECKI, M. KRUPIŃSKI, S. ALE- Planetary and Space Science, DOI: 10.1016/j. KSANDROWICZ; Multifractality in Humani- pss.2019.104811, 2019 tarian Applications: A Case Study of Internally 23. Hare, B. M., O. Scholten, J. Dwyer, T. N. G. Displaced Persons/Refugee Camps; IEEE Journal Trinh, S. Buitink, S. ter Veen, A. Bonardi, A. of Selected Topics in Applied Earth Obser- Corstanje, H. Falcke, J. R. Hörandel, T. Huege, vations and Remote Sensing DOI: 10.1109/ P. Mitra, K. Mulrey, A. Nelles, J. P. Rachen, L. jstars.2019.2950970, 2019 Rossetto, P. Schellart, T. Winchen, J. Ander- 28. Jin, Y., J. I. Moen, A. Spicher, K. Oksavik, W. J. son, I. M. Avruch, M. J. Bentum, R. Blaauw, J. Miloch, L. B. N. Clausen, M. POŻOGA, Y. W. Broderick, W. N. Brouw, M. Brüggen, H. R. Saito; Simultaneous Rocket and Scintillation Obser- Butcher, B. Ciardi, R. A. Fallows, E. de Geus, vations of Plasma Irregularities Associated With a S. Duscha, J. Eislöffel, M. A. Garrett, J. M. Reversed Flow Event in the Cusp Ionosphere; Journal Grießmeier, A. W. Gunst, M. P. van Haarlem, J. of Geophysical Research: Space Physics, Vol. W. T. Hessels, M. Hoeft, A. J. van der Horst, 124, Issue 8, pages 7098-7111, DOI: 10.1029/ M. Iacobelli, L. V. E. Koopmans, A. Kran- 2019JA026942, 2019 kowski, P. Maat, M. J. Norden, H. Paas, M. 29. KŁOS, Z., I. STANISŁAWSKA, B. DZIAK- Pandey-Pommier, V. N. Pandey, R. Pekal, R. JANKOWSKA; Heliogeophysical prediction service Pizzo, W. Reich, H. ROTHKAEHL, H. J. A. in Poland:past, present and future; History of Geo- Röttgering, A. Rowlinson, D. J. Schwarz, A. and Space Sciences, Volume 10, Issue 1, Pages Shulevski, J. Sluman, O. Smirnov, M. Soida, M. 193-199, DOI: 10.5194/hgss-10-193-2019, Tagger, M. C. Toribio, A. van Ardenne, R. A. 2019 M. J. Wijers, R. J. van Weeren, O. Wucknitz, P. 30. KOTARBA, A. Z., S. Chacewicz, E. Żmudz- Zarka, P. Zucca; Needle-like structures discovered ka; Night sky photometry over Warsaw (Poland) eva- on positively charged lightning branches; Nature, luated simultaneously with surface-based and satellite- volume 568, pages 360–363, DOI: 10.1038/ based cloud observations; Journal of Quantitative s41586-019-1086-6, 2019 Spectroscopy and Radiative Transfer, 235, 95- 24. Heggy, E., E. M. Palmer, A. Herique, W. 107, DOI:10.1016/j.jqsrt.2019.06.024, 2019 KOFMAN, M. R. El-Maarry; Post-rendezvous 31. Kozłowski, S., K. Kurek, J. Skarzyński, K. Sz- radar properties of comet 67P/CG from the Rosetta czygielska, M. DARMETKO; Verifying a con- Mission: understanding future Earth-based radar cept of adaptive communication with LEO satellites observations and the dynamical evolution of comets, using SDR-based simulations; International Jour- MONTHLY NOTICES OF THE ROYAL nal of Microwave and Wireless Technologies, DOI: 10.1017/S1759078719000552, 2019

118 32. KRÓLIKOWSKA, M., P. A. Dybczyński; Dis- 38. Łabiak, G., M. WĘGRZYN, A. Rosado-Mu- covery statistics and 1/a distribution of long-period ñoz, G. Bazydło; Dual-model approach for safety- comets detected during 1801–2017; Monthly Noti- critical embedded systems; Microprocessors and ces of the Royal Astronomical Society, Volu- Microsystems, Volume 72, Article number 10 me 484, Issue 3, Pages 3463-3475, DOI: 10. 2924, DOI: 10.1016/j.micpro.2019. 102924, 1093/mnras/stz02, 2019 2019 33. KRÓLIKOWSKA, M.; Non-gravitational effects 39. Matonti, C., N. Attree, O. Groussin, L. Jorda, change the original 1/a-distribution of real near- S. Viseur, S. F. Hviid, S. Bouley, D. Nébouy, A.- parabolic comets; Astronomy & Astrophysics, T. Auger, P. L. Lamy, H. Sierks, G. Naletto, R. DOI: 10.1051/0004-6361/201936316, 2019 Rodrigo, D. Koschny, B. Davidsson, M. A. 34. Kromuszczyńska, O., D. MÈGE, K. Dabniak, Barucci, J.-L. Bertaux, I. Bertini, D. Bodewits, J. GURGUREWICZ, M. Makowska, A. Lu- G. Cremonese, V. Da Deppo, S. Debei, M. De cas; Deep-seated gravitational slope deformation Cecco, J. Deller, S. Fornasier, M. Fulle, P. J. scaling on Mars and Earth: Same fate for different Gutiérrez, C. Güttler,W.-H. Ip, H. U. Keller, L. initial conditions and structural evolutions; Earth M. Lara, F. La Forgia, M. Lazzarin, A. Lu- Surface Dynamics Volume 7, Issue 2, Pages cchetti, J. J. López-Moreno, F. Marzari, M. 361-376, DOI: 10.5194/esurf-7-361-2019, Massironi, S. Mottola, N. Oklay, M. Pajola, L. 2019 Penasa, F. Preusker, H. RICKMAN, F. Schol- 35. KUBIAK, M. A., M. BZOWSKI, J. M. SO- ten, X. Shi, I. Toth, C. Tubiana, J.-B. Vincent; KÓŁ; Distribution Function of Neutral Helium Bilobate comet morphology and internal structure outside and inside the Heliopause; Astrophysical controlled by shear deformation; Nature Geo- Journal, Volume 882, Issue 2, Article number science, DOI: 10.1038/s41561-019-0307-9, 114, DOI: 10.3847/1538-4357/ab3404, 2019 2019 36. Kuzina, S. V., A. S. Kirichenko, M. STĘŚLI- 40. Moździerski, D., A. Pigulski, Z. Kołaczko- CKI, J. SYLWESTER, M. SIARKOWSKI, Ż. wski, G. Michalska, G. Kopacki, F. Carrier, P. SZAFORZ, S. PŁOCIENIAK, J. BAK¸ AŁA, Walczak, A. Narwid, M. STĘŚLICKI, J.-N. J. BARYLAK, P. PODGÓRSKI, D. ŚCISŁO- Fu, X.-J. Jiang, Ch. Zhang, J. Jackiewicz, J. WSKI, M. KOWALIŃSKI, S. A. Bogachev A. Telting, T. Morel, S. Saesen, E. Zahajkiewicz, A. Pertso; SOLPEX Complex for Studies of Solar P. Bruś, P. Śródka, M. Vuckovic, T. Verhoelst, Radiation in the Soft X-Ray Range; Technical V. Van Helshoecht, K. Lefever, C. Gielen, L. Physics, 2019, Vol. 64, No. 12, pp. 1738–1741, Decin, J. Vanautgaerden, C. Aerts; Ensemble DOI: 10.1134/S1063784219120132, 2019 asteroseismology of pulsating B-type stars in NGC 37. Lai, I.-L., W.-H. Ip, J.-C. Lee, Z.-Y. Lin, J.-B. 6910; ASTRONOMY & ASTROPHYSICS Vincent, N. Oklay, H. Sierks, C. Barbieri, P. Volume 632, Article Number A95, 22 pp. Lamy, P. Rodrigo, D. Koschny, H. RICK- DOI: 10.1051/0004-6361/201936418, 2019 MAN, H. U. Keller, J. Agarwal, M. A. Barucci, 41. NASTULA, J., M. Wińska, J. ŚLIWIŃSKA, D. J.-L. Bertaux, I. Bertini, D. Bodewits, S. Bou- Salstein; Hydrological signals in polar motion dreault, G. Cremonese, V. Da Deppo, B. Da- excitation – Evidence after fifteen years of the vidsson, S. Debei, M. De Cecco, J. Deller, S. GRACE mission; Journal of Geodynamics, Fornasier, M. Fulle, O. Groussin, P. J. Gutiér- Volume 124, Pages 119-132, DOI: 10.1016/j. rez, C. Güttler, M. Hofmann, S. F. Hviid, L. jog.2019.01.014, 2019 Jorda, J. Knollenberg, G. Kovacs, J.-R. 42. Østgaard, N., J. E. Balling, T. Bjørnsen, P. Bra- Kramm, E. Kührt, M. Küppers, L. M. Lara, M. uer, C. Budtz-Jørgensen, W. BUJWAN, B. Lazzarin, J. J. López-Moreno, F. Marzari, G. Carlson, F. Christiansen, P. Connell, C. Eyles, Naletto, X. Shi, C. Tubiana, N. Thomas; Sea- D. Fehlker, G. Genov, P. GRUDZIŃSKI, P. sonal variations in source regions of the dust jets on Kochkin, A. Kohfeldt, I. Kuvvetli, P. L. Tho- comet 67P/Churyumov-Gerasimenko; Astronomy msen, S. M. Pedersen, J. Navarro-Gonzalez, T. and Astrophysics, 630, A17 (2019), DOI: 10. Neubert, K. Njøten, P. ORLEAŃSKI, B. H. 1051/0004-6361/20173 2094 Qureshi, L. R. Cenkeramaddi, V. Reglero, M. Reina, J. M. Rodrigo, M. Rostad, M. D. Sabau,

119 S. S. Kristensen, Y. Skogseide, A. Solberg, J. and climate models; Remote sensing, 11(24), Stadsnes, K. Ullaland, S. Yang; The Modular X- 2949; DOI: 10.3390/rs11242949, 2019 and Gamma-Ray Sensor (MXGS) of the ASIM 49. ŚLIWIŃSKA, J., J. NASTULA; Determining Payload on the International Space Station; Space and evaluating the hydrological signal in polar motion Science Reviews, Volume 215, Issue 2, Article excitation from gravity field models obtained from number 23, DOI: 10.1007/s11214-018-0573- kinematic orbits of LEO satellites; Remote Sen- 7, 2019 sing, Volume 11, Issue 15, Article number 43. Popiński, W.; Least squares orthogonal polynomial 1784, DOI: 10.3390/rs11151784, 2019 regression estimation for irregular design; Commu- 50. SOKÓŁ, J. M., M. A. KUBIAK, M. BZOW- nications in Statistics - Theory and Methods, SKI, E. Möbius, N. A. Schwadron; Science op- Volume 49, Issue 3, Pages 631-647, DOI: portunities from observations of the interstellar neutral 10.1080/03610926.2018.1549244, 2019 gas with an adjustable boresight direction; The 44. Przylibski, T. A., M. KACZOROWSKI, L. Astrophysical Journal Supplement Series, Fijałkowska-Lichwa, D. Kasza, R. ZDU- 22pp., DOI: 10.3847/1538-4365/ab50bc, NEK, R. WRONOWSKI; Testing of 222Rn 2019 application for recognizing tectonic events observed on 51. SOKÓŁ, J. M, M. A. KUBIAK, M. BZOW- water-tube tiltmeters in underground Geodynamic SKI; Interstellar neutral gas species and their pickup Laboratory of Space Research Centre at Książ (the ions inside the heliospheric termination shock. the Sudetes, SW Poland); APPLIED RADIATION large-scale structures; The Astrophysical Journal, AND ISOTOPES, DOI: 10.1016/j.apradiso. 20pp, DOI: 10.3847/1538-4357/ab21c4, 2019. 108967, 2019 2019 45. Rahmanifard, F., E. Möbius, N. A. Schwadron, 52. SOKÓŁ, J. M., M. BZOWSKI, M. Tokumaru; A. Galli, N. Richards, H. Kucharek, J. M. Interstellar neutral gas species and their pickup ions SOKÓŁ, D. Heirtzler, M. A. Lee, M. BZOW- inside the heliospheric termination shock. Ionization SKI, I. KOWALSKA-LESZCZYŃSKA, M. rates for H, O, Ne, and He; The Astrophysical Jo- A. KUBIAK, P. Wurz, S. A. Fuselier, D. J. urnal, Vol.872, Number 1, DOI: 10.3847/ McComas; Radiation pressure from interstellar 1538-4357/aafdaf, 2019 hydrogen observed by IBEX through solar cycle 24, 53. Stamm, J., A. CZECHOWSKI, I. Mann, C. Astrophysical Journal 887:217, DOI:10. Baumann, M. Myrvang; Dust trajectory simu- 3847/1538-4357/ab58ce, 2019 lations around the Sun, Vega, and Fomalhaut; 46. Reisenfeld, D. B., M. BZOWSKI, H. O. Fun- Astronomy and Astrophysics, Volume 626, sten, P. H. Janzen, N. Karna, M. A. KUBIAK, Article number A107, DOI: 10.1051/0004- D. J. Mccomas, N. A. Schwadron, J. M. 6361/201834727, 2019 SOKÓŁ; The influence of polar coronal holes on the 54. SYLWESTER, B., J. SYLWESTER, M. polar ENA flux observed by ibex; Astrophysical SIARKOWSKI, K. J. H. PHILLIPS, P. POD- Journal, Volume 879, Issue 1, Article number GÓRSKI, M. GRYCIUK; Analysis of Quiescent 1, DOI: 10.3847/1538-4357/ab22c0, 2019 Corona X-ray Spectra from SphinX during the 2009 47. Savin, S., E. Amata, L. Zelenyi, C. Wang, H. Li, Solar Minimum; SOLAR PHYSICS Vol. 294, p. B. Tang, G. Pallocchia, J. Safrankova, Z. Ne- 176, 10.1007/s11207-019-1565-9, 2019 mecek, A. S. Sharma, F. Marcucci, L. Kozak, J. 55. SYLWESTER, J., M. STĘŚLICKI., J. BĄKA- L. Rauch, V. Budaev, J. BŁĘCKI, L. Legen, M. ŁA, S. PŁOCIENIAK, Ż. SZAFORZ, M. Nozdrachev; Collisionless Plasma Processes at KOWALIŃSKI, D. ŚCISŁOWSKI, P. Magnetospheric Boundaries: Role of Strong Non- PODGÓRSKI, T. MROZEK, J. BARYLAK, linear Wave Interactions; JETP Letters, DOI: A. MAKOWSKI, M. SIARKOWSKI, Z. 10.1134/S0021364019170028, 2019 KORDYLEWSKI, B. SYLWESTER, S. Ku- 48. ŚLIWIŃSKA, J., M. Biryło, Z. Rzepecka, J. zin, A. Kirichenko, A. Pertsov, S. Bogachev; NASTULA; Analysis of groundwater and total The soft X-ray spectrometer polarimeter SolpeX; Ex- water storage changes in Poland using GRACE perimental Astronomy, DOI: 10.1007/ observations, in-situ data, and various assimilation s10686-018-09618-4, 2019

120 56. TESSON, P.-A., S. J. Conway, N. Mangold, J. 4. KOTARBA, A. Z. (redaktor); Zanieczyszczenie CIĄŻELA J., S. R. Lewis, D. MÈGE; Evidence światłem. Źródła, obserwacje, skutki; ISBN 978- for thermal-stress-induced rockfalls on Mars impact 83-89439-03-1, 2019 crater slopes; Icarus, Article number 113503, DOI: 10.1016/j.icarus.2019.113503, 2019 Other articles in international and national 57. WAWRZASZEK, A., M. Echim, R. Bruno; publications (listed by the Polish Ministry of Multifractal Analysis of Heliospheric Magnetic Science and Higher Education) Field Fluctuations Observed by Ulysses; Astrophysical Journal, Volume 876, Issue 2, 1. ALEKSANDROWICZ, S., A. WAWRZA- Article number 153, DOI: 10.3847/1538- SZEK, M. JENEROWICZ, W. Drzewiecki, 4357/ab1750, 2019 M. KRUPIŃSKI; Local Multifractal Description 58. WAWRZASZEK, A., A. KRASIŃSKA; Hopf of Bi-Temporal VHR Images; 2019 10th Inter- Bifurcations, Periodic Windows and Intermittency in national Workshop on the Analysis of Multi- the Generalized Lorenz Model; INTERNATIO- temporal Remote Sensing Images (Multi- NAL JOURNAL OF BIFURCATION AND Temp), DOI: 10.1109/Multi-Temp.2019.88 CHAOS DOI: 10.1142/S02181274193 66963, 2019 00428, 2019 2. ALEKSIEJUK, K., J. BARAN, T. BARCIŃ- 59. WOŹNIAK, E., S. ALEKSANDROWICZ; SKI, J. MUSIAŁ; Planetary penetrator control ele- Self-adjusting thresholding for burnt area detection ctronics design concept; Proceedings of SPIE - based on optical images; Remote Sensing, Volume The International Society for Optical Engi- 11, Issue 22, Article number 2669, DOI: neering, Volume 11176, Article number 1117 10.3390/rs11222669, 2019 63X, DOI: 10.1117/12.2538027, 2019 60. Wysoczańska, R., P. A. Dybczyński, M. 3. BARYLAK, J., O.V. Dudnik, T. WOŹNI- KRÓLIKOWSKA; First stars that could signi- CZAK, V. O. Adamenko, R. V. Antypenko, ficantly perturb comet motion are finally found; N.V. Yezerskyi, M. KOWALIŃSKI, I.V. Monthly Notices of the Royal Astronomical Lazarev, A. ZIELIŃSKA, J. SYLWESTER, J. Society, DOI: 10.1093/mnras/stz3127, 2019 BĄKAŁA, P. PODGÓRSKI; Simulation of 61. Zalewska, N. E., M. Mroczkowska-Szerszeń, CubeSat caliber particle detector “MiRA_ep” J. Fritz, M. BŁĘCKA; Modeling of surface spectra response to energetic electrons and protons using with and without dust from Martian infrared data: GEANT4 package; Proceedings of SPIE - The new aspects; Aircraft Engineering and Aero- International Society for Optical Engineering space Technology, Volume 91, Issue 2, Pages Vol. 11176, 111763C-1, DOI: 10.1117/12. 333-345, DOI: 10.1108/AEAT-01-2018- 2536748, 2019 0051, 2019 4. BASMADJI, F. L., G. Chmaj, T. Rybus, K. SEWERYN; Microgravity testbed for the develo- Monographs, reviews in international and pment of space robot control systems and the demon- national publications stration of orbital maneuvers; Proceedings of SPIE - The International Society for Optical 1. KŁOS, Z., A. DŁUGOSZ; Wprowadzenie: Dy- Engineering, Volume 11176, Article number lematy Europejskiej Polityki Kosmicznej; Prawne 111763V DOI: 10.1117/12.2537981, 2019 aspekty działalności kosmicznej, Kancelaria 5. Christe, S., Y. Shih Albert, S. Krucker, L. Gle- senatu, 2019 sener, P. Saint-Hilaire, A. Caspi, S. GBUREK, 2. STANISŁAWSKA, I., B. DZIAK-JAN- M. STĘŚLICKI, C. Allred Joel, M. Battaglia, KOWSKA; ROZDZIAŁ IV: Prognozy pogody W. H. Baumgartner, J. Drake, K. Goetz, B. kosmicznej w służbie społeczeństw; Prawne as- Grefenstette, I. Hannah, G. D. Holman, A. In- pekty działalności kosmicznej, Kancelaria Se- glis, J. Ireland, J. A. Klimchuk, S.-N. Ishikawa, natu, 2019 E. Kontar, V. A. Massone; N. Vilmer; The 3. ORLEAŃSKI, P.; Satelitarna aparatura nauko- Focusing Optics X-ray Solar Imager (FOXSI); wa projektowanie instrumentów ze szczególnym uw- American Astronomical Society Meeting zględnieniem reguł dotyczących niezawodności; #234, id. 225.01. Bulletin of the American ISBN: 978-83-89439-02-4, 2019 Astronomical Society, No. 4, Vol. 51, 2019

121 6. CICHOCKI, A., K. Poźniak, R. Romaniuk; nal Conference on Electromagnetics in Modelling of soft fault propagation in sequential Advanced Applications, ICEAA 2019, Article circuits by fuzzy-logic simulations; Proceedings of number 8879384, Page 695, 2019 SPIE - The International Society for Optical 13. FOKS-RYZNAR, A., J. RYZENKO, K. Engineering Volume 11176, Article number TRZEBIŃSKA, J. TYMIŃSKA, E. WRZO- 111763B DOI: 10.1117/12.2536693, 2019 SEK, T. Zwęgliński; Trial as a pragmatic and 7. Dacko, A., T. Kowalski, J. B. BARAN, T. BAR- systematic approach for assessing new solutions in cri- CIŃSKI; Electronic box structural analyses for a sis management and rescue operations; Proceedings space flight; Proceedings of SPIE - The Interna- of SPIE - The International Society for Opti- tional Society for Optical Engineering, cal Engineering Volume 11176, Article num- Volume 11176, Article number 111763S ber 111763T, DOI: 10.1117/12.2537925, DOI: 10.1117/12.2537610, 2019 2019 8. Damaceno, J. G., C. Cesaroni, L. Spogli, M. 14. Fulara, M., K. SEWERYN; Efficiency of the GRZESIAK, G. De Franceschi, M. Cafaro; thermal energy storage made of lunar regolith, 8TH Regional short-term forecasting model to predict EUROPEAN CONFERENCE FOR ionospheric scintillation and TEC at low latitudes; AERONAUTICS AND SPACE SCIENCES 2019 URSI Asia-Pacific Radio Science Con- (EUCASS), DOI: 10.13009/EUCASS2019- ference, AP-RASC 2019 March 2019, Article 444, 15pp, 2019 number 8738621 DOI: 10.23919/URSIAP- 15. Galicki, M., M. BANASZKIEWICZ; Optimal RASC.2019.8738621, 2019 trajectory tracking control of omni-directional mobile 9. Drzewiecki, W., A. WAWRZASZEK, M. robot; 12th International Workshop on Robot KRUPIŃSKI, S. ALEKSANDROWICZ, M. Motion and Control, RoMoCo 2019 - Work- JENEROWICZ; Multifractal Parameters in Pre- shop Proceedings, Article number 8787377, diction of Land-use Components on Satellite Images; Pages 137-142, 2019 DOI: 10.1109/RoMoCo. IGARSS 2019 - 2019 IEEE International 2019.8787377, 2019 Geoscience and Remote Sensing Symposium, 16. GROMNY, E., S. LEWIŃSKI, M. RYBICKI, DOI: 10.1109/IGARSS.2019.8900247, 2019 R. MALINOWSKI, M. KRUPIŃSKI, A. THE INSTITUTE OF ELECTRICAL NOWAKOWSKI, M. JENEROWICZ; Crea- AND ELECTRONICS ENGINEERS INC., tion of training dataset for Sentinel-2 land cover classi- 2019 fication; Proc. SPIE 11176, Photonics Applica- 10. Drzewiecki, W., A. WAWRZASZEK, M. tions in Astronomy, Communications, Indu- KRUPIŃSKI, S. ALEKSANDROWICZ, M. stry, and High-Energy Physics Experiments JENEROWICZ; Multifractal parameters in predi- 2019, 111763D DOI:10.1117/12.2536773, ction of land-use components on satellite images, SPA 2019 2019: Signal Processing: Algorithms, Archi- 17. GROMNY, E., S. LEWIŃSKI, M. RYBICKI, tectures, Arrangements, and Applications: R. MALINOWSKI, M. KRUPIŃSKI, A. Poznań, 18-20 September 2019: conference NOWAKOWSKI; Post-processing tools for land proceedings, IEEE., ISBN: 978-83-62065- cover classification of Sentinel-2, Proc. SPIE 34-9, 296–301, 2019 11176, Photonics Applications in Astronomy, 11. DUDNIK, O.V., J. SYLWESTER, M. KO- Communications, Industry, and High-Energy WALIŃSKI, J. BARYLAK; Utilization of Physics Experiments, DOI:10.1117/12.2537 design features of the particle telescope STEP-F and 325, 2019 solar x-ray spectrophotometer SphinX for exploration 18. JENEROWICZ, M., A. WAWRZASZEK, M. of the Earth's radiation belt properties; Proc. of KRUPIŃSKI, W. Drzewiecki, S. ALEKSAN- SPIE Vol. 11176 111763L-1, DOI: 10.1117/ DROWICZ; APLICABILITY OF MULTI- 12.2537296, 2019 FRACTAL FEATURES AS DESCRI- 12. Eyraud, C., L.-I. Sorsa, A. Herique, J.-M. Gef- PTORS OF THE COMPLEX TERRAIN frin, S. Pursiainen, W. KOFMAN; Imaging the SITUATION IN IDP/REFUGEE CAMPS; interior of small Solar bodies: Towards a quantitative IGARSS 2019 - 2019 IEEE International approach; Proceedings of the 21st Internatio- Geoscience and Remote Sensing Symposium,

122 DOI: 10.1109/IGARSS.2019.8898588, 2019 neering, Volume 11176, Article number 1117 19. JENEROWICZ, M., A. WAWRZASZEK, M. 63P, DOI: 10.1117/12.2537380, 2019 KRUPIŃSKI, S. ALEKSANDROWICZ, W. 26. Martyński, K., A. Kułak, J. Młynarczyk, J. Drzewiecki; Comparison of mathematical mor- BŁĘCKI, R. WRONOWSKI, R. Iwański; The phology with the local multifractal description applied modification of the ionosphere over the thunderstorm to the image samples processing; Proc. SPIE 11176, area - registrations from DEMETER and Swarm Photonics Applications in Astronomy, Com- satellites; Publications of the Institute of Geo- munications, Industry, and High-Energy Phy- physics, PAS, vol 425 (M-32), pp.85-88, DOI: sics Experiments 2019, 1117638 DOI:10. 10.2517/InstGeoph_PAS_Publs-2019-016, 1117/12.2536408, 2019 2019 20. KACZOROWSKI, M., D. Kasza, R. ZDU- 27. MUSIAŁ, J., K. ALEKSIEJUK, J. BARAN, T. NEK, M. RUDNICKI, R. WRONOWSKI; BARCIŃSKI; Planetary penetrator electromagnetic Time dependencies between tectonic activity of drive design concept; Proceedings of SPIE - The Świebodzice depression (SW Poland) and seismic International Society for Optical Engineering, activity in poland and czech mining regions; E3S Web Volume 11176, Article number 111763Y, of Conferences, Volume 105, Article number DOI: 10.1117/12.2538028, 2019 02001, DOI: 10.1051/e3sconf/20191050 28. ORLEAŃSKI, P.; Design and development of 2001, 2019 scientific satellite instrumentation according to Space 21. Konacki, M., A. Malacz, A. Chimicz, P. LEJ- 4.0 approach: The dvantages and dangers; BA, P. Sybilski, R. Pawłaszek, S. Kozłowski, T. Proceedings of SPIE - The International So- SUCHODOLSKI, K. Kozłowski, A. Sybil- ciety for Optical Engineering, Volume 11176, ska, B. Rogowska, D. Pazderski, M. Żołnow- Article number 111763Q, DOI: 10.1117/12. ski, A. Shearer, A. Słowikowska, M. Pilichow- 2537399, 2019 ski, M. Malawski, M. Gędek; Optical, Laser and 29. PALMA, P., K. SEWERYN; Space robot equip- Processing Capabilities of the New Polish Space ped with compliant linear actuator on end effector: Situational Awareness Centre; Advanced Maui Simulations results; Proceedings of SPIE - The Optical and Space Surveillance Technologies International Society for Optical Engineering, Conference (AMOS), 22pp, 2019 Volume 11176, Article number 111763H, 22. KRUPIŃSKI, M., S. LEWIŃSKI, R. MALI- DOI: 10.1117/12.2537207, 2019 NOWSKI; One class SVM for building detection on 30. PALMA, P.; Linear Electromagnetic Actuator with Sentinel-2 images; Proc. SPIE 11176, Photonics Mechanical Impedance Control for Experimental Applications in Astronomy, Communica- Investigation of Landing and Transient Contact in tions, Industry, and High-Energy Physics Low Gravity; IFToMM World Congress on Experiments 2019, 1117635 DOI:10.1117/ Mechanism and Machine Science, Volume 73, 12.2535547, 2019 2019, Pages 2691-2700, DOI: 10.1007/978-3- 23. KRUPIŃSKI, M., A. WAWRZASZEK, W. 030-20131-9_266, 2019 DRZEWIECKI, S. ALEKSANDROWICZ, 31. POLAK, S., M. RATAJ, A. BIAŁEK, T. M. JENEROWICZ; Multifractal Parameters for PAŁGAN, P. Hartogh, J. P. Garcia, S. Stämm; Spectral Profile Description, IEEE International Design of the radiator for detection part of the Geoscience and Remote Sensing Symposium, Submillimeter Wave Instrument (SWI) of JUICE DOI: 10.1109/IGARSS.2019.8898588, 2019 mission; Proceedings of SPIE - The Interna- 24. Madry J., R. WAWRZASZEK; Design and tests tional Society for Optical Engineering, Volu- of sunsensor based on 2D position sensitive detector; me 11176, Article number 111763U, DOI: Proceedings of SPIE - The International So- 10.1117/12.2537980, 2019 ciety for Optical Engineering, Volume 11176, 32. POPIELAWSKA, B., A. Odzimek, J. Doro- Article number 111763Z, DOI: 10.1117/12. szkiewicz, G. Góral; SUPERDARN W POL- 2538029, 2019 SCE – PERSPEKTYWY; Przegląd Geofizy- 25. MALINOWSKI, B.; On the legality of appropria- czny, Tom LXIV, No. 3-4, 221-251, DOI: tion of space resources; Proceedings of SPIE - 10.32045/PG-2019-007, 2019 The International Society for Optical Engi- 33. POŻOGA, M., B. MATYJASIAK, Ł. TO-

123 MASIK; Space weather usage of LOFAR PL610 gineering Volume 11176, Article number 1117 station; Proceedings of SPIE - The Interna- 63K, DOI: 10.1117/12.2537290, 2019 tional Society for Optical Engineering, Volu- 41. Sokal, E., R. WAWRZASZEK,G. JUCHNI- me 11176, Article number 111763O, DOI: KOWSKI, J. ADAMIEC, T. Zawistowski T.; 10.1117/12.2537373, 2019 Design and test of magnetorquer in PCB technology 34. POŻOGA, M., B. MATYJASIAK, H. RO- for nanosatellites; Proceedings of SPIE - The THKAEHL, R. WRONOWSKI, Ł. TOMA- International Society for Optical Engineering, SIK; ELF Signatures in Low and High Radio Fre- Volume 11176, Article number 111763R, quency Signals; Publications of the Institute of DOI: 10.1117/12.2537411, 2019 Geophysics, PAS, vol. 425 (M-32), pp.71-72, 42. Thomas, N., et al. (including M. BANA- DOI:10.25171/instgeoph_pas_publs-2019- SZKIEWICZ, P. ORLEAŃSKI, P. WAJER 014, 2019 and P. P. WITEK from CBK PAN); The Effects 35. RATAJ, M., R. PIETRZAK, P. WAWER, P. of Past and Current Geologic Processes Observed by ORLEAŃSKI; Design of the MERTIS pointing the CaSSIS Imager Onboard ESA's ExoMars unit for BEPI Colombo mission; Proceedings of Trace Gas Orbiter; Ninth International Confe- SPIE - The International Society for Optical rence on Mars, No. 2089, id.6156, 2pp., 2019 Engineering Volume 11176, Article number 43. Thomas, N., et al. (including M. BANA- 111763F, DOI: 10.1117/12.2536807, 2019 SZKIEWICZ, P. ORLEAŃSKI, P. WAJER 36. RATAJ, M., P. WAWER, K. SKUP, M. SO- and P. P. WITEK from CBK PAN); Overview of BIECKI; Design of fine guidance system (FGS) for Imaging in the First 9 Months of the Prime Mission; ARIEL mission; Proceedings of SPIE - The Lunar and Planetary Science Conference, No. International Society for Optical Engineering, 2132, id.1585, 2pp., 2019 Volume 11176, Article number 111763E, 44. TOMASIK, Ł., M. POŻOGA, B. MATYJA- DOI: 10.1117/12.2536800, 2019 SIAK; Regional warning centre of Warsaw in 37. RICKMAN, H.; The IAU and the Impact Ha- heliogeophysical prediction service laboratory: Space zard; Proceedings of the International Astro- weather service in Poland; Proceedings of SPIE - nomical Union, Volume 349, Pages 71-74, The International Society for Optical DOI: 10.1017/S1743921319000140, 2019 Engineering, Volume 11176, Article number 38. SEWERYN, K., P. PAŚKO, G. Visentin; The 111763N, DOI: 10.1117/12.2537368, 2019 Prototype of Regolith Sampling Tool Dedicated to 45. WAWRZASZEK, R., M. RATAJ; Optimization Low Gravity Planetary Bodies; IFToMM World of angular rotation control for high accuracy and Congress on Mechanism and Machine Scien- repeatability mirror positioning system of space ce, Volume 73, 2019, Pages 2711-2720, DOI: hyperspectral spectrometer DESIS; Proceedings of 10.1007/978-3-030-20131-9_268, 2019 SPIE - The International Society for Optical 39. SKUP, K. R., A. CICHOCKI, K. BER, M. Engineering, Volume 11176, Article number DARMETKO, G. JUCHNIKOWSKI, W. 1117640, DOI: 10.1117/12.2538030, 2019 BUJWAN, M. MICHALSKA, M. WIN- 46. WOŹNIAK, E., W. KOFMAN, S. ALE- KLER, S. Krucker, S. Koegl, O. Grimm; STIX KSANDROWICZ, M. RYBICKI, S. LEWI- IDPU: Very efficient and reliable controller for a ŃSKI; Multi-Temporal Indices Derived from Ti-me scientific instrument; Proceedings of SPIE - The Series of Sentinel-1 Images as a Phenological Des- International Society for Optical Engineering cription of Plants Growing for Crop Classification; Volume 11176, Article number 111763J, 2019 10th International Workshop on the DOI: 10.1117/12.2537272, 2019 Analysis of Multitemporal Remote Sensing 40. SKUP, K. R., K. RUTKOWSKI, K. BER, W. Images, DOI: 10.1109/Multi-Temp.2019.88 NOWOSIELSKI, P. KORBA, P. KULIGO- 66905, Article number 8866905, 2019 WSKI, W. BUJWAN, M. WINKLER, P. 47. Zalizovski, A., B. DZIAK-JANKOWSKA, I. Hartogh, J. P. Garcia, E.-P. Miettinen; Design of STANISŁAWSKA, Y. Yampolski; Connection DPU and PSU for ESA JUICE Submillimeter between sporadic E layers and geomagnetic field varia- Wave Instrument (SWI); Proceedings of SPIE - tions at the Antarctic Peninsula and Europe; 2019 The International Society for Optical En- URSI Asia-Pacific Radio Science Conference,

124 Article number 8738614, DOI: 10.23919/ Other publications URSIAP-RASC.2019.8738614, 2019 1. CIĄŻELA, J.; Polacy przystępują do poszuki- 48. ZALIZOVSKI, A., Ł. TOMASIK, I. STANI- wań złota na Marsie; Wszystko Co Najwa- SLAWSKA; Technique for building the global maps żniejsze (https://wszystkoconajwazniej of MUF(3000) analysis and forecast; 2019 URSI sze.pl/jakub-ciazela-polacy-przystepuja-do- Asia-Pacific Radio Science Conference, Arti- poszukiwan-zlota-na-marsie/) cle number 8738328, DOI: 10.23919/ 2. WAJER, P., R. GABRYSZEWSKI; Rewolucja URSIAP-RASC.2019.8738328, 2019 kopernikańska okiem fizyka. Równanie Kep- 49. Grundmann, J. T., W. Bauer, R. Boden, M. lera, granica Laplace'a i rekurencyjne szeregi Ceriotti, S. Chand, F. Cordero, B. Dachwald, potęgowe; Fizyka w Szkole, 26-31, 2019 E. Dumont, C. D. Grimm, J. Heiligers, D. 3. KOTARBA, A.; Najjaśniej... nad latarnią. Hercík, A. Hérique, T.-M. Ho, R. Jahnke, W. Zanieczyszczenie światłem z perspektywy KOFMAN, C. Lange, R. Lichtenheldt, C. orbity; space24.pl McInnes, J.-G. Meß, T. Mikschl, E. Mikulz, S. 4. KRÓLIKOWSKA-SOŁTAN, M., KOTAR- Montenegro, I. Moore, I. Pelivan, A. Peloni, BA, A.; "Koniec świata"? "Planetoida D. Plettemeier, D. Quantius, S. Reershemius, zniszczy Ziemię"? Sprawdzamy!; space24.pl T. Renger, J. Riemann, Y. Rogez, M. Ruffer, K. 5. SCHREIBER, R.; Ciekawe strony interneto- Sasaki, N. Schmitz; Flights are ten a sail - Re-use we (stała rubryka); Urania - Postępy Astrono- and commonality in the design and system engineering mii, 1-6/XC of small spacecraft solar sail missions with modular 6. SCHREIBER, R.; Człowiek — istota kosmi- hardware for responsive and adaptive exploration; czna; Urania - Postępy Astronomii, 5/XC, str. Proceedings of the International Astronau- 62, 2019 tical Congress, Volume 2019-October, Article 7. STANISŁAWSKA, I., Z. KŁOS; Małe sateli- number IAC-19_B4_8_12_x53800, 2019 ty – nowy trend czy kolejna faza rozwoju; Fa- kty, Magazyn gospodarczy wydanie specjalne, str. 42-43, 2019

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127 Invited lectures dules, R. GABRYSZEWSKI; FUTURE SPA- CE Kick-off Meeting, 12-13.11. 2019, War- Lectures on international conferences organized szawa, Polska by the CBK PAN 11. Space Programme for science centres and NGOs - the idea and connection to Space Schools Programme, R. 1. FGS Detector ConOps (H2RG detector & Euclid GABRYSZEWSKI; FUTURE SPACE Kick- Sidecar capabilities, Foreseen FGS readout modes, off Meeting, 12-13.11.2019, Warszawa, Polska M. RATAJ, A. PRZEPIÓRKA, M. SOBIEC- KI, T. PAŁGAN; ARIEL Payload Consor- Other lectures on conferences not organized by tium Meeting, 17-19.06.2019, Warszawa, the CBK PAN Polska 1. Characteristics of Ionospheric Conditions During Se- 2. ARIEL FGS CBK Progress Meeting, M. RATAJ, vere Geomagnetic Disturbances Using LOFAR and ARIEL Payload Consortium Meeting, 17-19. Satellite Diagnostics, B. Matyjasiak, M. Pożoga, 06.2019, Warszawa, Polska H. Rothkaehl, D. Przepiórka, M. Grzesiak, 3. Geodynamic Laboratory of SRC in Książ, Poland. Scintillating Science: Cutting-Edge Science Geodynamic Investigations and Collection of Achieved Through the observations of Radio Instruments, M. KACZOROWSKI, D. Kasza, Scintillations, 14-19.07.2019, Hermanus, RPA R. ZDUNEK, R. WRONOWSKI; NOMAD 2. Classification of Sentinel-2 data – towards automatic Science Working Team #15 meeting, 12- LC service, S. Lewiński, IRSEL - Innovation on 13.09.2019, Wrocław, Polska Remote Sensing Education and Learning, 4. Far-IR spectrometer for detecting ore metals on Mars, 28.08.2019, Kraków, Polska MIRORES; J. CIĄŻELA, J. BĄKAŁA, M. 3. Codzienna informacja satelitarna dla zarządzania KOWALIŃSKI, M. CIĄŻELA, J. BARY- kryzysowego, J. Ryzenko, M. Milczarek, Możli- LAK, B. Pieterek, J. GURGUREWICZ, D. wości wykorzystania technik satelitarnych MEGE, Z. SZAFORZ, F. Pirajno, M. Giu- przez administrację publiczną w Polsce, ranna, T. MROZEK, P.-A. TESSON; Polish- 21.01.2019, Warszawa, Polska China consultations on X-ray detectors back- 4. Drift dispersion of LOFAR scintillation measu- ground modeling and analysis, 19-21.09.2019, rements, M. Grzesiak, D. Przepiórka, M. Pożo- Wrocław, Polska ga, B. Matyjasiak, H. Rothkaehl, K. Budzińska, 5. Spectrometer for Temperature and Composition R. Wronowski and R. Fallows, EGU 2019, 7- (STC), S. GBUREK; Polish-China consult- 12.04.2019, Wiedeń, Austria ations on X-ray detectors background model- 5. FGS alignment and calibration issues, M. Rataj, P. ing and analysis, 19-21.09.2019, Wrocław, Wawer, M. Sobiecki, Ariel Consortium Polska Meeting, 7-9.10.2019, Utrecht, Holandia 6. Projekt MGEM - Modular GEM detectors, S. 6. FGS hardware update and current issues, M. Rataj, GBUREK; Polish-China consultations on X- P.WAWER, K. SKUP, M. SOBIECKI, Ariel ray detectors background modeling and ana- Consortium Meeting, 7-9.10.2019, Utrecht, lysis, 19-21.09.2019, Wrocław, Polska Holandia 7. SphinX: Solar Photometer in X-Rays, S. 7. Heliosphere under influence of Sun-originating vs. GBUREK; Polish-China consultations on X- LISM-originating fluctuations, R. Ratkiewicz, M. ray detectors background modeling and ana- Strumik, 18th Annual International Astro- lysis, 19-21.09.2019, Wrocław, Polska physics Conference, 18-22.02. 2019, Pasade- 8. Detector Simulator for STIX, P. PODGÓR- na, USA SKI; Polish-China consultations on X-ray de- 8. Monitoring pokrycia terenu na podstawie zdjęć sa- tectors background modeling and analysis, telitarnych, S. Lewiński, Możliwości wykorzy- 19-21.09.2019, Wrocław, Polska stania technik satelitarnych przez administra- 9. The FUTURE SPACE Project overview; R. GA- cję publiczną w Polsce, 21.01.2019, Warszawa, BRYSZEWSKI; FUTURE SPACE Kick-off Polska Meeting, 12-13.11. 2019, Warszawa, Polska 9. MONITORING POKRYCIA TERENU NA 10. Space Schools Programme - the idea and thematic mo- ZDJĘCIACH SATELITARNYCH SENTI-

128 NEL-2, S. Lewiński, II Konferencja projektu 19. Turbulence in Space Plasmas on Magnetohydro- Sat4Envi, 19-20.11.2019, Warszawa, Polska dynamic and Kinetic Scales, Plenary-Keynote 10. National Project Managers Meeting, M. Rataj, Invited Talk, W. M. Macek, 12th Chaotic Mo- Ariel Consortium Meeting, 7-9.10. 2019, deling and Simulation International Confe- Utrecht, Holandia rence (CHAOS2019), 18-22.06.2019, Chania, 11. New Tools for the Diagnostics of Small-Scale Irregu- Crete, Greece larities in the Ionosphere, H. Rothkaehl, M. Grze- siak, D. Przepiórka, M. Pożoga, B. Matyjasiak, Other K. Budzińska, R. Wronowski, Scintillating Science: Cutting-Edge Science Achieved 1. Obserwacje bieżących deformacji tektonicznych Through the observations of Radio Scintilla- górotworu Depresji Świebodzic i jej związki z silnymi tions, 14-19. 07.2019, Hermanus, RPA zdarzeniami sejsmicznymi w Monoklinie 12. Planetary geology activities on the Wroclaw side of the Przedsudeckiej, M. Kaczorowski, D. Kasza, R. Space Research Centre, D. MÈGE, First Na- Zdunek, R. Wronowski, Seminarium Nau- tional Martian Seminar, 18.10.2019, Kraków, kowe Wydziału Geodezji i Kartografii Polite- Polska chniki Warszawskiej, 04.02.2019, Warszawa 13. Radio diagnostics, some new aspects, H. Rothkaehl, 2. Aktywność kinematyczna górotworu Depresji Świe- M. Morawski, B. Matyjasiak, M. Pożoga, M. bodzic. Rozkład czasowy silnych zdarzeń sejsmicz- Grzesiak, D. Przepiórka, R. Schreiber, B. Ata- nych w Monoklinie Przedsudeckiej, Niecce Górnoślą- maniuk, M. Marek, R. Wronowski, Disco- skiej oraz Masywie Czeskim z wyszczególnieniem vering Sky at Longest Wavelenght with Small zdarzeń sejsmicznych o skutkach tragicznych, M. satellite Constallation, 20-28.01.2019, Pekin, Kaczorowski, M. Rudnicki, D. Kasza, R. Zdu- Chiny nek, R. Wronowski, Seminarium Zakładu Fi- 14. Recent challenges of space plasma diagnostics in the zyki Litosfery, Instytutu Geofizyki UW, 08. 03. European satellite projects, H. Rothkaehl, Beacon 2019 Satellite Symposium 2019, 18-23. 08.2019, 3. Jak powstał świat? Wielki wybuch czy stworzenie?, Olsztyn, Polska W. M. Macek, Konferencja Interdyscypli- 15. SATELITARNE BIG DATA, S. Lewiński, narna, 01.06.2019, Akademia Pomorska w M. Rybicki, R. Malinowski, E. Gromny, M. Słupsku Krupiński, C. Wojtkowski, M. Jenerowicz, A. 4. Polskie pozaatmosferyczne badania struktur korony Nowakowski, VII Forum BioGIS – System słonecznej: najważniejsze wyniki i plany, J. Sylwe- Informacji Przestrzennej w badaniach różno- ster, XXXIX Zjazd PTA, 11.09. 2019, Olsztyn rodności biologicznej, 21-22.03.2019, Poz- 5. Roboty w przestrzeni kosmicznej, F. Liliana nań, Polska Basmadji, Szkolenie dla Wojskowego Biura Zarzą- 16. Satellite Earth Observation applications for DRR, dzania Częstotliwościami, 21.10. 2019, Warszawa, M. MILCZAREK, Pierwsze Krajowe Forum Polska Ograniczenia Ryzyka Katastrof, 25-26.11. 6. Sygnały tektoniczne rejestrowane w Laboratorium 2019, Warszawa, Polska Geodynamicznym w Książu, R. Zdunek, M. Ka- 17. Monitoring of Space Weather conditions with czorowski, R. Wronowski, Seminarium CBK LOFAR station in Borowiec, H. Rothkaehl, B. PAN/PW, 15.02. 2019, Warszawa Matyjasiak, M. Pożoga, M. Grzesiak, K. Bu- 7. System astronomicznego satelity UVSat, R. dzińska, Ł. Tomasik, R. Wronowski, D. Prze- WAWRZASZEK, Posiedzenie KBKiS, 12.12. piórka, B. Atamaniuk, LOFAR Science 2019, 2019, Warszawa 19-23.05.2019, Lejda,Holandia 8. Aktywności kinematyczna górotworu w Książu 18. Spatio-temporal analysis of LOFAR scintillation (Depresja Świebodzic) w momentach tragicznych measurements, M. Grzesiak, D. Przepiórka, M. zdarzeń sejsmicznych w górnictwie polskim w latach Pożoga, B. Matyjasiak, H. Rothkaehl, K. Bu- 2015-2018, M. Kaczorowski, M. Rudnicki, dzińska, R. Wronowski, LOFAR Science D.Kasza, R. Zdunek, R. Wronowski, Seminar- 2019, 19-23.05.2019, Lejda, Holandia

129 ium Zakładu Geodezji Planetarnej CBK dji, Seminarium CBK PAN, 30.05. 2019, War- PAN, 22 lutego 2019 szawa 9. Projekt ESA e.Deorbit: Rozwój technologii do usu- 23. Multifraktalna i intermitentna natura turbulencji na wania kosmicznych śmieci, Tomasz Rybus, Semi- podstawie pomiarów sondy Ulysses, A. Wawrza- narium CBK PAN, 07.02.2019, Warszawa szek, Seminarium CBK PAN, 06.06.2019, 10. Emisje AKR-podobne w jonosferze - dane z misji Warszawa RELEC i DEMETER, M. Marek, Semi- 24. Obserwacje laserowe śmieci kosmicznych, P. Lejba, T. narium CBK PAN, 14.02.2019, Warszawa Suchodolski, P. Michałek, S. Zapaśnik, J. Bar- 11. Więcej niż slajdy - efektywne prezentacje naukowe, P. toszak, M. Kalarus, S. Schillak, Seminarium Wasylczyk (Wydz.Fizyki UW), Seminarium CBK PAN, 13.06.2019, Warszawa CBK PAN, 21.02.2019, Warszawa 25. The birth and childhood of planetary systems, H. 12. Stanowiskowy aktuator elektromagnetyczny o stero- Rickman, Seminarium CBK PAN, 03.10.2019, wanej impedancji mechanicznej, P. Palma, Semi- Warszawa narium CBK PAN, 28.02.2019, Warszawa 26. Sonda Międzygwiazdowa: pierwszy jasno określony 13. Badania Marsa – misja Insight, P. Witek, Semi- krok ludzkości w drodze do innych gwiazd, R. Rat- narium CBK PAN, 07.03.2019, Warszawa kiewicz, Seminarium CBK PAN, 10.10. 2019, 14. Dynamika nanocząstek pyłu kosmicznego w pobliżu Warszawa Słońca - uwzględnienie korotacji, A. Czechowski, 27. Odszyfrowywanie parametrów termicznych lodowego Seminarium CBK PAN, 14.03.2019, Warsza- regolitu księżycowego w symulacjach MES na bazie wa danych eksperymentalnych, G. Wasilewski, Semi- 15. W poszukiwaniu kulturowej i monetarnej wartości narium CBK PAN, 17.10.2019, Warszawa piksela, E. Woźniak, Seminarium CBK PAN, 28. STEVE – świetlna zagadka i pierwsze sukcesy w jej 21.03.2019, Warszawa wyjaśnianiu, B. Popielawska, Seminarium CBK 16. Co wynika z nowego modelu ciśnienia promieniowa- PAN, 24.10.2019, Warszawa nia w heliosferze?, I. Kowalska-Leszczyńska, Se- 29. Detekcja i klasyfikacja zmian pokrycia terenu na minarium CBK PAN, 28.03.2019, Warszawa zdjęciach satelitarnych bardzo wysokiej rozdzielczo- 17. Modelowanie transferu promieniowania w atmosfe- ści, S. Aleksandrowicz, Seminarium CBK rach kometarnych, S. Szutowicz, 04.04.2019, PAN, 07.11.2019, Warszawa Warszawa 30. Hydrologiczna funkcja pobudzenia bieguna ziem- 18. Simultaneous monitoring of the limited area iono- skiego z obserwacji misji GRACE oraz innych sateli- sphere with the use of GPS and ionosonde, O. Gry- tów na niskich orbitach okołoziemskich, J. Śliwiń- nyshyna-Poliuga, Seminarium CBK PAN, 11. ska, Seminarium CBK PAN, 21.11.2019, War- 04.2019, Warszawa szawa 19. Akcelerometry dla satelitów Galileo drugiej generacji, 31. Mechanizm rekoneksji magnetycznej na skalach ki- M. Kalarus, Seminarium CBK PAN, 09. 05. netycznych na podstawie danych z misji MMS, W. 2019, Warszawa Macek, Seminarium CBK PAN, 28.11. 2019, 20. Walidacja robotów kosmicznych w warunkach neu- Warszawa tralnej pływalności, P. Zagórski (AGH), Se- 32. Zaburzenia w jonosferze rejestrowane przez satelity minarium CBK PAN, 16.05.2019, Warszawa DEMETER i Swarm w czasie burz magnetycznych 21. Symulacje numeryczne procesów kriowulkanicznych i atmosferycznych - podobieństwa i różnice, J. Błęcki, jako narzędzie projektowania kamery wielospek- Seminarium CBK PAN, 05.12.2019, War- tralnej w misji Enceladus Orbiter, N. Zalewska, Se- szawa minarium CBK PAN, 23.05.2019, Warszawa 33. Komety z Obłoku Oorta, M. Królikowska-Soł- 22. Stanowisko testowe w CBK do walidacji algorytmów tan, Seminarium CBK PAN, 12. 12.2019, War- sterowania robotem kosmicznym, F. Liliana Basma- szawa

130 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. Udział Polski w projekcie LOFT; kit; Polish participation in LOFT mission; (Barylak Jaromir, grant - PRELUDIUM, TT/ (Michalska Małgorzata, projekt międzynaro- 248/2016) dowy niewspółfinansowany, TT/196/14) 8. Mobilność nieholonomicznych robotów 2. Analiza modeli ziemskich ośrodków ciekłych kosmicznych w obecności przestrzennie oraz modeli klimatycznych CMIP celem ich rozległych przeszkód posiadających moment weryfikacji pod względem zgodności ich eks- pędu "NONHOLONOMIC"; cytacji ruchu bieguna z obserwowanymi zmia- Mobility Of A Nonholonomic Space nami tego ruchu; Robot Constrained By Large Movable Ob- Analysis of geophysical surficial fluids stacles; models and CMIP climate models for ve- (Sąsiadek Jerzy, grant własny, TT/259/2016) rification of polar motion excitation fun- 9. V-MACS: Nowy obraz gigantycznego mar- ctions in terms of their compatibility with sjańskiego systemu kanionów; changes in the observer polar motion; V-MACS - Novel views of the Martian (Nastula Jolanta, grant własny, TT/216/15) giant canyon system; 3. Powstawanie pęcherzyków w skorupie obto- (Mege Daniel, grant własny, TT/261/16) pieniowej meteorytów eukrytowych; 10. Polski wkład w przygotowanie i przeprowa- Formation Of Vesicles Within The Fusion dzenie programu badawczego projektu CTA Crust Of Eucritic Meteorites; w pierwszej fazie działania; (Nicolau-Kuklińska Agata, grant - PRELU- Polish input into preparation and realiza- DIUM, TT/247/2016) tion of the first phase of CTA scientific 4. Polski udział w misji kosmicznej NASA Inter- program; stellar Boundary Exploret (IBEX): Skąd po- (Seweryn Karol, projekt międzynarodowy chodzi ciepła bryza i jaki ma związek z asyme- niewspółfinansowany, TT/271/2017) trią heliosfery?; 11. Ocena przydatności formalizmu multifrak- Polish Participation In The Nasa Space talnego w przetwarzaniu i analizie optycznych Mission Interstellar Boundary Explorer obrazów teledetekcyjnych; (Ibex): What In The Source For The Evaluation of the usefulness of multifra- Warm Breeze And How Is It To The ctal formalism in the processing and Asymmetry Of The Heliosphere?; analysis of optical remote sensing images; (Bzowski Maciej, projekt międzynarodowy (Wawrzaszek Anna, grant własny, TT/273/ niewspółfinansowany, TT/250/2016) 2017) 5. Udział Polski w naukowym rozwoju nowego 12. Badanie stanu plazmy w rozbłyskach słone- teleskopu rentgenowskiego ATHENA; cznych na podstawie analizy widm rentgenow- Polish Contribution In Scientific Develop- skich uzyskanych za pomocą przyrządu Bent ment New XRay Telescope ATHENA; Crystal Spectrometer z pokładu satelity (Rataj Mirosław, projekt międzynarodowy NASA Solar Maximum Mission; niewspółfinansowany, TT/255/2016) Investigation of physical conditions in 6. Ośrodek międzygwiazdowy w okolicy Słońca: flaring plasma based on the analysis of X- wnioski z analizy obserwacji strumieni ato- ray spectra observed by Bent Crystal Spec- mów neutralnych; trometer on NASA Solar Maximum Mis- Interstellar medium in the vicinity of the sion satellite; Sun: inferences from analysis of the flux (Sylwester Barbara, grant własny, TT/286/18) of neutral atoms; 13. Reprezentatywność globalnych ocen zachmu- (Bzowski Maciej, grant własny, TT/256/ rzenia z satelitarnych misji lidarowych i rada- 2016) rowych (LiRa-C); 7. Rentgenowski spektrometr obrazujący STIX: Representativeness of global lidar and

131 radar climate record on clouds (LiRa-C); 3. Satelitarna identyfikacja i monitorowanie (Kotarba Andrzej, grant własny, TT/284/18) upraw na potrzeby statystyki rolnictwa - SAT- 14. Badanie zmian parametrów fizycznych górnej MIROL; jonosfery wywoływanych wyładowaniami ele- Remote sensing based crop detection and ktrycznymi w atmosferze; monitoring for agricultural statistics - The studies of the changes of the upper SATMIROL; ionospheric physical parameters caused (Woźniak Edyta, TT/308/19) by electric discharges in the atmosphere; (Błęcki Jan, grant własny, TT/293/18) Ministry of Science and Higher 15. Badanie rozbłysków słonecznych na podsta- Education Grants wie obserwacji wykonanych za pomocą pol- skiego spektrofotometru SphinX; 1. Europlanet 2020 Infrastruktura Badawcza; The investigations of solar flares based on Europlanet 2020 Ressearch Infrastru- the data of Polish spectrophotometer cture; SphinX; (Tomasik Łukasz, wsparcie uczestnictwa jed- (Gryciuk Magdalena, grant - ETIUDA, nostki w programie HORYZONT 2020, TT/ TT/298/18) 232-M/17) 16. Struktura wiatru słonecznego - kto ma rację?; 2. LOFAR dla Pogody Kosmicznej; Solar wind structure - who is right?; LOFAR for Space Weather; (Kowalska-Leszczyńska Izabela, SONATA, (Rothkaehl Hanna, wsparcie uczestnictwa TT/322/19) jednostki w programie HORYZONT 2020, 17. Analiza zgodności hydrologicznych funkcji TT/288-M/18) pobudzenia bieguna ziemskiego otrzymanych 3. Wprowadzanie innowacji w zarządzaniu z danych misji GRACE i GRACE Follow-On kryzysowym w Europie (DRIVER+); z hydrologicznym sygnałem w obserwowa- DRiving InnoVation in crisis manage- nym pobudzeniu ruchu bieguna ziemskiego; ment for European Resilience + (DRI- Analysis of agreement between hydrolo- VER+); gical polar motion excitation functions (Foks-Ryznar Anna, międzynarodowy współ- obtained from GRACE and GRACE finansowany, TT/274-M/18) Follow-On missions with hydrological si- 4. Identyfikacja nieużytków rolnych w Europie i gnal in observed polar motion excitation; rozbudowa ich potencjału jako obszaru sek- (Śliwińska Justyna, PRELUDIUM,TT/319/ wencji CO2 - MAIL; 19) Identifying Marginal Lands in Europe and strengthening their contribution po- National Centre for Research tentialities in a CO2 sequestration stra- and Development Grants tegy — MAIL; (Woźniak Edyta, międzynarodowy współ- 1. Penetrator planetarny z systemem pobierania finansowany, TT/307-M/19) gruntu na misje Luna-Resurs 1; Planetary penetrator equipped with a soil EU Programme Grants sampling system intended for the Luna- Resurs 1 mission; 1. Europlanet 2010 Infrastruktura Badawcza; (Barciński Tomasz, TT/214/15) Europlanet 2020 Research Infrastructure; 2. Woda w glebie - monitoring satelitarny w po- (Tomasik Łukasz, HORYZONT 2020, TT/ prawie retencji wodnej przy użyciu biowęgla 232/15) (SoilAqChar); 2. Wspieranie innowacyjności w zarządzaniu Water in soil - satellite monitoring and im- kryzysowym – DRIVER; proving the retention using biochar (Soil- Driving Innovation in Crisis Management AqChar; for European Resilience; (Słomiński Jan, BIOSTRATEG, TT/285/18) (Foks-Ryznar Anna, 7PR, TT/274/15)

132 3. EXOMHYDR – Wpływ systemów magmo- (Nawrocki Jerzy, HORYZONT 2020, TT/ wych i tektoniki na aktywność hydrotermalną 318/19) na Marsie w świetle badań misji ExoMars/ 12. Umowa na wykonanie usługi badawczo- TGO: warunki dla obecności życia i zasobów rozwojowej - opracowania studium wykonal- naturalnych; ności ruchomego zwierciadła wtórnego do EXOMHYDR – Magmatic plumbing sys- aktywnej korekcji frontu falowego w modu- tems and tectonic control of hydrother- łowym teleskopie Deploscope; mal activity on Mars revealed by Exo- Contract for the provision of research and Mars/TGO: constraints for life and development services - development of a resources; feasibility study for a mobile secondary (Mege Daniel, POIR,TT/280/17) mirror for active correction of the wave- 4. System operacyjnego gromadzenia, udostęp- front in the DeploScope modular telesco- niania i promocji cyfrowej informacji sateli- pe; tarnej o środowisku (Sat4Envi); (Barciński Tomasz, POIR, TT/317/19) System of operational collection, sharing, 13. Umowa na wykonanie usługi badawczo- and promotion of digital satellite data rozwojowej - opracowania komputerowego about the environment (Sat4Envi); układu optycznego dla modułowego telesko- Foks-Ryznar Anna, POPC, TT/283/17) pu Deploscope; 5. LOFAR dla Pogody Kosmicznej; Contract for the provision of research and LOFAR for Space Weather; development services - development of a (Rothkaehl Hanna, HORYZONT 2020,TT/ computer optical system for the modular 288/18) Deploscope telescope; 6. Centrum Referencyjne Galileo-Krajów czło- (Wawer Piotr, POIR, TT/316/19) nkowskich; 14. Umowa na wykonanie usługi badawczo-roz- Galileo Reference Centre - Member Sta- wojowej - opracowanie studium wykonalnosi tes; komputerowego modelu geometrycznego (Świątek Anna, GNSS, TT/296/18) konstruckji nosnej i fukncyjnej w modulowym 7. Komputery pokładowe dla platform i teleskopie Deploscope; ładunków satelitarnych w przyszłych Contract for the provision of research and mikrosatelitach; development services - development of a Future control and data handling unit for computer optical system for the modular platforms and payloads for microsatelli- Deploscope telescope; tes; (Barciński Tomasz, POIR, TT/315/19) (Orleański Piotr, POIR,TT/300/18) 15. Modularne Detektory GEM; 8. Wsparcie Monitorowania Wyników Systemu Modular GEM Detectors; EGNOS; (Kowaliński Mirosław, POIR, TT/326/19) EGNOS Service Performance Monitoring 16. Wykonanie usług badawczych w zakresie wy- suport (SPMS); konania analiza wykorzystania wielospektral- (Świątek Anna, GNSS, TT/311/19) nych metod pomiarowych oraz budowy ka- 9. Future Space; mery przystosowanej do identyfikacji patoge- (Gabryszewski Ryszard, Erasmus+, TT/327/ nów pomidora z pokładu drona; 19) Research services in the field of multi- 10. Konstrukcja odbiornika czasowego Galileo spectral measurements application and do zastosowań o znaczeniu krytycznym; camera construction for tomato patho- Development of a Galileo-based timing gens detections from drones; receiver for critical infrastructures; (Krupiński Michał, POIR, TT/312/19) (Nawrocki Jerzy, GNSS, TT/324/19) 17. Identyfikacja nieużytków rolnych w Europie i 11. Trwałe zegary optyczne dla międzynaro- rozbudowa ich potencjału jako obszarów sek- dowych skal czasu (ROCIT); wencji CO2 - MAIL; Robust Optical Clocks for International Timescales;

133 Identifying Marginal Lands in Europe Scientific Exploitation of Operation Mis- and strengthening their contribution po- sions (SEOM) S2-4sci Land and Water, tentialities in a O2 sequestration strategy' Study 3: Classification; — 'MAIL; (Lewiński Stanisław, TT/246/15) (Woźniak Edyta, HORYZONT 2020,TT/ 8. Eksperckie centra pogody kosmicznej: defi- 307/19) nicja i rozwój; 18. Centrum Referencyjne Galileo-Krajów człon- Space Weather Expert Service Centres: kowskich; Definition And Development; Galileo Reference Centre - Member Sta- (Dziak-Jankowska Beata, TT/254/16) tes; 9. Lekki, kompaktowy system optyczny bazujący (Świątek Anna, GNSS,TT/296.1/19) na DOE i Elementach asferycznych (DOE); A Lightweight, compact optical system ESA Grants based on DOE; (Rataj Mirosław, podwykonawstwo, TT/275/ 1. Zespół koła z filtrami i polaryzatorami; Stero- 17) wnik koronografu dla misji PROBA3; 10. HIPERO: Rekonfigurowalny Komputer Po- PROBA 3 Coronagraph Control Box (P3 kładowy o Dużej Mocy Obliczeniowej; CCB) Filter Wheel Assembly & Polarisers HIPERO: High Performance Reconfi- (FWA); gurable OBC; (Baran Jędrzej, TT/193/15) (Cichocki Andrzej, TT/279/17) 2. Polski udział techniczny w fazie D projektu 11. LOOP - Lądując raz na Fobosie; STIX/Solar Orbiter (STIX-D); LOOP - Landing Once On Phobos; Polish Technical Participation in Phase D (Barciński Tomasz, TT/281/18) of STIX/Solar Orbiter; 12. Testowanie potencjału rozwiązania PaaS (plat- (Skup Konrad, PRODEX, TT/198/14) forma jako usługa) dla segmentu jonosfery- 3. Robotycznie wspierane lądowanie (REST); cznego domeny pogody kosmicznej; Robotically Enhanced Surface Touch- Testing the Potential of the PaaS (plat- down (REST); form as a Service) Solution for Ionosphe- (Seweryn Karol, TT/204/14) ric Segment of the Space Weather Domain 4. Badanie związków między nocnym wzrostem (SW satellite); koncentracji plazmy jonosferycznej a zmien- (Dziak-Jankowska Beata, TT/292/17) nością pola magnetycznego; 13. WFI (WIDE FIELD IMSAGER) na pokła- Investigation of the linkage between dzie satelity ATHENA. Projekt i wykonanie ionospheric plasma night-time density dwóch podsystemów: Filter Wheel Assembly- enhancements and magnetic field variabi- FWA (Zespół Koła Z Filtrami) oraz Power lity; Distribution Unit -PDU (System Rozdziału (Błęcki Jan, TT/212.1/18) Mocy); 5. Polska realizacja instrumentu RPWI dla misji Wfi (Wide Field Imager) On Board Of JUICE; Athena (Advanced Telescope For High Overall contribution to the RPWI instru- Energy Astrophysics) Satellite. Design ment for JUICE mission; And Manufacture Of Two Subsystems: (Rothkaehl Hanna, TT/217.1/14) Filter Wheel Assembly (FWA) and Power 6. Jupiter Icy Moons Explorer (JUICE) Submil- Distribution Unit (PDU); limetre Wave Instrument - misja ESA L2; (Barciński Tomasz, TT/294/18) Jupiter Icy Moons Explorer (JUICE) 14. Rolnictwo w Polsce. System informacji sta- Submillimetre Wave Instrument - misja tystycznej dla rolnictwa w oparciu o dane sa- ESA L2; telitarne / Eostat; (Skup Konrad, TT/223/13) Agriculture Poland. Services for Earth 7. Wykorzystanie Naukowe Operacyjnych Misji Observation- Based Statistical Informa- Obserwacyjnych (SEOM) S2-4Sci Woda i tion for Agriculture / Eostat; Lądy, Studium 3: Klasyfikacja; (Woźniak Edyta, TT/295/18)

134 15. Odbiornik GNSS dla małych rakiet nośnych i 25. P3-SST-XII Akwizycja Danych z Sensorów mikro-satelitów na bazie radia programowal- SST; nego; P3-SST-XII SST Sensor Data Acquisition; Sw defined radio GNSSW receiver for (Lejba Paweł, TT/306/19) micro-launchers and micro-satellites; (Wawrzaszek Roman, TT/297/18) Projects supported by other 16. Serwis monitoriningu obszarow zabudowa- nych Mazowsza/BAMS-Mazovia; Polish organizations and Built-up Areas Monitoring Service for institutions Mazovvia/BAMS-Mazovia; 1. Dostarczanie danych obserwacyjnych GPS, (Malinowski Radosław, podwykonawstwo, pochodzących ze stacji referencyjnej BOR1 TT/301/18) znajdującej się w Borowcu; 17. Udział techniczny w projekcie Athena/XIFU; Providing GPS observational data from Technical Participation in Athena/XIFU; reference stations BOR1 located in Boro- (Skup Konrad, PRODEX, TT/302/18) wiec; 18. Planowanie obserwacji SST przez Internet; (Lejba Paweł, TT/7.11/08) WebPlan: Web-based sensor planning 2. Bieżące opracowanie zestawu danych helio- tools SST; geofizycznych do prognozowania warunków (Lejba Paweł, TT/303/18) łączności radiowej oraz rozwój metodyki i 19. Fine Guidance System (FGS) misji ESA systemów prognozowania warunków łącz- ARIEL (Atmospheric Remote-sensing ności radiowej; Infrared Exoplanet Large-survey) – M4 The current development of a heliophysic mission. Faza B1- FGS/ ARIEL; data set to predict conditions of the radio (Rataj Mirosław, PRODEX, TT/309/18) communication and the development of 20. ATHENA WFI PDU; methodologiest and forecasting systems (Skup Konrad, PRODEX, TT/331/19) of radio communication conditions; 21. LARAMOTIONS - Studium Ewolucji (Dziak-Jankowska Beata, TT/67.7/18) Sensora; 3. Opracowanie systemu pozycjonowania i LARAMOTIONS - Laser Sensor Evolu- kontroli orientacji satelity (AOCS - Attitude tion Study; and Orbital Control Systems) dla platformy (Lejba Paweł, TT/321/19) satelitarnej HyperCube budowanej w ramach 22. Highland terrain hopper Galago – opraco- Projektu Renesans; wanie innowacyjnego systemu mobilności Design and development of positionning planetarnej do terenów górskich; and orientation control system (AOCS - Highland terrain hopper – cutting edge Attitude and Orbital Control Systems) for planetary locomotion system (Galago); HyperCube satellite platform under de- (Gurgurewicz Joanna, TT/314/19) velopment in a frame of Renesans project; 23. Geodezyjny SAR dla unifikacji systemu wy- (Wawrzaszek Roman, TT/287/18) sokości Bałtyku i badań poziomu Morza Bał- 4. Rozwój Badań Kosmicznych; tyckiego; (Denis Mirosław, program Akademickie Part- Geodetic SAR for Baltic Height System nerstwa Międzynarodowe, TT/305/18) Unification and Baltic Sea Level Re- 5. Dostarczenie i przetworzenie danych obser- search; wacyjnych i kalibracyjnych z infrastruktury (Nastula Jolanta, TT/313/19) obserwacyjnej oraz sensora 24. Rolnictwo w Polsce. System informacji sta- (Lejba Paweł, TT/330/19) tystycznej dla rolnictwa w oparciu o dane sa- 6. Chematics Analisys Software Alpha wersja telitarne/ ACCESS-4FI; alpha; ACCESS-4FI-Autmated Crop Classifica- Schematics Analysis Software Alpha; tion and yield Estimation online ServiceS (Cichocki Andrzej, TT/328/19) for Food Industry; 7. Projekt, pomiar techniką GNSS i opracowanie (Woźniak Edyta, TT/310/19)

135 szczegółowej osnowy dwufunkcyjnej na 2. Budowa strefy bezpieczeństwa w Borówcu terenie powiatu lubartowskiego - część II; (Lejba Paweł) Project, GNSS measurement and compu- 3. Budowa Systemu nr 2 stacji laserowej CBK tation of bifunctional network in the PAN w Borówcu Lubartów county; (Lejba Paweł) (Jaworski Leszek, TT/323/19) 4. Analizy pomiarów i modelowanie atmosfery i powierzchni Marsa Projects supported by other (Kofman Włodek) foreign organizations and institutions Monitoring the sustainability of the projects co-financed 1. Techniczna obsługa stacji EGNOS-RIMS; Technical service of the EGNOS-RIMS from European funds station; (Jaworski Leszek, TT/13.3/13) CBK PAN monitors the projects co-financed 2. Jonosonda LAERT; from European structural funds after the com- LAERT Ionosonde; pletion of their implementation in the life of the (Rothkaehl Hanna, TT/68/10) project. The monitoring covers the output and 3. STIX IDM "Dummy” outcome indicators as outlined for each projects. (Skup Konrad, TT/325/19) The following projects are under monitoring: 4. Udział i nadzór nad testami wstrząsowymi 1. PROTEUS. Integrated mobile system for urządzenia EBOX w firmie Astro- und Fein- counterterrorism and rescue operations (POIG). verktechnik Adlershof GmbH; 2. Future control and data handling unit for Participation and supervision over vibra- platforms and payloads for microsatellites tion testing of EBOX device at Astro- und (TEAM TECH FNP). Feinverktechnik Adlershof GmbH, Berlin 3. EXOMHYDR. Magnetic plumbing systems Germany, hereinafter "Astrofein"; and tectonic control of hydrothermal activity on (Rothkaehl Hanna, TT/320/19) Mars revealed by ExoMars/TGO constraints for life and resources (TEAM FNP). Projects supported by the 4. SAT4ENVI. System operacyjnego gromadze- nia, udostępniania i promocji cyfrowej informacji state budget: satelitarnej o środowisku (POPC 2.3).

1. PECASUS, PAN- European Consortium for (M. Michalska) Aviation Space Weather User Services (Tomasik Łukasz)

136 GENERAL INFORMATION Staff fessor title from the President of the Republic of Poland. Agnieszka Gil-Świderska was advanced At the end of 2019 the Centrum Badań Kosmi- with PhD, DSc degree. Sebastian Aleksandro- cznych, PAN employed 212 persons of whom 18 wicz was advanced with PhD degree. are professors, 15 habilitated doctors and 42 PhD (H. Żurek) research associates. Jerzy Sąsiadek received pro- Finances – preliminary estimates The state budget of Centrum Badań Kosmicz- 4% national grants, 14% EU framework pro-jects, nych, PAN, in 2019 was 11.044 thousand PLN 32% contracts (national and international, ESA), while total was 31.876 thousand PLN. The budget 15% other sources. structure was following: 35% basic allocation, (W. Roszkowska) Grants and Contracts Centrum Badań Kosmicznych PAN in 2019 was (NCBiR), 25 from ESA, 18 from EU Programme involved in 82 projects including 4 from the including 8 funded by the EU Structural Funds, 4 Ministry of Science and Higher Education from the state budget and 11 other contracts. (MNiSW), 17 from the National Science Centre (A. Kamińska) (NCN), 3 from the National Centre for Research Intellectual Rights Management Policy Polish Patent No 233151 Assignee: Centrum Badań Kosmicznych PAN, Title: Linowy mechanizm przechwytujący śmieci Akademia Górniczo-Hutnicza kosmiczne oraz sposób przechwytywania sateli- Developer: K. Seweryn, K. Grassmann, T. Ku- tów za pomocą linowego mechanizmu ciński Assignee: Centrum Badań Kosmicznych PAN RPA Patent No 2015/08517 Developer: Tomasz Pałgan Title: Electromagnetic drive, the winding core and European Patent No 3063776 method for manufacturing the electromagnetic Title: Electromagnetic drive and method of drive production thereof Assignee: Centrum Badań Kosmicznych PAN Assignee: Centrum Badań Kosmicznych PAN Developer: J. Grygorczuk, Ł. Wiśniewski, M. Developer: J. Grygorczuk, Ł. Wiśniewski, M. Do- Dobrowolski, B. Kędziora browolski, B. Kędziora RPA Patent No 2015/08518 European Patent No 3093427 Title: Clamping Mechanism, Locking Arrange- Title: Drive for tubular member, curling strip and ment and Method of Operating a Reconfigurable tubular boom Manipulator Assignee: Centrum Badań Kosmicznych PAN Assignee: Centrum Badań Kosmicznych PAN Developer: K. Seweryn, K. Grassmann Developer: K. Seweryn, T. Kuciński RPA Patent No 2015/07066 Title: Drilling head driving device, spragging (M. Michalska) mechanism and drilling method Awards Tomasz Rybus - one of the winners of the 10th edition of the Program LEADER of the NCBiR (National Center for Research and Develop- ment).

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

138 demy; 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 experiment RPWI (Radio Plasma Waves Investi- Deblin; 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 toge- Tohoku University, Sendai, Japan; Space and ther institutions and companies from over 14 co- Atmospheric Physics group at Imperial College untries 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, tech- Polytechnique, France; Observatoire de Paris; nology 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; Uni- National Centre of Radioastronomy and versity of Oulu, Finland; Sodankyla Geophysical Engineering; 2012; technical science, space ex- Observatory, Finland; University College Lon- ploitation, 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 Aeronomy, Brussels, Belgium; Centrum Badań University of Technology, Centrum Badań Kos- Kosmicznych Polskiej Akademii Nauk, Warsaw, micznych PAN, Jagiellonian University, University Poland; Technical University of Denmark, Na- of Zielona Góra, Nicolaus Copernicus Astrono- tional 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 Kosmi- Sciences; Polish Academy of Sciences Faculty of cznych Polskiej Akademii Nauk, Geophysics Physics and Applied Informatics (University of Institute PAS, Institute of Geological Sciences Łódz); The Henryk Niewodniczanski Institute of PAS, Institute of Oceanology PAS, Nicolaus Nuclear Physics (Polish Academy of Sciences); Copernicus 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 Elec- France, Observatoire de Paris, LERMA, France, trical Engineering, Automatics, Computer Scien- Chalmers, Sweden, University of Bern, Switzer- ce and Biomedical Engineering (Polish Academy land, NICT, Japan, Omnisys Instrument AV, of Sciences). Sweden, Radiometer Physics GmbH, Centrum

139 Polish Consortium of the Project "Athena- www.asgeupos.pl/index.php?wpg_type=syst_de PL” 2018, CBK PAN, CAMK PAN, Centrum scr&sub=ref_st. Fizyki Teoretycznej PAN, Narodowe Centrum EUROLAS – EUROpean LASer Network, 1989, Badań Jądrowych, Uniwersytet Jagielloński, Uni- coordination of satellite and lunar laser mea- wersytet Wrocławski, Uniwersytet w Białym- surements and observational campaigns carried stoku, Uniwersytet Jana Kochanowskiego Kielce, out by European stations, 16 stations:http//ilrs. Uniwersytet Zielonogórski, Uniwersytet Mikołaja gsfc.nasa.gov/network/stations/active/index. Kopernika, Uniwersytet Szczeciński, Uniwersytet html Łódzki. Satellite Geophysics, 2005, satellite geophysics, Polish Consortium of the Project "UVSat” IG PAN, IGIK, CBK PAN, UW, PW. 2018, CAMK PAN, CBK PAN, Creotech International Laser Ranging Service; 1997; Instruments. coordination of satellite and lunar laser stations, analysis centers, laser technology data banks, 42 CBK PAN is part of scientific laser stations, 29 Analysis centers, 2 Data banks. networks, among them: National Center for Space and Satellite En- AirClim-Net, 2005, problems of atmospheric gineering; 2013; space and satellite engineering, pollution and climate change, http //www.airclim Military University of Technology in Warsaw, -net.eu/ Centrum Badań Kosmicznych Polskiej Akademii ASG-EUPOS – Active Geodetic Network - Eu- Nauk; ropean POsition determination System, ..., coor- International Space Environment Service - dination of GNSS measurements and their tran- ISES; 1977; cosmic weather; 22 local branches lo- sfer in real time to the computing center; 126 cated around the world, Regional Warning Cen- stations, full description available at the: http// ters (RWC), e.g. RWC Warsaw. CBK PAN organized and co-organized conferences and meetings: National: International: 1. IX seminarium Sekcji Teledetekcji KBKiS 1. ARIEL FGS CBK Progress Meeting; Warsza- PAN, Obserwacje satelitarne, przykłady wa; 3-4.09.2019 zastosowań, część IV; Warszawa; 21.05.2019 2. NOMAD Science Working Team #15 mee- 2. X seminarium Sekcji Teledetekcji KBKiS PAN ting; Wrocław; 12-13.09.2019 Obserwacje satelitarne, przykłady zastosowań, 3. ARIEL Payload Consortium Meeting; Wro- część V; Warszawa; 9.12.2019 cław; 19-21.09.2019 4. Polish-China consultations on X-ray detectors background modeling and analysis; Wrocław; 19-21.09.2019 5. FUTURE SPACE Kick-off Meeting; Warsza- wa; 12-13.11.2019 6. PROGRESS ON SPECTROSCOPY AND IMAGING III; Wrocław; 19-21.11.2019 7. eXTP LAD PSU-Digital Electronic Meeting; Warszawa; 16-17.12.2019

140 EDUCATIONAL AND PROMOTIONAL ACTIVITIES

Doctoral studies created. There was also presentation of the developed interactive space robot simulator. We There were 18 students in the Doctoral Studies in ran educational games and activities for children, Centrum Badań Kosmicznych PAN in 2019, 2 and for older audience there were talks and new students were admitted in 2019. presentations prepared, including scientific Trainings and internships instruments developed at CBK PAN and currently working in space on various satellites in CBK PAN also on the ISS International Space Station. It was 55 external scientists, engineers and students possible to move a robotic arm in space in a participated in the trainings and internships in computer game and try to 'catch' another object various research groups and laboratories of CBK (eg space debris). PAN in 2019. On Open Day, our employees presented 3 popular science lectures: 'Secrets of the Solar System' - Ry- List of activities undertook by the szard Gabryszewski, 'Life in Space' - Paweł Wajer employees of Centrum Badań and 'Far-reaching Voyager missions' - Romana Rat- kiewicz. There were also astronomical shows Kosmicznych, PAN: completeed at the CBK PAN by the Planetarium SCIENCE FESTIVALS AND PICNICS of the Educational Centre 'Planeta Anuka.' 23rd Science Picnic in Warsaw, 11.05.2019 - this In 2019, the Warsaw Science Festival included an year's main theme was "We and Machines". CBK Asteroid Day organized by the CBK PAN (23 – 24 PAN prepared two shows for the May Picnic: September 2019). This was an opportunity for The first show was entitled 'Why don't satellites scientists from the Solar System Dynamics and fall to Earth?' We showed our audience how this Planetology Department (SSDP), together with process works. The show presented the move- Małgorzata Michalska and Paweł Z. Grocho- ment of the satellite (suspended on a long line) walski to give a series of lectures, accompanied by around a globe placed under the suspension point. practical demonstrations. The satellite could be set in motion at different In another effort to disseminate knowledge about initial speeds: too small speed led falling on the asteroids, and encourage people from Warsaw to globe, large enough brought it into the "orbit" participate in this event, a special website, dedica- around the globe on which it was able to make at ted to asteroids, was developed by Andrzej Kotar- least a few laps. The show was complemented by ba and researchers from the Department (http:// photos and recordings of real Earth satellites. dzienplanetoid.pl/). The following lectures were The second show was carried out with a device given: “Asteroids are everywhere” - Małgorzata used to extract water from the crater of the Moon Królikowska-Sołtan, “Cosmic catastrophes” (Ry- along with the basic subsystems: the PACK- szard Gabryszewski), “ Gravitational game of pla- MOON measuring system mounted on the rover nets and asteroids” (Piotr Witek), „ How many and the regolith extraction and processing/ moons does the Earth actually have?” (Paweł analysis system. Wajer), „Why comets and asteroids are so In addition, there were crosswords, games and different from each other, and yet sometimes we activities for children at the Picnic, including can't tell them apart?” (Sławomira Szutowicz). creating your own comet, rocket and satellite. There were also presented the shows: „Creating a 23rd Warsaw Science Festival 2019, 22.09.2019 comet” and „ How impact craters are created”. nd CBK PAN held an Open Day event. On this day 22 Lower Silesian Science Festival 2019 our employees were talking, also to the youngest Researchers from the Solar Physics Division gu-ests, about many subjects; among others about participated in the XXII Lower Silesian Science Mars, our nearest neighbour in the solar system - Festival (Dolnośląski Festiwal Nauki 2019) and what this planet is like, how we study it and how the third World Space Week. They also organized we get to know it. an exhibition space instrumentation constructed There were workshops on how the comet's nu- at Wrocław. cleus is formed and how impact craters are

141 VISITS AT CBK PAN and “How much does a man weigh in space?” (P. In 2019, there were numerous groups of children Lejba). The most important event was a night laser and youth in CBK PAN, as well as students show at Borowiec (21 September 2019), which (among them students of the university of the presented the capabilities of the station's satellite/ third age) and employees of various Polish and space debris lasers. foreign companies cooperating with CBK PAN. Agnieszka Gil-Świderska gave the lecture “Space During these visits, guests had the opportunity to weather and Polish energy infrastructure” during see our laboratories and learn about the work 21st Science and Arts Festival in Siedlce, 17-20 carried out in the Centre. Talks and lectures were October 2019. prepared for pupils and students. In total we have hosted 20 different groups. These included IAU100 National Committee dedicated lectures and talks on “On a collision In 2019, the International Astronomical Union course“, “Danger from Space", “Asteroids (IAU) celebrated its 100th anniversary. To com- threatening the Earth” (R. Gabryszewski), “Life memorate this milestone, it organised a year-long in space” (P. Wajer), “Wave experiments” (M. celebration to increase awareness of a century of Morawski), “First Polish Scientific Satellites Brite- astronomical discoveries, and to support and im- PL” for students of University of the third age, prove the use of astronomy as a tool for educa- “What membership in ESA gives us”, “How tion, development and diplomacy, around the satellites and space instruments are created” and central theme 'Under One Sky'. “What we do at CBK PAN” (M. Michalska). The centennial celebrations stimulated worldwide Also in the Borowiec Observatory there were nu- interest in astronomy and science and reached out merous visits and lectures for independent scho- to the global astronomical community, national ols, university students and many different guests. science organisations, societies, policy-makers, students, families and the general public. LECTURES AND TALKS OUTSIDE OF Ryszard Gabryszewski became one of the IAU CBK PAN 100 National Committee members in Poland, and Other science picnics represented the Centrum Badań Kosmicznych Natalia Zalewska and Piotr Witek participated in PAN. th 5 Science Picnic of PAN in Olsztyn on 8 May Astronomers in schools 2019. They had there shows and presentations Ryszard Gabryszewski, Małgorzata Królikowska “How we examine Mars” and “Why don't and Paweł Wajer took part in this international satellites fall to Earth?”. project, coordinated in Poland by the Polish Fatina Basmadji and Joanna Rothkaehl have talked Astronomical Society (https://www.pta.edu.pl/ about CBK PAN work during Lubuskie astronomers-in-schools/). M. Królikowska gave th Voivodeship Day, 15 of June 2019. two popular talks about the Solar System and Małgorzata Królikowska was invited to partici- exoplanet orbiting of solar-type stars (to the pate in the 10th Pogórze Science Attractions (X primary school in Ortel Książęcy, eastern Poland, Pogórzańskie Atrakcje Naukowe), a family science and the Małachowianka' secondary school in picnic held in Łużna, southern Poland (14–15 Płock, central Poland), and took part in two dis- September 2019). During the picnic, she gave a cussions with pupils and teachers about astro- talk about comets accompanied by the experiment nomy and its role in education. P. Wajer gave three entitled “Creating a Comet in Earth's conditions”. popular lectures in two schools in Warsaw and the The BORL team from Borowiec has actively town of Wołomin. participated in the popularisation of science. The Seminars and other popular science lectures most notable activities in 2019 included Kórnik Hans Rickman led a series of four seminars in Science Days (Kórnickie Dni Nauki), 19–21 Sep- October–November 2019 at the Centrum Badań tember 2019. Several theoretical classes were gi- Kosmicznych PAN. Topics related to the small ven at the Observatory and in local schools by bodies of the Solar System and their early BORL staff: “Why do we need artificial satellites”

142 dynamical evolution, including the gravitational highlight the econo-mic and social benefits of effects of the Sun's birth cluster. In March 2019, space exploration, and expose participants to he gave two lectures about cosmogony at career paths that are avai-lable to both STEM Stockholm Senior University and, in December specialists, and graduates in law and social 2019, a popular talk titled Meteorites – Eye sciences. Witnesses of the Birth of the Planets at Köping in The Project is based on a wide range of training Sweden. programmes, which draw upon the expertise of its Ryszard Gabryszewski gave a series of lectures partners: the Computer Assisted Education and about the problem of collisions in the present-day Information Technology Centre (OEIiZK), War- Solar System at a secondary schools in Warsaw. He szawa, Poland; the NEMO Science Museum, Am- also gave a talk “Research on comets and the sterdam, the Netherlands; the NOESIS Science development of science (from Babylonian times Centre at Thessaloniki, Greece; and the Polish to the present day)” at XXXV Bolesław Prus Space Agency in Gdańsk, Poland. The consortium Secondary School in March 2019. Romana is led by the CBK PAN. Ratkiewicz gave the lectures in secondary school The Project is headed by R. Gabryszewski, and is in Nadarzyn, the lectures were related to the co-financed by the European Union Erasmus+ planned sending of Interstellar Probe by NASA. Programme. It was launched on 1st October 2019, Tomasz Mrozek gave the lectures for young and and will run over 30 months. older students: “Sizes and distances in the Solar System”, “The end of the X-ray carousel: Application to confer doctoral degrees in the RHESSI 2002-2018” and “Awakening of the discipline of Astronomy Sun”. Jakub Ciążela gave two lectures to the In 2019, the Centrum Badań Kosmicznych PAN general public about Martian geology at Wrocław began the process of obtaining the right to confer scientific degrees in the field of Astronomy. R. The FUTURE SPACE project Gabryszewski prepared a portfolio of documen- The EU-funded FUTURE SPACE project is tation that outlines the activities of the Solar focused on astronomy and space exploration. It System Dynamics and Planetology Department aims to be a catalyst for change in understanding in recent years, and collected other materials to and teaching STEM subjects in European support the application. education. Although it is primarily directed at upper secondary school students and teachers, it International conferences and workshops is also open to informal educational organizations Consultations on the modelling and analysis of such as small science centres and NGOs. The orbital background in X-ray detectors, were held Pro-ject aims to inspire students to take an interest 19–20 September 2019, at Wrocław. See the link in science, increase the number of STEM below for further details: candida-tes, and introduce young people to career http://www.cbk.pan.wroc.pl//conferences/mee oppor-tunities and further professional ting_2019/meeting_2019.html development in the space sector and other innovative areas. Ano-ther objective is to build cross-cutting and soft competencies that are important for the labour market and address a lack of achievement in natu-ral science subjects. The two main deliverables are the Space Schools Programme and the Space Programme for science centres and other informal education organiza-tions. The former Programme will include modu-les devoted to global challenges in the 21st centu-ry, and practical solutions resulting from research into, and exploration of, the near- space environ-ment. Both Programmes will Fig. 1. Conference participants.

143 First transnational project meeting of the Others FUTURE SPACE project Our scientists and researchers participated as the The first transnational FUTURE SPACE project lecturers or panelist in: 23rd School Workshops meeting was organized by R. Gabryszewski and A. about Astronomy, Summer school of EAAE (Eu- Grzegorczyk, and held at the Centrum Badań ropean Association for Astronomy Education), Kosmicznych PAN on 12–13 November 2019. It 2nd Forum Vision of Progress (Forum Wizja Roz- brought together 16 representatives from all five woju), SmartUp! West Pomeranian Days of Inno- partners in Poland, Greece and the Netherlands. vation and Entrepreneurship Startupday / Inno- The meeting gave the consortium a better under- vation Forum (SmartUp! Zachodniopomorskich standing of the intellectual outputs, and activities Dni Innowacji i Przedsiębiorczości Startupday / that have to be prepared during the first phase of Forum Innowacji), 3rd Silesian Festival of Science the project. Nineteen presentations were given, (Katowice). eight by CBK PAN researchers (R. Gabryszewski, A few classes were given at schools and for A. Grzegorczyk, G. Wasilewski, M. Michalska and preschoolers (B. Popielawska and A. Wawrzaszek) E. Woźniak). There were an additional three discussion and brainstorming sessions, one led by A. Grzegorczyk.

Fig. 2. 23rd Warsaw Science Festival 2019 in CBK PAN.

144 Fig. 3. Some press releases on CBK PAN activity in 2019.

145