Space Research Centre

SPACE RESEARCH CENTRE

POLISH ACADEMY OF SCIENCES

ANNUAL REPORT

2013

WARSAW

SPACE RESEARCH CENTRE Polish Academy of Sciences Bartycka 18A, 00-716 Warsaw, Poland Phone: (48-22) 49 66 200 Fax: (48-22) 840 31 31 e-mail: [email protected]

Achievements 2013

In 2013 groups from Space Research Centre have been active in many fields of space research, technology and applications. The main achievements are the following: The first Polish scientific satellite LEM, a member of the BRITE constellation, has been launched on a Russian rocket on Nov 21, 2013. The satellite is equipped with a camera that is going to observe small variations of light emitted by bright starts. Obtained data will be used to determine the inner structure of stars. LEM has been built by a SRC engineering team, and the interpretation of scientific data will be carried out by Nicolaus Copernicus Astronomical Centre. So far the satellite works very well and the performance of all subsystems is as it has been expected. The project has proved that the Polish space sector is able to successfully integrate and operate a satellite as well as develop or improve a number of new technologies implemented in BRITE. One of them was a novel type of separation mechanism DRAGON, developed in Mechatronics and Satellite Robotics Laboratory of SRC. After 35 years of journey to the outskirts of the Solar System, the Voyager 1 spacecraft has left the heliosphere, crossing the heliopause, which is the boundary between the plasma originating from the Sun and the local interstellar medium. The identification of this event from the spacecraft data was not obvious and became a subject of controversy among scientific groups. The apparent discrepancy between observations of cosmic rays flux and measurements of magnetic fields has been explained in a few papers published by researchers from the Solar System and Astrophysics Laboratory. The researchers developed a hydromagnetic model of plasma processes at the heliopause and showed that results of their modelling are in agreement with the Voyager observations. This has lend support to the conclusion that Voyager 1 indeed crossed the heliopause. This conclusion has been confirmed by NASA and was based on independent analysis. The numerical simulations performed in SRC also indicated that a non-negligible transport of interstellar plasma exists across the heliopause and into the heliosphere. For years SRC has specialized in building the ionosondes and radio waves analyser in HF frequency domain that measures remote and in situ plasma concentration in the Earth upper atmosphere. Now, this experience has been used in developing a spaceborne version of the instrument that will be able to measure the electron concentration from above. The joint effort of the Plasma Group and the Electronic Construction Laboratory has resulted in an original device, which will be located on board of 4 identical Russian spacecraft. Once space proved, the instrument can be offered as a part of equipment on ESA satellites and guarantee Polish research institutions and industry access to many near Earth missions. More than ten years ago, the Polish X-ray spectrometer RESIK working onboard the Russian CORONAS-F mission provided the best in the world observations of X-ray spectra of solar flares. In 2013 the Heliophysics Group has developed a break-through AbuOpt method of determining chemical composition of solar flare plasma based on those observations. The method employs Bayesian optimization that allows to separate the determination of ion abundances from the retrieval of plasma temperature. Thus, for the first time, it will be possible to get the chemical composition and plasma temperature from the same set of measurements. Up till now, a very strong assumption of plasma isothermal state has been made. Department of Planetary Geodesy of SRC in cooperation with OPGP Lublin has realized a contract solicited by the Head Office of Geodesy and Cartography for a new determination of the vertical reference network for Poland. The fundamental vertical network in Poland is divided into the first class and second class. The final determination refers to the European Vertical Reference Frame EVRF2007-

NH. The results of computations give a physical realization of a new Polish vertical reference frame PL- EVRF2007-NH that is compliant with the frame defined by the European Union. The new reference frame will soon replace the Kronsztadt86 frame used in Poland so far. An important event took place in 2013 in the institute. The main lecture hall was named after the great Polish astronomer and the first chairman of the SRC Scientific Council, Prof. Stefan Piotrowski. The ceremony was attended by the members of Scientific Council, invited guests and the family of Prof. Piotrowski.

(1933-2013)

Prof. dr hab. Andrzej Jurewicz suddenly passed away on the 14th of July 2013. The Space Research Centre has lost one of the most distinguished staff member and dear colleague.

SPACE PROJECTS

ROSSETTA International Rosetta Mission is a Cornerstone Mission in ESA's Science Programme; its destination is short-period comet 67P/Churyumov-Gerasimenko. Rosetta is the first mission designed to orbit and land on a comet. It consists of an orbiter, carrying 11 science instruments, among them VIRTIS and OSIRIS, especially important for researchers from SRC, and a lander, called ‘Philae’, carrying 10 additional instruments with projects important to us CONSERT, and MUPUS, for the most detailed study of a comet. Rosetta was launched on the 2nd of March 2004 by an Ariane-5G rocket from Kourou, French Guiana. The journey to the comet lasts 10 years: first Earth fly-by (November 2005), Mars fly-by (February 2007), second Earth fly-by (November 2007), asteroid 2867-Steins fly-by (September 2008), third Earth fly-by (November 2009), asteroid 21 Lutetia fly-by (July 2010), deep-space hibernation (May 2011 – January 2014), comet approach (January – May 2014), comet mapping/characterisation (August 2014), landing on the nucleus of the comet (November 2014). The orbiter continues to orbit comet 67P/Churyumov-Gerasimenko, observing what happens as the icy nucleus approaches the Sun and then travels away from it. The mission ends in December 2015.

Fig. 1. Rosetta mission.

Rosetta spacecraft has awoken from its 957 days in slumber on the 20th of January 2014, ahead of its mission to rendezvous with the Churyumov–Gerasimenko comet in August. The spacecraft awakening was confirmed by controllers at ESA’s Space Operations Centre (ESOC) in Darmstadt, Germany. In 2013 researchers from the SRC have still been working on interpretation of existing data coming from the OSIRIS camera and VIRTIS instrument on board Rosetta satellite and on modelling the future cometary data (see section Planetology and Solar System Dynamics). (Maria Błęcka, Marek Banaszkiewicz, Jerzy Grygorczuk)

BRITE-PL Bright Target Explorer (BRITE) is a project developed within the Canadian-Austrian-Polish cooperation. Consortium plans to launch a constellation of micro-satellites (20 cm 20 cm 20 cm, 7 kg) to the Low Earth Orbit. This is the first scientific satellite which was developed in Poland between 2010 and 2013. The astronomy project, which cost will exceed 14 million PLN, will be helpful in understanding the stellar oscillations and internal structure of the biggest stars (brighter and hotter than the Sun) in our galaxy. Activities in 2013 concentrated on two major events: the launches of both Polish scientific satellites, Lem and Heweliusz. Lem, which was being stored in a clean room for over one year, underwent remaining tests (open field verification of the telescope and the star tracker). Polish payload for the Heweliusz spacecraft was verified and qualified for flight, the final fitting tests on a 3d prototype of the satellite printed from plastic were conducted, the instruction manual for spacecraft integration was completed. Because of the delay connected with finding an appropriate launch opportunity for Heweliusz, activities commenced in order to prepare a public tender for the launch of the second Polish satellite. Finally the winning launch offer was selected. It was submitted by China Great Wall Industry Corporation. After choosing the launch provider, activities started to implement compatibility between the spacecraft and the launch vehicle. A new separation device, called Dragon was designed, built, tested and flight– qualified at SRC. It attracted the attention of the launch provider, owing to the record development time and its simplicity. SRC received a request for proposal from the launch provider to deliver several such satellite deployers.

Fig. 2. DNEPR Launch Vehicle carried Fig. 3. Last picture taken by the telescope Lem to orbit. of Lem on Earth.

At the same time the integration of Heweliusz took place, which was followed by environmental testing. In parallel the launch campaign of Lem started and the satellite with all its accompanying hardware was sent through Canada to Yasny in Russia, where it was subjected to ground testing before being loaded on the launch vehicle. On November 21st at 7:10 UTC Lem was launched from the Dombarovski Launch Base near the Kazachstan border and subsequently the radio contact was

6 established with the satellite. So far it has travelled more than 1200 orbits. It is now undergoing commissioning tests in orbit. The Lem launch event was organized by Nicolaus Copernicus Astronomical Center, with the participation of VIPs (parliamentary committee on space research, among others) and the media. The launch of Heweliusz was scheduled for December 30th, 2013, but on December 10th due to the launch failure of the preceding flight all launches were aborted till May 2014, when the launch of Heweliusz is expected. Activities promoting the BRITE PL project were taking place: on July 31st, 2013 the Polish Post Office released a stamp devoted to the Heweliusz spacecraft. On September 25th at the Modern Music Festival Warsaw Autumn a piece for a symphony orchestra and a choir was premiered – it was commissioned by the Space Research Centre and the Modern Music Festival and was commemorating the Heweliusz spacecraft creation.

Fig. 4. Last photo of LEM before the launch.

Fig. 5. Stamp devoted to the Heweliusz spacecrft (The Fig. 6. Satellite deployer Dragon made for the Polish Post office issued 300 000 stamps). Heweliusz spacecraft. (Tomasz Zawistowski)

ASIM ASIM - The Atmosphere-Space Interactions Monitor (ASIM) aboard ISS is proposed for the study of high-altitude optical emission from the stratosphere and mesosphere related to thunderstorms. One of the two main ASIM instruments is Miniature-X and Gamma-ray Sensor (MXGS) designed by the University of Bergen and University of Valencia in cooperation with SRC PAS in Warsaw. SRC is responsible for the design and manufacturing the Power Supply Unit and it autonomous (FPGA based) Housekeeping System.

In 2013 the design and manufacturing of EM model of DCDC block of MXGS/ASIM/ISS instrument has been finished. The activities have been performed in SRC PAS and Creotech – the first Polish company involved in manufacturing of space electronics according to EPSS rules.

Fig. 7. Integration of ASIM EM, Power Supply Unit (DCDC Block) from SRC top right.

(Paweł Grudziński)

TARANIS TARANIS is a low-altitude CNES micro-satellite mission that will provide a set of unprecedented and complementary measurements on the physics of TLEs (Transient Luminous Events) and TGFs (Terrestrial Gamma ray Flashes). Specific examples include:  The first combined images of TLEs and TGFs (through fast micro-cameras and photometers, nadir-viewing and X- and Gamma-ray measurements) and the associated measurements of relativistic electrons and wave fields;  The first high resolution measurement of energetic electrons in energy, pitch angle and time allowing both to detect runaway

electrons and LEPs and to track natural and man-made Fig. 8. TLE effects. controlled variability of the radiation belts;  The first on-board wave field measurements in a frequency range running from DC to 30 MHz allowing to record radio signatures of optical and particle transient phenomena and to detect the presence of quasi-electrostatic thundercloud fields. SRC participates in the scientific program of the mission and designs the MEXIC Power Unit (MPU) - the supply block dedicated for the whole TARANIS Payload. In 2013 the EM Models of MPE block of MEXIC/Taranis instrument have been tested and integrated with the rest of Taranis MEXIC blocks. The documentation for FM models has been finished. The project was formally closed in NCN.

Fig. 9. Left - block scheme of one part of Taranis MEXIC MPU, right -MPU EM1 block integrated as bottom part of MEXIC unit. (Roman Wawrzaszek)

STIX In October 2011 Solar Orbiter, Fig. 10 was adopted by SPC/ESA for implementation as M1 Mission, with a targeted launch date of 2017. The Solar Orbiter payload, devised to address the science goals of the mission, accommodates a set of in-situ and a set of remote sensing instruments, with a total payload mass of 180 kg. The in-situ instruments consist of detectors for observing particles and events in the immediate vicinity of the spacecraft: the charged particles and magnetic field of the solar wind, radio andmagnetic waves in the solar wind, and energetically charged particles flung out by the Sun. The remote sensing instruments will observe the Sun's surface and atmosphere. The gas of the atmosphere is best seen by its strong emissions of short-wavelength ultraviolet rays. Tuned to these will be a full-Sun and high-resolution imager and a high-resolution spectrometer. The outer atmosphere will be revealed by ultraviolet and visible-light coronagraphs that blot out the bright disc of the Sun. To examine the surface by visible light, and measure local magnetic fields, Solar Orbiter will carry a high-resolution telescope and magnetograph.

X-ray Spectrometer/Telescope Instrument (STIX), one of 6 remote sensing instruments on-board SolO, provides imaging spectroscopy of solar thermal and non-thermal X-ray emission. STIX will provide quantitative information on the timing, location, intensity, and spectra of accelerated electrons as well as of high temperature thermal plasmas, mostly associated with flares and/or microflares. PI of the Instrument: Dr. Sam Krucker, FHNW, Windisch, Switzerland. Collaborating countries (HW and SW): CH, PL, D,

CZ, F. As the result of common agreement within STIX Consortium, the Polish participation in STIX consists of the Fig. 10. Solar Orbiter Satellite (ESA). following work-packages: 1. Participation in STIX scientific program and in Data Reduction and Archiving (J. Sylwester) 2. Thermal Modeling of the whole Instrument and its subsystems, (K. Seweryn) 3. Instrument Data Processing Unit (IDPU) including IDPU hardware, low level flight software and mechanical frame for both: IDPU and PSU (Power Supply Unit to be delivered by Czech Republic) (K. Skup) 4. Instrument EGSE (M. Kowaliński)

In 2013 the following activities have been performed:  IDPU Box STM has been manufactured and tested in SRC and delivered to STIX Consortium, STIX Instrument (Imager plus DEM Box and separately X-ray Window) has been tested in TV Chamber in SRC,  The Full and Reduced Numerical Models (ESATAN) of whole STIX Instrument have been developed and delivered to ESA,  IDPU EM has been manufactured in 5 copies (one for software development at EvolvedSys, one for PSU tests at CSRC, one for Detector tests at AoT, two for SRC engineering activities. The electrical design, PCB layout and FPGA code have been validated based on this model. The mechanical and thermal designs of IDPU have been validated based on IDPU STM,  The first models of: STIX EGSE (Spacecraft Simulator delivered by ESA, software written in SRC, SpaceWire Simulator and Thermoelectric Cooler developed in SRC) and STIX Detector Simulator have been manufactured and integrated.

(Piotr Orleański, Konrad Skup, Karol Seweryn, Mirosław Kowaliński)

Fig. 11. SRC persons during the DEM and Imager (left) and X-ray window thermal tests (right).

Fig. 12. STIX EGSE, first (technological) model of SpaceWire

Simulator and Thermoelectrical Cooler.

CaSSIS

The 2016 ExoMars Trace Gas Orbiter (TGO) is the first in a series of Mars missions to be undertaken jointly by the two space agencies, ESA and Roscosmos. A key goal of this mission is to gain a better understanding of methane and other atmospheric gases that are present in small concentrations (less than 1% of Fig. 13. ExoMars Orbiter in cruise configuration. Credit: ESA. the atmosphere) but nevertheless could be

Fig. 14. One of fifth models of STIX IDPU EM Fig. 15. STIX IDPU Box Structure and Thermal Model. manufactured in SRC. evidence for possible biological or geological activity. One of the instruments of TGO is CaSSIS–Colour and Stereo Surface Imaging System. A high resolution camera (5 metres per pixel) capable of obtaining colour and stereo images over a wide swath. CaSSIS will provide the geological and dynamical context for the sources or sinks of trace gases detected by two other instruments: NOMAD and ACS. CaSSIS Principal Investigator: Nicolas Thomas, University of Bern, Switzerland, participating countries: Switzerland, Italy, Poland.

Late 2013 SRC PAS was invited to CaSSIS Consortium as responsible for Power Converter Module for Instrument. Due to the extremely tight schedule (EM and FM models had to be delivered to University of Bern in 2014) the activities in SRC were concentrated in parallel: on finalization of the requirements and specifications, and on design and manufacturing of the simplified engineering model of PCM.

Fig. 16. CASSIS Instrument, © University of Bern (left), PCM first prototype (right).

(Piotr Orleański, Witold Nowosielski)

ELSA ELSA is a project founded in a frame of European 7FP program. Magnetically levitated reaction sphere ELSA is a novel concept of attitude control system actuator which consists of magnetic rotor and special set of coils placed around the rotor to generate forces and torques which keep the rotor in a centre of the stator and rotate it in any direction if required. In year 2013 project ELSA reached an important level of development which allows to enter a next phase which is manufacturing a final design. ELSA is a complex magnetic system. Up till now, the main theoretical investigations related to the final design like: modelling, control strategy development and system design optimization have been finished. The next phase of the project planned for year 2014 will be hardware manufacturing, integration and testing. CBK collaborates in this project with MAXON, CSEM, RedShift, SABCA and SENER.

Fig. 17. Final design of ELSA rotor which consists of eight permanent neodymium magnets mounted on special mechanical structure. (Roman Wawrzaszek) The RELEC

The RELEC (Relativistic ELECtrons) satellite will be launched into a sun synchronous orbit to the height of about 750 km in 2014. The aim of the RELEC mission is to study precipitation of magnetosphere relativistic electrons and their impact on the Earth atmosphere and ionosphere including the observations of fast transient phenomena in the upper atmosphere. It will provide combined observations of UV, X and gamma radiation and charge particle fluxes, as well as electromagnetic fields.

Radio Frequency Analyser (RFA) has been developed by SRC PAS. The Radio Frequency Analyzer (RFA), with three electric field components of antenna system, is devoted to diagnose temporal and spatial electric field fluctuation in the frequency range from 20 kHz to 15.0 MHz. In order to observe the effects related to the thunderstorm activity, the instrument will have possibility of registering a very fast (25 ns) wave form. The instrument can also be used for monitoring the electromagnetic ecosystem for the space weather purpose. The flight model FM was delivered on a spacecraft complex in summer 2013.

Fig.18. Laboratory tests of the electromagnetic signal reception. Fig. 19. Ultra-light electric antenna before deploy.

(Hanna Rothkaehl, Marek Morawski, Jerzy Grygorczuk, Marta Tokarz, Marcin Krzewski) 12

OBSTANOVKA The aim of OBSTANOVKA experiment, on board ISS station, is to monitor and diagnose the electromagnetic radiation and property of plasma around station, to enable the development theory of near Earth plasma interaction and for application purposes in space technology. To achieve these goals the Plasma-Wave Complex PWC was designed and constructed. Radio Frequency Analyser RFA, part of PWC complex, has been developed jointly by SRC PAS in Warsaw and by IRF in Uppsala. New design radio receiver for frequency band 0.1-15 MHz, with three electric and magnetic field components of antenna system on board ISS was designed to monitor and investigate the ionospheric plasma property and artificial noises generated around ISS. The instrument can also be used for monitoring the electromagnetic ecosystem for space weather purpose. New digital technology of this instrument creates an excellent possibility for monitoring the electromagnetic emissions in space and time domain. The investigations on the ISS will be focusing on the following main topics:

- Understanding the consequence of human activity in the nearest space environment. - Description of global changes in the ionosphere-magnetosphere system. - Selection and description of artificial and natural noises detected in the ionosphere. - Analyse interaction between the ISS infrastructure and surrounding plasma. - Diagnose changes of detected signals on the board of ISS during discharging process related to the moor of Space Shuttle.

The complex of OBSTANOVKA instrument was transported on ISS on the 12th February 2013. The successful installation and deployment of the antenna system was conducted by the cosmonauts of 35 Expedition on the Russian Zvezda service module on the 19th February 2013. First scientifically data has been registered on the 3th September 2013.

Fig. 20. The astronauts install the antennas of polish radio frequency analyser RFA.

(Hanna Rothkaehl, Marek Morawski, Jerzy Grygorczuk)

LEART Electromagnetic emissions observed in the nearest Earth environment are superposition of natural emissions and various types of man-made noises. Also as a consequence of thunderstorm activity and an earthquake or volcanic eruption, on the board of low orbiting satellites the electromagnetic

13 emissions are detected. At the current stage of space physics investigations, we can describe many different magnetospheric and ionospheric activities driven by changes in the Sun-Earth system. Moreover, we still have problems with forecasting geospace conditions, particularly during disturbed geomagnetic conditions. In order to achieve this goal the four spacecraft JONOSOND missions led by the Russian Space Agency was proposed. The four identical spacecrafts will be located at the polar circular orbit at the altitude 600 km and 800 km. In the frame of contract with Russian side, the four ionosonds LAERT, dedicated to top-side in situ active diagnostics were designed in SRC PAS. The QM model was designed, constructed and delivered to spacecraft factory. Each instrument consists of two parts, the receiver and transmitter, and preamplifier for the antenna system.

Fig. 21. The satellite configuration of IONOSONDE satellites.

(Hanna Rothkaehl, Andrzej Rokicki, Marek Morawski, Marcin Krzewski)

IONOSAT-MICRO project The primary objective of the proposed IONOSAT-MICRO project, led by the Ukrainian Space Agency and IKI is to monitor the Earth's space environment and obtain a complete picture of the electromagnetic plasma environment and description of near Earth turbulent structures region. This project is a first stage of IONOSAT mission devoted to a multi-point global monitoring of dynamic processes in the ionosphere. IONOSAT-MICRO is the forerunner project scheduled for launch on board of a Ukrainian microsatellite MICROSAT with the X is polar LEO around 500 km. The scientists and engineers from Space Plasma Group have been invited to build the HF wave analyser. The new technologies of RFA radio analyser will give the possibility for 3D diagnostics of electric field component (spectra and wave forms) with extremely high time resolution. Moreover, the registration from the RFA radio analayser located on board of low orbiting satellite RELEC will give the unique opportunity for multipoint diagnostics. Based on the data gathered by different sensors located on board of IONOSAT-MICRO it will be possible to investigate the following topics: - Space-temporal structure of inhomogeneities in neutral atmosphere and ionosphere; - Global structure and dynamics of electric currents, electric and magnetic fields; - Wave structures and turbulences at different scales; - Synchronous experiments with ground support facilities.

Fig. 22. Scientific instruments on board of IONOSAT-MICRO satellite.

(Hanna Rothkaehl, Marek Morawski, Marta Tokarz, Marcin Krzewski)

LOFAR LOFAR is the Low-Frequency Array, exploring the poorly studied range between 30-240 MHz frequencies. It constitutes of a European array of thousands of antennas - a challenge for data transfer and processing techniques. The project is based on an interferometry array of radio telescopes using about 25,000 small antennas concentrated in at least 48 larger stations. 40 of these stations are distributed across the Netherlands, five in Germany, and one each in Great Britain, France and Sweden. The data processing is performed by a Blue Gene/P supercomputer situated in the Netherlands at the University of Groningen.

LOFAR will study objects in early Universe (like the high-redshift neutral hydrogen) and cosmic plasma in conditions unreachable in earth-based laboratories: densities either very high (pulsars) or extremely low, temperatures ranging from single Kelvins to millions of degrees and a wide range of magnetic field strengths. LOFAR will be challenges for Sun-Earth system monitoring and modeling, Space Weather program and for space plasma technologies. The LOFAR facilities in Poland will be distributed among three sites: Łazy (East of Kraków), Borówiec near Poznań and Bałdy near Olsztyn. They all will be connected via PIONIER dedicated links to Poznań. Each site will host one LOFAR station (96 high-band+96 low-band antennas). For most of the time they will work as a part of the European network, however, when less charged, they can operate as a national network. Stations will be maintained by institutes owning particular sites: Jagiellonian University (Łazy), Space Research Center of Polish Academy of Sciences (Borówiec) and University of Warmia and Mazury (Bałdy). The data from all our stations will be sent online to Poznań via fast (GB/s) PIONIER network and then to the correlator in the Netherlands. This will be a good test for the PIONIER fast digital network. The proposed LOFAR installation in Poland will give us a unique possibility to take part in leading European and world scientific research in astronomy and space physics. Poland will join an exclusive group of several European countries in one of the most advanced projects in astronomy and space science in the world.

Fig. 23. The LOAFR antenna system in headquarter Exloo Nederland.

Fig. 24. Low and high frequency antennas. (Hanna Rothkaehl)

RESONANCE The primary objective of RESONANCE project is to diagnose and monitor the Earth's space environment and obtain a complete picture of transport of energy between inner magnetosphere and ionosphere system than those available hitherto. Particularly attention is paid on long-standing and still unsolved issue like inter relationship between noise and discrete emissions in cyclotron maser, the role of different wave mode in acceleration and precipitation of energetic charged particles, and energy transfer from hot to cold plasma component. The proposed RESONANCE mission consists of 4 identical spacecrafts, located within the same magnetic flux tube up to 3 hours. Such an orbit is parti- 16 cularly suitable for studying the processes for which field-aligned wave propagation and particle motion are significant. The ”Active part" of RESONANCE project also has the unique and novel character of investigation. Using the ground base heat facility, as HARP installation, it will be possible to diagnose the changes of near Earth environment generated by artificial electromagnetic pumping.

Fig. 25. Trajectories’ scheme.

The HF radio analyser, designed and built by the polish team, is an electronic module devoted to measure electrical and magnetic components of radio frequency emissions in the frequency range from 10 kHz up to 1.0 MHz and phase difference of measurement of two monochromatic signals on frequency 5.0 MHz and 15.0 MHz transmitted from “RIC” instrument. The instrument is composed of main units that includes two Digital Vector Receivers and Data Processing Unit with Control Module. Signals to be analysed by HFA came from the following sources: • three dimensional low frequency electric field antenna set (AMEF-WB), • three dimensional magnetic field antenna set, • narrow band 5MHz and 15 MHz antenna sets. The EM model was designed in 2013.

(Hanna Rothkaehl, Roman Schreiber, Marek Morawski, Marcin Krzewski)

BepiColombo 1. Bepi Colombo – ESA mission to Mercury BepiColombo is Europe’s first mission to Mercury. It consists of two orbiters, one for planetary investigation and one for magnetospheric studies. They will reach Mercury in 2020 after a six-year journey towards the inner Solar System, to make the most extensive and detailed study of the planet ever performed. The 'Mercury Planetary Orbiter' (MPO), under ESA’s responsibility, will study the surface and the internal composition of the planet at different wavelengths and with different techniques. The Mercury Magnetospheric Orbiter (MMO), under the responsibility of the Japan Aerospace Exploration Agency (ISAS/JAXA), will study the magnetosphere, that is the region of space around the planet that is dominated by its magnetic field.

Space Research Centre is involved in the MPO-MERTIS and ISA experiments. The experiment MERTIS (MErcury Radiometer and Thermal Infrared Spectrometer) is led by the German Space Institute from Berlin. The MERTIS is dedicated to global mineralogical mapping and measurements of surface temperatures and thermal inertia in the spectral range of 7-14 µm. SRC is responsible for the part of the spectrometer – Pointing Unit (acronym MPOI).The MPOI as one of the spectrometer 17 modules is situated in front of MERTIS to orient the optical entrance of the instrument to 4 different targets sequentially. These targets are the Mercury surface and deep space as well as two black body of 300 and 700 K. Besides strong needs for the miniaturization of environmental conditions they are key for design details: operational temperature range –30°C to +70°C, random vibration loads around 40g rms and high level of radiation. The required performance is characterized with a pointing accuracy of 0.8 arcmin for the main targets and a pointing mirror flatness of more than 0.4 µm for sufficient wave front quality. The following tasks were realized in 2013. The main goal was (goal) conducting tests of Spare Flight Model (SFM). All tests of SFM MPOI were carried out in reported period. We carried out additional functional tests with new EGSE equipped in the new s/w according to requirements delivered by DLR and we prepared End Item Data Package of SFM. The SFM is waiting for the end of basic tests of MERTIS. The delivery date of SFM was planned for the beginning of March 2014.

Fig. 26. SFM MPOI. (Mirosław Rataj) JUICE RPWI JUICE - JUpiter ICy moons Explorer - is the first large-class mission in ESA's Cosmic Vision 2015-2025 programme. JUICE will perform detailed investigations of Jupiter and its system in all their inter-relations and complexity with particular emphasis on Ganymede as a planetary body and potential habitat. The main goals of JUICE project are: - Conducting a comparative study of Ganymede, Callisto and Europa, with an emphasis on the characterization of Ganymede as a planetary object and possible habitat. - Providing a complete spatio-temporal characterisation of the giant, rotating magnetosphere, and of the meteorology, chemistry and structure of Jupiter's gaseous atmosphere. - Studying coupling processes inside the Jupiter system, with an emphasis on the two key coupling processes within that system: the tidal effects that couple Jupiter with its satellites Fig. 27. Jupiter and the moons. and the electrodynamic interactions that couple Jupiter and its satellites with their atmospheres, sub-surface oceans, magnetospheres and magnetodisc.

The Radio&Plasma Waves Investigation is one of the scientific payload instruments. RPWI consists of a highly integrated instrument package that will carry out measurements that allow for 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. 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). Thus, the RPWI sensors provide complete measurements of the electric and magnetic field vectors. The SRC-PAS has a major role in the JUICE/RPWI consortium, both with regard to instrument hardware and software as well as in the science investigation. The SRC-PAS responsibilities in the instrument implementation are: - designing the mechanics of the four booms and sensors for the Langmuir Probe & Plasma Wave Instrument (LP-PWI) part of RPWI, - designing the main RPWI Digital Processing Unit (DPU), - designing the mechanics of the Radio Wave Instrument (RWI) antenna part of RPWI.

(Hanna Rothkaehl, Marcin Dobrowolski, Marek Morawski, Jerzy Grgorczuk)

DATA ACQUISITION

GNSS Observatory in Warsaw The observatory is involved in the following projects:  new global navigation system GALILEO,  navigation with EGNOS system,  monitoring of the quality EGNOS corrections in cooperation with ESA in IMAGE/PERFECT,  positioning measurements and defining the national reference frame with GPS technology

GALILEO In 2009 new GESS+ (Galileo Experimental Sensor Station) was installed in SRC Warsaw. After few months of tests of observed data quality, station was included to the global monitoring network of the GIOVE satellites.

Fig. 1. New GALILEO GESS+ station (GWAR) in SRC, Warsaw.

Every week ESA-ESTEC generates a report with information about status of stations and observation data quality for GPS and GIOVE signal. (Leszek Jaworski, Anna Świątek) EGNOS

In Warsaw is located one of the RIMS stations (Ranging and Integrity Monitoring Station) of the EGNOS System designed to broadcast embedded correction signals in Europe, which will provide improved performance with GPS (Fig. 2).

Fig. 2. The EGNOS Ground Segment (RIMS, MCC, NLES, PACF).

Beside RIMS station SRC cooperates with Polish and European institutions in research of the EGNOS System. Most interesting are:  participation in ESA IMAGE/PERFECT Project,  dynamic tests of the system using Mobile GNSS Laboratory.

One of the main objectives of the EEGS2 project (EGNOS Extension to Eastern Europe: Applications) funded by the 7th Framework Programme of the European Commission and reviewed by the European GNSS Agency (GSA) is to demonstrate through flight trials the benefits of SBAS EGNOS (SBAS – Satellite Based Augumentation System, EGNOS – European GNSS Navigation Overlay System) in areas of Eastern Europe where EGNOS is not yet available and prepare the civil aviation authorities and navigation service providers of those areas for the future usage of EGNOS. The project has been coordinated by the Spanish company GMV. The countries which do not have EGNOS coverage yet will familiarize with the EGNOS procedures through the flight trials and also pilots will be able to really understand and feel the EGNOS performances and advantages. These flight trials will contribute to the adoption of SBAS systems in countries where the EGNOS signal is not yet available. During the second quarter of 2013 a flight test campaign covering Moldova, Poland, Romania and Ukraine was carried out. In the scope of the EEGS2 project the magicLPV (LPV – Landing Procedure with Vertical guidance) system has been developed by GMV. This system allows flying LPV procedures using the signal simulated by the special software magicSBAS; therefore LPV procedures can be flown in areas where SBAS is not available (considering there is a network of ground stations to deliver GNSS data to be used as inputs in magicSBAS). As a general conclusion, magicLPV is currently capable of providing LPV guidance with magicSBAS signal and very good navigation performances when the altitude is lower than 1000 ft. With EGNOS signal the system works at every altitude. Therefore magicLPV together with magicSBAS is a very powerful platform to demonstrate the performances of an SBAS system in places where SBAS is still not available or is not providing the expected performances. This has been demonstrated by the test flights done in Poland at the Dęblin airport of the Polish air Force Academy. In addition the business study for EGNOS application in the Eastern Europe has been prepared showing the benefits as well as costs of this development. Finally the Roadmap of the introduction of EGNOS to the airports in Poland has been prepared.

(Leszek Jaworski, Anna Świątek, Janusz B. Zieliński) 21

GPS Permanent Station

Starting from February of the 2003 in Warsaw permanent GPS station (CBKA) integrated with pilot project Active Geodetic Network (ASG-PL) for Poland has been in operation. Starting from December of the 2007 station CBKA was included in ASG–EUPOS project. (Leszek Jaworski, Anna Świątek)

The Geodynamic Laboratory in Książ

RESEARCH ON THE ŚWIEBODZICE DEPRESSION TECTONIC ACTIVITY IN GEODYNAMIC LABORATORY (LG) OF SRC IN THE KSIĄŻ SUBURB OF WAŁBRZYCH

The Książ castle is located in the central part of the Sudetes in the Wałbrzych Foothills area. From the geological standpoint the Książ orogen is situated almost in the central part of the geological structural unit of Swiebodzice Depression. Sediments within Świebodzice Depression are from the epochs of Upper Devonian and Lower Carboniferous.

Determination of faults parameters in the LG corridors The location of LG in underground tunnels provides unique opportunity to observe and study tectonic activity of the orogen from the inside. The knowledge of tectonic faults locations and routes in the surroundings of castle buildings as well as inside the orogen is necessary for a comprehensive description of the geological and tectonic situation. The inspection of LG corridors performed last year revealed the presence of numerous surfaces of discontinuity. Some of them run directly under the measuring gauges, which allows for the registration of tectonic activity on these faults in real time in form of tiltings of foundation and vertical motions.

In order to determine the directions of routes and dips angles of all undergrounds lines of dislocation visible in the LG, geodetic measurements were executed. In the first phase of the works the horizontal measurement network points were stabilized in the corridors. Recognition of distribution of dislocation surfaces of faults allowed to divide the set of all faults into classes according to their routes azimuths (W-E and SW-NE directions). The faults of single class are in good approximation parallel to each other. It was proved that in the Książ orogen there are two dominant systems of faults belonging to two separated classes. The faults of the first class are parallel to the main southern fault (Fig. 3) whereas the azimuths of routes of the second class faults (class 2) differ by ~30º from the west (counterclockwise) in relation to the azimuth of the main southern fault.

Fig. 3. Plan of underground of Laboratory with The first two classes of the faults occur in tectonic marked three classes of faults and main deformations of orogen in different manner. southern fault.

Probably the faults of class one, which are parallel to the main southern fault, are active in situation when northern wing of the main southern fault is in slower motion than its southern wing. In the inverse situation, when the northern wing is faster than the southern wing, class two of the faults is active. Taking into account the geological indicators of delay of the northern wing in relation to the southern wing, we suggest to call the first case as the compensation phase of the tectonic phenomenon, and the second case as the shifted phase. This thesis is motivated by changes of faults activity observed after 2009 by the water-tube tiltmeters.

(Marek Kaczorowski)

Damages in the Książ castle architectural objects produced by recent tectonic motions

Documentation of the routes of the dislocation surfaces and registrations of indicators of recent tectonic activity determined by the LG instruments gave basis for further research on the influence of tectonic deformations on the ground surface and the architectural objects. The influence

of recent tectonic activity which is Fig. 4. The Książ castle architecture on the Pelcznica river peninsula and the main tectonic faults recognized on primary faults oriented SW- NE is well visible in the morphology of terrain by deformations of Pelcznica Valley meander (Fig.4) and the geological structure of the research area. The activity of primary faults will be firstly considered for the assessment of the influence of tectonic effects on the Książ architectural objects. The examination of Książ castle architecture objects was executed in order to recognize macroscopic damages which could be made by strike-slip movements on the faults passing under these objects. In the frame of the examination works some suspicious cracks in construction of the wall of St. George Tower were noticed, in the wall of Chestnut Terrace as well as sequences of cracks in the window stone elements and in the window sills above the Chestnut Terrace and also in the western wall of terraces (fragments repeatedly repaired) (Fig. 5). The cracks are also visible from the southern side of the castle complex in the stone wall and stairs leading to the terraces (con- creted cracks that quickly open again) (Fig. 5).

The routes of dislocations zones marked on the map of primary faults and the determined lines of Fig. 5. Damages in the elements of st. george tower of Książ castle located on the recently damages (Fig. 4) show the existence of distinct active tectonic fault. relationship between them. (Marek Kaczorowski) 23

The Astrogeodynamical Observatory in Borowiec

Time and Frequency Laboratory In 2013 the work at Time and Frequency Laboratory concentrated on:  Realization of the UTC(AOS) kept with-in the range of ±5 ns from UTC.  Realization of Polish Atomic Time Scale TA(PL)with stability of ~2×10-15  International comparisons of atomic time scales are based on two methods: – Two Way Satellite Time and Frequency Transfer (TWSTFT) method, which assures uncertainty of the measurements in the range of 200 ps. – Phase GPS@GLONASS measurements with enable time transfer with uncertainty of 50 ps. This new method is based on the use of Precise Positioning computations (PPP) carried with Bernese and NRC software.

The data supplied by constructed at the Observatory the TTS-4 receiver observing GPS, GLONASS and Galileo satellites. The receiver is equipped with 116 channels and carries on observations at GPS L1, GPS L2/L2C, GPS L5, GalileoE1/E5A, GLONASS L1/L2.

The Laboratory continues:  Realization and development of Polish Atomic Time Scale – now about 17 atomic clocks from Poland and laboratories from Lithuania.  Participation in the realization of UTC and TAI in cooperation with the BIPM in Sevres. In 2013 the measurements with very precise method of time transfer were continued using telecom network with time and frequency transfer over optical fiber with stabilization of propagation delay at the level up to 40 ps. The permanent optical fiber connection of over 420 km between Central Office of Measures (GUM) in Warsaw and Astrogeodynamical Observatory of Space Research Centre (AOS) in Borowiec near Poznan was used for time comparisons. Both laboratories maintain the local UTC(k) realizations: UTC(PL) and UTC(AOS) respectively. The optical time transfer link has been calibrated with accuracy of about 0.6 ns (including systematic effects) and does not require any other time transfer methods as a reference. The method and the glass fibre equipment were developed by the Institute of Electronics of the AGH University of Science and Technology. In future it is expected to be the most precise method of time comparisons of the future most precise atomic optical clocks. Precision of comparisons of atomic clocks at AOS (H-maser) and GUM (cCs clock) equals to ~10 ps, which is at the moment the best result of long-distance time transfer in the world.

In 2013 two calibrations campaign were performed:  calibration of AOS TWSTFT system – increasing the accuracy of the measurements to about 100 ps,  calibration of BIPM GPS equipment using optical fibre link AOS – GUM.

AOS also participates in the realization of two grants:  OPTIME – time and frequency dissemination system based on fiber optical network. Project PBS1/A3/13/2012) is co-founded by The National Centre for Research and Development – Poland. The project is realized by the consortium of AGH University of Science and Technology (AGH), Kraków, Orange Poland (TPSA) and Poznań Supercomputing and Networking Center (PSNC), Poznań, and Space Research Centre.

 GLOVE - Galileo Integrated Optimization with VANET Enhancements, International project realized within the frames of the 7th European Framework Programme Communication project based on Vehicular Ad-hoc Networks (VANETs) - emerging type of car networks that enable a broad range of applications such as public safety, traffic management, traveller information support and entertainment. The project is led by Instituto Superiore Mario Boella in Torino, Italy. In the realization participates Centro Ricerche Fiat, Italy, Deutsches Zentrum für Luftund Raumfahrt, Germany, Galatasaray University, Turkey and Infotech from Turkey. (Jerzy Nawrocki)

BOR 1 station Long-term provision of GPS data from the GNSS station BOR1 for national and worldwide scientific and surveying project was realized. The permanent GPS station located at Borowiec and known as BOR1 has been integrated with IGS and EUREF networks since 1996. Actually, results from BOR1 as one from 100 worldwide reference stations, participated in the realization of Reference Frame IG05. The data streams from BOR1 station are available through IGS-IP and EUREF-IP projects. High quality data files makes a valuable contribution to the global geodesy and related research in the frame of IGS (International GPS Service). The data delivered by BOR1 are used for precise orbit calculation by many international institution as CODE (Central Orbit Determination Europe) Bern Switzerland, GFZ-IGS Processing Centre Germany, JPL-IGS/FLYNN Processing Centre Pasadena USA, Massachusetts Institute of Technology USA, Scripts Institution of Oceanography USA, and National Geodetic Survey Canada. The BOR1 station participates in the multifunctional precise satellite positioning system "ASG- EUPOS" established by the Head Office of Geodesy and Cartography as one of the reference stations. The data and behavior of the station are shown on our web page: http://ofelia.cbk.poznan.pl. (Marek Lehmann)

Satellite Laser Ranging Station In 2013 the Borowiec Observatory obtained government funds for purchase of a new laser for Borowiec SLR station. The laser parameters which also enabled the possibility of the space debris observations were prepared. The new laser was installed in Borowiec Observatory at the end of December 2013 (Fig. 6).

Fig. 6. New laser at the Borowiec Observatory. (Stanisław Schillak) 25

Obserwatorium Borowiec On August 12, 2013 the research project NN526170040 “Time scale comparison with the use of GNSS phase signals with sub-nanosecond precision” has been completed. The last results obtained in a frame of this project were presented during two international conferences European Geosciences Union General Assembly (EGU), which was held on April 7-12, 2013 and European Time and Frequency Forum (EFTF), which was in Prague on July 21-25, 2013. The presented results concern the time transfer determination between different time and frequency laboratories by means of NRCan PPP software based on phase and pseudoranges measurements on the use of various computational variants. The details of all analyses and results were published in Proceedings of EFTF and submitted to the GPS Solutions JRC journal. As a contractor and head of SRC PAS group I was engaged in educational project EDUSCIENCE. The full title of the project is “Developing students‘ competence in the range of mathematics, natural science and IT with the usage of innovative methods and technology – Eduscience”. This project is managed by Institute of Geophysics of the Polish Academy of Sciences in period 2011-2014. EDUSCIENCE project is directed to the hundreds of schoolchildren and teachers from 250 schools in Poland chosen at random on all levels of education. The goals of the project can be characterized as follow:  Creating bigger interest in mathematical-natural science/informatics-technical science/ foreign languages thanks to diametrical change of previous teaching formulas.  The rise of skills connected with identifying and defining research problems and using research methods in the range of science owing to pupils taking part in the real research process.  The development of using information-computer technology skills in the process of learning owing to using the e-learning/blended learning method. In 2013 Borowiec Observatory was visited by 13 groups of schoolchildren from all over Poland under the EDUSCIENCE project. (Paweł Lejba)

INTERPRETATION AND MODELING SPACE PHYSICS Solar physics (Wrocław Solar Physics Division)

RESIK RESIK was a unique Bragg crystal spectrometer operating in one of the two previous missions of the Russian CORONAS program. RESIK was launched on CORONAS-F satellite on the 31st July 2001. The instrument took measurements close to the maximum of 23rd solar activity. The instrument recorded ~1. 8 mln. high quality spectra in the spectral range 3.3-6.1 Å. In the spectra, several prominent X-ray emission lines are seen formed in active regions and flares. In 2013, further analyses of these spectra have been performed. The main results obtained are the following: The active binary stars σ Gem and HR1099 X-ray spectra obtained from the Chandra High Energy Transmission Grating Spectrometer have been compared with the solar flare spectra obtained with the RESIK instrument at similar resolution in an overlapping bandpass.

Fig. 1. We show the spectra and models in the short wavelength region where HETG and RESIK spectra overlap. Flux- corrected spectra are in black, and the red is the model convolved by the instrumental resolution. Below each, in blue, are residuals. The top panel shows σ Gem; the middle is HR 1099; the bottom is the rise phase of the solar flare on 2002 December 26 (maximum at 06:30 UT). Huenemorder, Phillips, Sylwester & Sylwester, The Astrophysical Journal, 768:135 (15pp), 2013 May 10).

The primary goal of this work was to compare low and high FIP elemental abundances in the Sun and stars. We have determined new elemental abundances. For the lowest FIP species—particularly K and Na, the abundances in σ Gem are similar to that in the solar corona, other low-FIP elements (Na, Al, Ca, Mg, Fe, and Si) are strongly depleted, only becoming near or above solar for the high FIP elements N, Ar, and Ne. Even the stellar S abundance (considered high-FIP) has a very low relative abundance. In another study RESIK fluxes of the Si XIV Ly-β line (5.217 Å) and the Si XIII 1s2 – 1s3p line (5.688 Å) for 21 flares have been analyzed to obtain the silicon abundance relative to hydrogen. The

27 emitting plasma for each spectrum was assumed to be characterized by a single temperature and emission measure given by the ratio of emission in the two channels of GOES.

Fig. 2. Upper panel: Spectra for RESIK Channels 3 and 4 for all 1822 spectra analyzed in this work, stacked in order of TGOES increasing upwards, with the scale shown on the left. Lower panel: Five RESIK Channels 3 and 4 spectra averaged over 2-MK intervals, with the average temperature TGOES shown in each case. The Si XIV Ly-β line at 5.217 Å has increasing intensity relative to the Si XIII 1s2 −1s3p line at 5.688 Å for increasing TGOES, while the Si XIII line predominates in Channel 4 spectra at lower temperatures.

The silicon abundance was determined to be A(Si) = 7.93 ± .21 (Si XIV) and 7.89 ± .13 (Si XIII) on a logarithmic scale with H = 12. These values, which vary by only very small amounts from flare to flare and sometimes within flares, are 2.6 ± 1.3 and 2.4 ± 0.7 times the photospheric abundance, and are about a factor of three times higher than RESIK measurements during a period of very low activity. There is a suggestion that the Si/S abundance ratio increases from active regions to flares. (B. Sylwester, K. J. H. Phillips, J. Sylwester, A. Kępa, Solar Phys. 283:453–461).

A new analysis method AbuOpt for determination of time/temperature dependent composition and differential emission measures the structure of flaring plasmas that have been developed and used for the analysis of selected flare (SOL2002-11-14T22:26). The analysis starts by finding an abundance set that is consistent with the observed spectra, then solves? for the differential emission measure shape using a maximum-likelihood routine (the Withbroe–Sylwester method). The abundance optimization leads to revised abundances of silicon and sulfur in the analyzed flare plasmas: A(S) = 6.94 0.06 and A(Si) = 7.56 0.08 (on a logarithmic scale A(H) = 12).

Fig 3. Left: Contour plot of the differential emission measure during the SOL2002-11-14T22:26 flare, darker colors indicate greater emission measure. The horizontal scale is the logarithm of temperature, and the time increases upwards, measured from 22:14:41 UT. Horizontal dotted lines define the time intervals a, g, i, l, and q and the smooth curve running from top to bottom is the temperature derived from the ratio of the two GOES channels on an isothermal assumption. Right: Emission measure distributions for the intervals indicated in the left plot, derived from the Withbroe–Sylwester routine. Vertical error bars indicate uncertainties. A cooler (temperature 4 - 5 MK) component is present over the entire time interval shown, with hotter component (~18 MK) at the peak of the GOES light curve.

During the flare’s maximum phase, the DEM analysis shows the X-ray-emitting plasma to have a basically two-temperature component, with the cooler plasma at approximately constant temperature (4–5 MK) and hotter plasma at ~18 MK. The cooler plasma is present before, during, and after the flare maximum.

(Barbara Sylwester, Janusz Sylwester, K. J. H. Phillips, Anna Kępa, Tomasz Mrozek)

SphinX SphinX soft X-ray spectrophotometer successfully operated aboard the Russian CORONAS-Photon satellite between February and December 2009. The instrument collected ~2 mln. spectra covering a period of very low solar activity, the lowest for approximately 100 years. No other X-ray instrument was capable of taking the X-ray spectra at such low activity and therefore the SphinX measurements are unique in this respect. The CORONAS -Photon, third spacecraft of this series, has been launched on 30 January 2009. Over the year 2013, comparison of SphinX measurements with other measurements

29 making similar X-ray measurements have been performed. In particular the MESSENGER data from SAX solar monitor has been used and fluencies compared in similar energy bands.

Fig. 4. The comparison of soft X-ray lightcurves as recorded by SphinX D1 detector (blue line) and two channels of MESSENGER SAX (in black and gray). For the period indicated, centered on the 19th of September 2009, the Messenger spacecraft looked at the same part of the solar corona as SphinX from Earth orbit.

A very good correspondence has been observed (as seen on the above plot). This indicates that the databases of SphinX and SAX complement each other, however the SphinX sensitivity for D1 detector is at least order of magnitude better than SAX. Quantitative analysis of common data set is in progress.

(Anna Kępa)

Solar corona during 2009 activity minimum Common analysis of the SphinX spectra and Hinode/XRT intensities for the most in-active corona observed allows to distinguish four clear features in the temperature distribution of emission (DEM): a colder emission below 1 MK (log T ≈ 5.9), the main maximum at ~1 MK (for log T in the range 5.9- 6.1), a the second maximum or enhancement at ~1.6 MK (for log T in the range 6.1- 6.4) and a hotter emission with T>2.5 (log T above 6.4). Using XRT temperature maps as obtained applying image-ratio technique allows to unveil the spatial arrangement of these different plasma temperature components in projection. Example of derived temperature maps is presented in the Figure below for 2009 February 21 0604 UT, the period of lowermost global solar soft X-ray flux yet measured.

Fig. 5. An example of temperature map obtained from Hinode/XRT data on 2009 Feb 21 06:04 UT. Black, blue, yellow, and red colors correspond to log(T) = 5.0 > 5.9 > 6.1 >6.4 ranges respectively as shown in the inset. The characteristic white network corresponds mainly to the CCD pixels where the contamination effects were pronounced. These pixels were not used for temperature mapping.

The colors represented plasmas at indicated temperatures. We can see that the colder emission corresponds to regions of coronal holes and above towards outer corona. Blue color corresponds to T in the range 0.8 – 1.3 MK i.e. close to “an average” quiet corona temperature is distributed over most of the disk. The yellow areas corresponds to somewhat hotter emission on DEM distribution with T in the range 1.3 – 2.5 MK constitutes left-overs of the “active corona” i.e. small active regions and the bright points. This hotter emission occupies also regions of inner corona close above the limb. The red color areas represent the quiet corona hottest emission where T > 2.5 MK. No red colors are seen within active regions and/or bright points due to saturation of respective XRT pixels. No hottest emission is seen on the disk, but it overwhelms the outer corona due to the line-of-sight integration effects. These results have never been obtained before and respective publication is under preparation (Marek Siarkowski et al.). They were discussed during the XVI Consultations on Solar Physics (22-25 May 2013) in Wrocław, Poland.

(Marek Siarkowski et al.)

Theoretical Modeling We (Sylwester Kołomanski, Tomek Mrozek and Barbara & Janusz Sylwester) continued modelling efforts of the response of solar atmosphere to flare energy release occurring in the corona confined within a “rigid” magnetic environment of coronal loop. For the first time, we modelled the evolution of plasma

31 along the loop throughout entire event, in the flare scenario considered covering approximately 1.5 day. Such a long modelling exercise was possible thanks to the access to supercomputers at the Wroclaw Academic Supercomputer Centre. For the first time we can study the late phase of flare evolution showing the “recovery” of flaring plasma to initial condition, before the flare heating initiation. On the diagnostic diagram shown, this decay-phase variability strictly follows so-called quasi-steady-stay cooling. This type of evolution is characteristic for the case of the heating operating quite long into the decay of the event.

Fig. 6. Example of time variability of physical conditions as modelled using the Palermo-Harvard HD code for a loop of semi-length 50 Mm. Time dependence of the plasma temperature T, density N and pressure P are plotted in the three upper-left diagrams in color, representing the time elapsed from switch-on of flare heating at t=500s. The fourth diagram (lower-right) represents so-called diagnostic diagram.

(Sylwester Kołomański, Tomasz Mrozek and Barbara & Janusz Sylwester)

Heliospheric physics (Laboratory for Solar System Physics and Astrophysics SRC)

Studies of the Galactic neighborhood of the Sun The journey of the Sun through the dynamically active local interstellar medium creates an evolving heliosphere environment. This motion drives a wind of interstellar material through the heliosphere that has been measured with Earth-orbiting and interplanetary spacecraft for 40 years. Recent results obtained by NASA's Interstellar Boundary Explorer mission during 2009 – 2010 suggest that neutral interstellar atoms flow into the solar system from a different direction than previously found. These

32 prior measurements represent data collected from Ulysses and otherspacecraft during 1992 – 2002 and a variety of older measurements acquired during 1972 – 1978. Consideration of all data types and their published results and uncertainties, over the three epochs of observation, indicates that the trend for the interstellar flow ecliptic longitude to increase with time is statistically significant. There is no obvious bias in the data that would explain the longitude trend, although possibly some uncertainties were underestimated. The variation in the interstellar wind longitude indicated by these historical data may be evidence for variations in the galactic environment of the solar system. These conclusions were published in the Science magazine by an international team of scientists led by P. C. Frisch, including M. Bzowski and J. M. Sokół from SRC PAS.

(Maciej Bzowski and Justyna M. Sokół)

A new diagnosis of two different states of the local interstellar medium (LISM) near our solar system, was carried out in the form of a sensitivity study constrained by several distinct and complementary observations of the LISM, solar wind, and inner heliosphere. Assuming the Interstellar Boundary Explorer (IBEX) He flow parameters for the LISM, the strength of the interstellar magnetic field in the Local Cloud equals to ~ 2.7 ± 0.2 μG and the direction pointing away from the galactic coordinates (longituide, latitude) = (28°, 52°) ± 3° was found based on fitting the Voyager 1 and Voyager 2 in situ plasma measurements and the IBEX energetic neutral atoms ribbon. When using the Ulysses parameters for the LISM He flow, the same field direction, but a lower strength of 2.2 ± 0.1 μG was recently reported. It was pointed out that with the Ulysses He flow, the solution obtained is in the expected hydrogen deflection plane (HDP). In contrast, for the IBEX He flow, the solution is ~20° away from the corresponding HDP plane. Secondly, the long-term monitoring of the interplanetary He flow speed shows a value of ~26 km s−1 measured in the upwind direction using the Doppler shift in the strong Lyα sky background emission line. All elements of the diagnosis seem therefore to support the Ulysses He flow parameters for the interstellar state. Based on these findings it was concluded that reliable discrimination between superfast, subfast, or superslow states of the interstellar flow should be based on in situ and remote observations carried out using various techniques and analyzed together with global modeling of the heliosphere. For the commonly accepted LISM ionization rates, a fast interstellar bow shock should be present upstream of the heliopause. These findings were published in The Astrophysical Journal by L. Ben Jaffel from Astrophysics Institute in Paris and R. Ratkiewicz, M. Strumik, and J. Grygorczuk from SRC PAS.

(Romana Ratkiewicz, Marek Strumik, and Jolanta Grygorczuk)

Studies of the distant heliosphere by in situ and remote-sensing observations A new high-resolution 2.5-D numerical MHD model of the plasma at the heliospheric boundary was developed. Using this model, processes related to magnetic reconnection and plasma turbulence occurring in the presence of the heliopause (HP) and the heliospheric current sheet were studied. It was shown that the interaction of plasmoids initiated by magnetic reconnection may provide connections between the inner and outer heliosheath and lead to an exchange of particles between the interstellar medium and the solar wind plasma previously shocked during the passage through the heliospheric termination shock (see Fig. 7). The magnetic reconnection may also cause plasma density and magnetic field compressions in the proximity of the HP. It was argued that these phenomena could possibly be detected by the Voyager spacecraft approaching and crossing the HP. These results seem to clarify the concepts of the “magnetic highway” and the “heliosheath depletion region” recently proposed to 33 explain recent Voyager 1 observations. The modeling results strongly support the hypothesis that the spacecraft has crossed the heliopause and is currently in the outer heliosheath. These conclusions were published in The Astrophysical Journal Letters by a team of SRC PAS scientists led by M. Strumik and including A. Czechowski, S. Grzędzielski, W.M. Macek, and R. Ratkiewicz.

(Marek Strumik, Andrzej Czechowski, Stanisław Grzędzielski, Wiesław M. Macek, Romana Ratkiewicz)

A study of expected signal from neutral energetic He atoms under various heliospheric scenarios was performed to check prospects for using He ENA as heliospheric information carriers. To that end, a model of heliosheath density and energy spectra of α-particles and He+ ions carried by the solar wind was developed. Neutralization of heliosheath He ions, mainly by charge exchange with neutral interstellar H and He atoms, was calculated to give rise to ~0.2 – ~100 keV fluxes of energetic neutral He atoms (He ENA). Such fluxes, if observed, would give information about plasmas in the heliosheath and heliospheric tail. Helium ions after crossing the termination shock constitute suprathermal test particles, convected by hydrodynamically calculated background plasma flows. Locally, these test particles undergo some diffusion. Three versions of flows were employed. The He ions proceed from the TS towards the heliopause and finally to the heliospheric tail. Calculations of the evolution of α- and He+ particle densities and energy spectra include binary interactions with background plasma and interstellar atoms (radiative and dielectronic recombinations, single and double charge exchange, stripping, photoionization and impact ionizations), adiabatic heating (cooling) resulting from flow compression (rarefaction), and Coulomb scattering on background plasma. It was found that neutralization of suprathermal He ions leads to the emergence of He ENA fluxes with energy spectra modified by the Compton-Getting effect at emission and ENA loss during flight to the Sun. Energy-integrated He ENA intensities are in the range ~0.05 – ~50 cm−2 s−1 sr−1 depending on spectra at the termination shock (assumed kappa-distributions), background plasma model, and look direction. The tail/apex intensity ratio varies between ~1.8 and ~800, depending on model assumptions. Energy spectra are broad with maxima in the ~0.2 – ~3 keV range, depending on the look direction and model. It was concluded that expected heliosheath He ENA fluxes may be measurable based on the capabilities of the IBEX spacecraft. Data could offer insight into the heliosheath structure and improve understanding of the post-termination shock solar wind plasmas. The heliotail direction and extent could be assessed. These results were published in Astronomy & Astrophysics by S. Grzędzielski, P. Swaczyna, and M. Bzowski.

(Stanisław Grzędzielski, Paweł Swaczyna, Maciej Bzowski)

The signal of non-planetary energetic neutral atoms (ENAs) in the 0.4–5.0 keV range, measured with the Neutral Particle Detector (NPD) of the ASPERA-3 and ASPERA-4 experiments on board the Mars and Venus Express satellites, was reanalyzed. Owing to improvements in the knowledge of the sensor characteristics and exclusion of data sets affected by instrument effects, the typical intensity of the ENA signal obtained by ASPERA-3 turned out to be an order of magnitude lower than in earlier reports. The ENA intensities measured with ASPERA-3 and ASPERA-4 now agree with each other. In the present analysis, we also correct the ENA signal for the Compton–Getting effect and for ionization loss processes under the assumption of the heliospheric origin of the signal. We find spectral shapes and intensities consistent with those measured by the Interstellar Boundary Explorer (IBEX). The principal advantage of ASPERA with respect to the IBEX sensors is the twice as good spectral

34 resolution. These observations are the only independent tests of the heliospheric ENA signal measured with IBEX in this energy range. The ASPERA measurements also allow to check for a temporal variation of the heliospheric signal as they were obtained between 2003 and 2007, whereas IBEX has been operational since the end of 2008. The results were published in The Astrophysical Journal by an international team of scientists led by A. Galli from the University of Bern, Switzerland, including M. Bzowski, J.M. Sokół, and M.A. Kubiak.

(Maciej Bzowski, Justyna M. Sokół, Marzena A. Kubiak)

Studies of neutral interstellar gas The interaction of the local interstellar medium with the solar wind shapes our heliospheric environment. Hydrogen is the dominant component of the very local ISM. The H distribution observed at 1 AU is expected to be different from the one outside the heliopause due to ionization, photon pressure, gravity, and filtration by interactions with heliospheric plasma populations. Interstellar hydrogen atoms move along trajectories that are quite different than those of heavier interstellar species such as helium and oxygen, which experience practically vanishing radiation pressure. Thus, a variation of the observed flux as a function of solar activity level is expected. Analysis of interstellar hydrogen sampled in situ by IBEX during the first four years of the mission was carried out and indeed, the hydrogen wind observed at 1 AU has decreased and nearly disappeared as the solar activity has increased over the last four years; the signal at 1 AU has dropped off in 2012 by a factor of ~8 to near background levels. The longitudinal offset of the observed inflow direction from the flow direction in the interstellar medium has also increased with time, presumably due to greater radiation pressure deflecting the interstellar wind. These observations provide an important benchmark for modeling the global heliospheric interaction. They were published in The Astrophysical Journal by a team of IBEX researchers led by L. Saul and including M. Bzowski and M.A. Kubiak from SRC PAS.

(Maciej Bzowski, Marzena A. Kubiak)

Extending this analysis, a team of IBEX researchers, led by N.A Schwadron from the University of New Hampshire and including M. Bzowski from SRC PAS, demonstrated clear effects of radiation pressure in a large longitudinal shift in the peak of interstellar hydrogen based on IBEX observations compared with that of interstellar helium. Specifically, results from the Lee et al. interstellar neutral model were compared with IBEX-Lo hydrogen observations to describe the distribution of hydrogen near 1 AU. They provided new estimates of the solar radiation pressure: it was found that over the period analyzed from 2009 to 2011, radiation pressure divided by the gravitational force (μ) increased slightly from μ = 0.94 ± 0.04 in 2009 to μ = 1.01 ± 0.05 in 2011. The speed, temperature, source longitude, and latitude of the neutral H atoms were also derived. It was found that they are roughly consistent with those of interstellar He, particularly when considering the filtration effects that act on H in the outer heliosheath. Thus, this analysis shows that over the period from 2009 to 2011, signatures of neutral H consistent with the primary distribution of atoms from the LISM and a radiation pressure that increases in the early rise of solar activity were observed. These findings were published in a paper in The Astrophysical Journal. The abundance of deuterium in the interstellar gas in front of the Sun gives insight into the processes of filtration of neutral interstellar species through the heliospheric interface and potentially into the chemical evolution of the Galactic gas. The possibility of detecting neutral interstellar deuterium at 1 AU from the Sun by direct sampling by IBEX was investigated by in-depth modeling studies. Using

35 both previous and the most recent determinations of the flow parameters of neutral gas in the Local Interstellar Cloud and an observation-based model of solar radiation pressure and ionization in the heliosphere, the flux of neutral interstellar D at IBEX for the actual measurement conditions was simulated. The number of interstellar D atom counts expected during the first three years of IBEX operation was assessed. Also the simulated observations were expected during an epoch of high solar activity. In addition, the expected counts of D atoms from the thin terrestrial water layer covering the IBEX-Lo conversion surface, sputtered by neutral interstellar He atoms, were simulated to make basis for comparison with actual observations, which contain the terrestrial water deuterium foreground. This study was published in Astronomy & Astrophysics by an international team of researchers led by M.A. Kubiak from SRC PAS and including also M. Bzowski and J.M. Sokół.

(Marzena A. Kubiak, Maciej Bzowski, Justyna M. Sokół)

Based on this modeling reconnaissance, the team identified interstellar deuterium atoms in the signal measured by IBEX-Lo. All data from the spring observation periods of 2009 through 2011 were analyzed. In the first three years of the IBEX mission time, the observation geometry and orbit allowed for a total LISM observation time of 115.3 days. However, the effects of the spacecraft spinning and stepping the observations through 8 energy channels reduced the effective observation time to 1.44 days. During this time, 2 counts for interstellar deuterium were identified. This number is conservatively assessed: because of a possibility of systematic error or additional noise in the data, though eliminated in our analysis to the best of our knowledge, the detection is supported only at a 1- sigma level. From these observations, the ratio D/H = 5.8 ± 4.4 × 10-4 at 1 AU was derived. After modeling the transport and losses of D and H from the termination shock to Earth’s orbit, it was -5 found that the result of (D/H)LIC = 1.6 ± 1.2 × 10 agrees with the abundance (D/H)LIC =1.6 ± 0.4 × 10-5 for the Local Interstellar Cloud. This weak interstellar signal was extracted from a strong terrestrial background signal, consisting of sputtering products from the sensor’s conversion surface. As a reference, the terrestrial D/H ratio in these sputtered products was accurately measured and then used to subtract this terrestrial background source. Because of the diminishing D and H signal at Earth’s orbit during the rising solar activity due to photoionization losses and increased radiation pressure, this result demonstrates that in situ measurements of interstellar deuterium in the inner heliosphere require a sensor with a much higher collection power. This result was published in Astronomy & Astrophysics by an international team of researchers led by D.F. Rodriguez from University of Bern, Switzerland, and including M. Bzowski, M.A. Kubiak, and J.M. Sokół from SRC PAS.

(Maciej Bzowski, Marzena A. Kubiak, Justyna M. Sokół)

Direct sampling of neutral interstellar atoms by IBEX can potentially provide a complementary method for studying element abundances in the LIC and processes in the heliosphere interface. An extensive study of ionization processes was performed to set the stage for abundance-aimed in- depth analysis of measurements of NIS He, Ne, and O by IBEX and determine systematic differences between abundances derived from various calculation methods and their uncertainties. Using a model of ionization rates of the neutral interstellar species in the heliosphere, based on independent measurements of the solar wind and solar EUV radiation, a time-dependent method of calculating the survival probabilities of neutral interstellar atoms from the termination shock of the solar wind to IBEX was developed. Densities of these species along the Earth’s orbit were calculated

36 and the fluxes of NIS species as observed by IBEX were simulated. Ratios of survival probabilities, densities, and fluxes of NIS species at IBEX were pairwise computed to calculate correction factors for inferring the abundances at the termination shock. It was found that the previously used analytic method of calculating the survival probabilities gives acceptable results only for He and Ne during low solar activity. For the remaining portions of the solar cycle, and at all times for O, a fully time- dependent model should be used. Electron impact ionization is surprisingly important for NIS O. Interpreting the IBEX observations using the time-dependent model yields the LIC Ne/O abundance of 0.16 ± 40%. The uncertainty is mostly due to uncertainties in the ionization rates and in the NIS gas flow vector. This value is in agreement with astrophysically-derived abundance of species in the solar Galactic neighborhood. These results were published in Astronomy & Astrophysics by a team of SRC PAS scientists M. Bzowski, J.M. Sokół, and M.A. Kubiak.

(Maciej Bzowski, Justyna M. Sokół, Marzena A. Kubiak)

Recently Sokół et al. (2012) presented a reconstruction of the heliolatitudinal and time variations of the solar wind speed and density. The method of the reconstruction was based on (i) measurements of the interplanetary scintillations, (ii) OMNI-2 solar wind data in the ecliptic plane, and (iii) Ulysses solar wind data out of the ecliptic plane. To verify these findings, hydrogen charge exchange rates derived from these results were used as input parameters to calculate the interstellar hydrogen distribution in the heliosphere in the frame of our 3-D time-dependent kinetic model. The hydrogen distribution was then used to calculate the backscattered solar Lyman-α intensity maps. The theoretical Lyman- α maps were subsequently compared with the SOHO/SWAN measurements during the maximum and minimum of the solar cycle activity. It was found that in the solar minimum there is a quite good agreement between the model results and the SWAN data, but in the solar maximum the sky maps of the Lyman-α, the intensities are qualitatively different for the model results and observations. The study was published in Journal of Geophysical Research by an international team led by O. Katushkina, including J.M. Sokół from SRC PAS.

(Maciej Bzowski, Marzena A. Kubiak, Justyna M. Sokół)

Studies of multifractal scaling properties of interplanetary magnetic field Continuing studies carried out during recent years, the multifractal scaling of the fluctuations in the interplanetary magnetic field strength, measured onboard Voyager 2 in the entire heliosphere were analyzed in greater detail. Specifically, spectra observed by Voyager 2 in a wide range of solar activity cycles during the years 1980 – 2009 at various heliospheric latitudes and distances from 6 to 90 astronomical units (AU) were analyzed. Focus was put on the singularity multifractal spectrum before and after crossing the termination heliospheric shock by Voyager 2 at 84 AU from the Sun. In addition, parameters of the model that describe the asymmetry of the spectrum, depending on the solar cycle, were investigated. It was pointed out that the spectrum is prevalently right-skewed inside the whole heliosphere. Moreover, a change in the asymmetry of the spectrum at the termination shock was probably observed. It was shown that the degree of multifractality is modulated by the solar activity. Hence these basic results also bring significant support to some earlier claims suggesting that the solar wind termination shock is asymmetric. These findings were published in Nonlinear Processes in Geophysics by W. M. Macek and A. Wawrzaszek.

(Wiesław M. Macek and Anna Wawrzaszek) 37

Studies of various space plasma processes The behavior of finite magnetic field lines during reconnection processes was studied. The field line motions were portrayed using the Euler potentials representation. A new insight into plasma flow fields related with magnetic reconnection was proposed. In this approach, reconnection is treated as a breakage of magnetic topology, which results in deviation from the line preserving flow regime. Constraints and general equations for these flows were derived. In this approach, the flux preserving flows are treated as a special case of the line preserving regime. Also a constraint on the non-ideal term in Ohm’s Law within diffusion regions was derived, which relates plasma flow with resistivity, and which must hold for non-reconnective diffusion. A new method of detecting magnetic reconnection was proposed. These results were published by a SRC PAS PhD student P. Figura and a SRC scientist W. M. Macek in Annals of Physics.

(Wiesław M. Macek, Przemysław Figura)

Analysis of measurements from the ESA/NASA Cluster mission showed in situ acceleration of ions to energies of 1 MeV outside the terrestrial bow shock. The observed heating can be associated with the presence of electromagnetic structures with strong spatial gradients of the electric field that lead to ion gyro-phase breaking and to the onset of chaos in ion trajectories. It results in rapid, stochastic acceleration of ions in the direction perpendicular to the ambient magnetic field. The electric potential of the structures can be compared to a field of moguls on a ski slope, capable of accelerating and ejecting the fast running skiers out of piste. This mechanism may represent the universal mechanism for perpendicular acceleration and heating of ions in the magnetosphere, the solar corona and in astrophysical plasmas. This is also a basic mechanism that can limit steepening of nonlinear electromagnetic structures at shocks and foreshocks in collisionless plasmas. These findings were published in European Physics Letters by an international team of scientists led by K. Stasiewicz from SRC PAS, including M. Strumik.

(Krzysztof Stasiewicz, Marek Strumik)

The velocity distribution of interstellar pickup ions (PUIs) has typically been described as evolving through fast pitch angle scattering, followed by adiabatic cooling while being transported radially outward with the solar wind. The slope of the observed pickup ion distributions is determined by a combined action of ionization processes, which control the radial profile of interstellar neutrals being the source population for PUI, and the PUI cooling processes. In the past, a cooling index of 3/2 for the PUI velocity distributions has been used in almost all studies. This value is based on the implicit assumptions of immediate PUI isotropization due to pitch angle scattering and solar wind expansion with the square of the distance from the Sun. In a study by an international team of scientists led by Ph.D. student J.H. Chen from the University of New Hampshire, including M. Bzowski and J.M. Sokół from SRC PAS, the observed PUI cooling index was determined for He+ PUI distributions observed with ACE SWICS at a ~30° interval in the upwind direction each year from 1999 through 2010, i.e., over the past solar cycle. The results were compared with an isotropic PUI model with the cooling index treated as a free parameter. The ionization rate was obtained for the actual observation time from independent observations. To extract effects of slow PUI pitch angle scattering, the comparison was repeated for the intervals when interplanetary magnetic field (IMF) was perpendicular to the solar wind expansion direction. When averaged over the entire data set, the cooling index turned out to be very close to 3/2. However, it varies substantially from 1.1 to 1.9 between samples, shows a distinct 38 variation with solar activity, and has a significant correlation with the sunspot number, when data is restricted to nearly perpendicular IMF ( θB,vSW > 60°), excluding the slow pitch angle scattering in the radial IMF direction. These findings were published in Journal of Geophysical Research.

Fig. 7. Illustration of simulation results: Top panel: early phase of the development of the phenomenon of plasma transport from the outer heliosheath inside the heliopause, initiated by magnetic reconnection and interaction between magnetic islands at the heliopause and the heliospheric current sheet. Only small intrusions of interstellar matter in the heliosphere are visible. Middle panel: the MHD equations used in the modeling lead to development of channels within which interstellar matter is transported covering large distances inside the heliosphere. Bottom panel: After some time, the transport of plasma through the heliopause ceases, but the interstellar matter intrusions remains inside the inner heliosheath, arranged in layers in the inner heliosheath.

(Maciej Bzowski, Justyna M. Sokół)

Ionospheric and magnetospheric physics (Plasma Physics Group SRC)

Turbulence in the magnetosphere and ionosphere The analysis of the low frequency fluctuations of the electric fields registered by DEMETER, CLUSTER, GEOTAIL and THEMIS satellites has been continued. The nonlinear phenomena that controls the interaction between plasma flow (solar wind) and magnetic barrier (magnetosphere). For the first time we have shown that the dominant solar wind kinetic energy: excites boundary resonances and their harmonics which modulate plasma jets under the bow shock; produces discrete 3-wave cascades, which could merge into a turbulent-like one; jet produced cascades which provide the effective anomalous plasma transport inside and out of the magnetosphere. We analyzed the disturbances registered by DEMETER prior to the earthquake starting 2 weeks before this event. Special attention was given to the characteristics of the spectra of these variations and the search of nonlinear effects. This analysis is possible in the time intervals when the ELF waveform has been transmitted. The observations done by DEMETER suggested the presence of plasma turbulence over seismic areas. The characteristics of the observed disturbances are studied with wavelet and bispectral analysis, the tools which are more relevant to analyze plasma turbulence. The characteristics of the turbulence over seismic regions have been compared to the characteristics of the turbulence in the polar cusp, polar trough and in the equatorial ionospheric anomaly. The turbulent cascades have been noted in all discussed cases. The PhD thesis on this subject is in the final stage of preparation.

Fig. 8. Wavelet spectrogram of the electric field variations over epicenter of Chile earthquake (27February 2010) registered by DEMETER satellite 9 days before the event.

Fig. 9. Evolution of the bispectra during flight over Chile epicenter showing developing of the turbulence cascade.

Fig. 10. Power spectrum for the given in the previous figures event. The slope of the spectrum indicate mhd character of the turbulence.

Fig.11. Global distribution of the ELF turbulence in the ionosphere as seen by DEMETER satellite.

(Jan Błęcki, Małgorzata Kościesza, Jan Słomiński, Roman Wronowski)

The discussion of the possible source of the low frequency plasma waves registered by CLUSTER in the polar cusp has been conducted. These waves have been registered in the polar cusp as emissions with high intensity below the electron cyclotron frequency by Interball 1. They correlate with strong fluxes of high energetic electrons observed within the polar cusp by Interball 1 and Magion 4. Similar effects have been registered by Polar satellite. Cluster measurements give new insight of these emissions. Taking into account the plasma and magnetic field parameters in the polar cusp as well as geometry of the waves propagation, it been found that these emissions can be generated by so called “fan instability”, but also horse shoe instability can be discussed. Both instabilities play important role in the nonlinear wave –particle interactions leading to the isotropisation of the fluxes of the particles and heating of the plasma. Another mechanism of generation of these emissions- relativistic cyclotron maser has been studied, but the result was negative.

(Jan Błęcki, Krzysztof Mizerski)

Transient Luminous Events in the upper atmosphere The main goal of the JEM-EUSO experiment are studies of the extremely high energetic cosmic rays (1019 - 1021 eV), but method which will be used (registration of the secondary light emissions induced by cosmic rays in the atmosphere) allows to study other luminous phenomena. The UHERC will be detected through the registration of emission in the range between 290 to 430nm. In this range some part of TLEs emission also appears. We have discussed the possibility of the use JEM-EUSO to get new scientific results on TLEs. The high time resolution of this instrument allows to see evolution of TLEs with great precision just in the moment of their origin. Our discussion was directed to study the possible progress of science in this field with the use JEM EUSO and possible cooperation with other space projects devoted to study of TLEs - TARANIS and ASIM. Studies of the TLE became one of the main physical problems in the atmospheric physics. They were discovered in 1989. In years 1992 - 1994 the registrations from satellite, aircraft and space shuttle were done and recently from International Space Station. These events have short duration (milliseconds) and small scales (km to tens of km) and appear at altitudes 50 - 100km . Their nature is still not clear and each new experimental data can be useful for better understanding these mysterious phenomena.

Fig. 12. A schematic overview of different types of the Transient Luminous Events. http://upload.wikimedia.org/wikipedia/commons/c/c4/Upperatmoslight1.jpg.

Fig.13. Modeling of the temporal evolution of ELV as can be seen by JEM EUSO telescope.

(Jan Błęcki, Kinga Słomińska, Jan Słomiński )

Modeling of space plasma processes About 5200 AKR sources’ positions (equivalent to about nine hours of observations) measured with POLRAD experiment (Interball-2 mission) have been statistically analyzed. Two coordinate systems have been employed: (1) - Tangent Plane (TP) coordinates proposed by Mutel et al., 2008] (angular coordinates: TP longitude and TP latitude) and (2) - classical spherical coordinates system with symmetry axis aligned with local magnetic field line direction at the AKR source (angular coordinates: emission angle measured with respect to the local magnetic field direction at the AKR source and azimuth measured with respect to direction tangent to circle of constant magnetic latitude). Histograms of TP latitude and longitude confirmed basic findings of Mutel et al., [2008], in particular the concentration of AKR beams close to the plane tangent to the auroral oval (or strictly speaking, circle of constant geomagnetic latitude). Second coordinates’ system is well suited for finding AKR beams strongly deflected from the auroral oval - small number of such beams have been identified in POLRAD's data (Fig.14). They are not reported in Mutel et al., [2008] paper – TP coordinates are not good for such analysis, but recently Menietti et al., [2011] modeled AKR spectra observed onboard POLAR s/c and produced by auroral arcs oblique to the auroral oval. For shorter time spans (up to 10 minutes, when the movement of s/c with respect to the far AKR sources can be neglected) AKR visibility maps for single s/c have been introduced. They are similar to joint visibility maps introduced by Mutel et al. for 4 CLUSTER s/c. With our maps we can directly visualize both azimuth and emission angle for single measurements of AKR sources positions (Fig.14A). AKR sources’ positions in Invariant Latitude - MLT coordinates for all analysed data are shown on.

Fig.14. Histograms of AKR beams azimuth and emission angles as determined for all data (A), and for cases of AKR beams not tangent to the auroral oval (B).

Fig.15. Example of AKR visibility map (A), and AKR sources positions in InvLat - MLT coordinates for all data (B).

(Roman Schreiber, Jan Hanasz)

CALIBRA: Countering GNSS high Accuracy applications Limitation due to ionospheric disturbance in BRAzil

CALIBRA is a collaborative project under the Seventh Framework Program (FP7) funded by European GNSS Agency (GSA) and coordinated by Nottingham Geospatial Institute (NGI) at the University of Nottingham. For project purposes the preliminary version of the local empirical model of parameters that describe the propagation of the L-band signal, have been developed for Brazil region, where strong scintillations are observed. The model is based on the transport process described by the continuity equation. Experimental TEC data obtained from Cigala network is used for constant velocity field reconstruction, that forms an input for TEC field predictions. The predictions are calculated by integration of the passive scalar transport equation. First results have been described in D2.2 FP7 CALIBRA internal report. An example of the short-term (up to 20 min) TEC field predictions have been presented. The predictions were based on the FP7 CIGALA archival data from the 1st of November 2011 in strong scintillations regime.

Fig. 16. Reconstructed velocity field. Green arrows presents the velocity vector of magnitude 100 m/s.

Fig. 17. Example of TEC predictions. Red colour is the predicted TEC, and green dots are measured TEC data. 46

These preliminary results can be further incorporated in the development of the system for differential position corrections for Brazil area. The current model will be expanded for forecasting scintillation parameters such as S4, for purposes of stochastic algorithm for position derivation.

(Marcin Grzesiak)

Performance analysis and perspectives of automatic whistler detection Whistler method for studying plasma properties allowed for plasmasphere discovery over a half century ago. Up to now it is relatively cheap tool used in magnetospheric research by means of remote diagnostics. Our work aimed at the automatic detection method of the whistlers. Due to characteristic dispersive properties the most suitable approach deals with the representation in time-frequency domain. In that domain we perform summation along with the whistler trace for set of two parameters: time and alpha. Alpha is the parameter that scales the time-frequency relation. The summation process consists of two parts. In first approach we transform spectrogram image using the dispersion relation so that the whistler traces are represented by vertical lines (see Figure 18). Second step is simply summation along each column.

Fig. 18. Left picture is the whistlers spectrogram (DEMETER data). Right picture is the same spectrogram after the 'generalised' Radon transform was applied.

As a result we obtain another 2D image in time-alpha parameter space, where local maxima indicates possible presence of a whistler trace. Coordinates in the time-alpha parameter space describe whistler trace properties in the same time. The method was tested on synthetic spectrograms, example of which is on Figure 19 (left). Right image on Figure 19 is the spectrogram representation in time-alpha domain.

Fig 19. Figure on the left presents synthetic whistler traces computed with use of the low-frequency approximation. Right- side figure presents the space, where the maxima (red areas on the image) indicate the possible presence of whistler in the time (x-axis) and alpha (y-axis) space, where alpha is the parameter responsible for whistler shape.

(Dorota Przepiórka, Marcin Grzesiak, Hanna Rothkaehl) Mid-latitude trough studies The mid-latitude trough, located on the equatorward side of the auroral oval, is the region of depleted ionisation. The structure can be observed in both hemispheres for almost whole year. It is mainly night- time phenomenon, most regularly seen during local winter. Its detailed characteristics and features depend on the solar cycle, season, time of the day and many others. The main trough is extended in longitudes but narrow in latitudes. It is storm-phase depended structure, very sensitive for geomagnetic conditions. Mid-latitude trough is considered as a plasmapause projection onto the ionosphere. During intensified geomagnetic activity the magnetosphere is the subject of the compression caused by the pressure of the Solar Wind. In result a plasmapause can be observed at lower L-shell. Registration of electron concentrations and temperatures shows that the mid-latitude trough tends to move equatorward with enhanced geomagnetic activity (towards lower L-shell).

Fig. 20. Electron density distribution (left) and electron temperatures (right) during geomagnetic storm in January 2005 at selected longitudinal location for the consecutive days since 18 January till 24 January. The minimum Dst value was observed in 22 January (magenta line). Data obtained from DEMETER ISL experiment.

Fig. 21. Position of mid-latitude trough minimum during different geomagnetic conditions in 2005. Left panel shows that for Kp in range 0-2 MIT occurs at latitudes about ±60˚ and for higher geomagnetic activity Kp=4-6 (right panel) trough moves equatorward reaching up to ±50˚ of geomagnetic latitude. Data obtained from DEMETER ISL experiment.

Fig. 22. Seasonal variations of electron density during 2005 (left) and 2007 (right). Maps show typical behaviour of trough structure strongly correlated with annual insolation. Phenomenon intensifies during local winter for both hemispheres ( 2nd panel for southern and 4th for northern hemisphere) and almost disappears for local summer.

(Dorota Przepiórka, Barbara Matyjasiak, Hanna Rothkaehl)

SWEX program During 2013, Plasma Physics Group continued the program SWEX (Soil Water and Energy eX- change) for validating ESA SMOS Mission (Soil Moisture and Ocean Salinity) for Soil Moisture (SM) data in Poland. This year SMOS for the first time, experienced less RFI contamination from Poland than before. However RFI cleanliness in Poland at 1.4 GHz is still 2 orders above international ITU standards. Therefore the group keeps monitoring RFI, and undertook other actions on preventing SMOS observations against pollution. SWEX contributes to a wider global validation program in frames of ESA SVRT (SMOS Validation and Retrieval Team). Since January 2013 SWEX runs without financing for the sake of keeping and updating the 4th year of Soil Moisture data from SMOS globally, within our particular scope on Europe and Poland. The SMOS data base has a very decisive meaning for all research topics related to the Climate Change (CC) and Water Cycle on large regional. The group keeps elaborating our own L3 products for Poland, and cooperating with the action of COST-1001 SMOS-MODE focused on 49 employing SMOS data over oceans. SMOS is one of the most innovative EO missions, related to CC, in scientific goals and targets as well as in technological means. Innovative importance of SMOS is in microwave polarization radiometry employing full Stokes vector methods, and in creating new standards of watching fundamental climate ECVs (Environmental Climate Variables) from space and monitoring on the ground. Currently we cooperate with IA_PAN, Lublin in agrophysical soil aspects of SMOS and negotiate with ESA possibilities of installing few Validation Super-Sites for ESA EO from Sentinel-1, SMOS, and NASA SMAP in Poland. Currently ground based measurements for monitoring ECV variables are in focus of GEOSS to mature new global standards on Quality Assurance (QA4EO). The SWEX team is still the partner contributing to ISMN (International Soil Moisture Network) TUWIEN. Wide range of our activities related to SMOS brought also additional support to possible ionospheric researches by Ewa Słomińska who wrote PhD Thesis “Signatures of the Midlatitude Nightime Summer Anomaly in the Topside Ionosphere – Analysis of the 6-year Trend from the Demeter Mission”, completed in 2013. Other effects of our activities are in keeping correspondence to past achievements in engineering by W. Marczewski who in 1994 proposed particular design solutions related to the Stokes Vector Detection and now they find correspondence to SMOS technology. In this thread the invention USPat. 4755775 on “Microwave balun for modulators and mixers” made with CBK PAN in 1983, is accounted for more than 4000 patent related citations now in 2013. It is a noticeable longterm achievement of W. Marczewski in the engineering area related to SMOS worth quoting.

Fig. 23. Three day cycle C3_EU_SM values within SMOS L2 data in 14-16 February 2014. For the mostly wet regions in Europe are Andalusia and southern Portugal.

(Wojciech Marczewski, Ewa Słomińska, Jan Słomiński)

B-spline model of the ionospheric scintillation Ionospheric scintillation is defined as a random fluctuations of radio waves transmitted from the satellite and received on the ground. Scintillation is caused by diffraction on electron density irregularities. Since scintillation can disturb the satellite transmission it is an important component of, so called, space weather. Attempts to model scintillation for prediction purposes have long history. In our approach we used satellite in situ data to construct climatological model of scintillation variations at high latitudes.

Fig. 24. Maps of the spectral index for electron density fluctuations and scintillation index S4 derived using the B-spline model.

Parameters upon which scintillation is dependent on are derived from DE 2 satellite data as a function of local time, season, invariant magnetic coordinates, Kp index and solar flux value F10.7, are expressed as simultaneous products of univariate normalized B-splines. The satellite data is appended with parameters derived from ionospheric model. Those are: peak electron density, peak height, irregularity slab thickness. Maps of the input parameters are constructed to visualize the pattern of their variations. Finally the maps of the scintillation index are constructed. Examples of such maps are shown in Figure 24.

(Shishir Priyadarshi and Andrzej W. Wernik)

Ionospheric Statistical Analysis of High and Low Latitude Scintillation Studies For the decades ionospheric scintillations represented the problem for the science and industry, affecting satellite and ground radio signals, especially in high and low magnetic latitudes. Modeling and simulating ionospheric plasma dynamics and scintillations influence of the radio wave signals represents an important source for building scintillation mitigation techniques. Previous researches in the field of GNSS scintillating signal statistics and ionospheric modeling gave various solutions in the probability of distribution of the scintillation signals and predictions of the ionospheric plasma processes and their influences on propagating signal phase and power, but neither of them represents an easy solution. In 51 order to get information about the probability of distribution function of scintillating signal, statistical analysis have been done using higher order moments of phase and power of the signal, as the a tools for testing the probability of distribution functions. Research was done for the periods of strong and moderate geomagnetic storm periods during 5-6th of April 2010 for the ground GPS monitoring data at Hornsund Bay, Svalbard and 1st of November 2011 for measurements made by GPS receiver set at Presidente Prudente, Brasil. Examination was performed by a comparison of the probability of distribution function obtained from measured data and theory. Probability distribution function test on higher order moments shows that strong amplitude scintillations of the GPS signal is not following Gaussian, and contrary to wide understanding it follows Nakagami-m distribution just in some cases. This results lead to necessity for improvements of accuracy in the ionospheric scintillation modeling and possible enhancements in scintillation forecasting and prediction.

Fig. 25. Each of the plots illustrates higher order moments dependences of scintillation indices for 5th (left column) and the 6th of April 2010 (middle column) and the 1st of November 2011 (right column). Solid lines in the upper graphs represent fitted theoretically derived skewness (blue) and kurtosis (red) from Nakagami distribution function for signal power.

(Dorde Stevanović, Andrzej W. Wernik)

Regional Ionosphere Mapping with Kriging and B-spline Methods The concept and practical examples of mapping of regional ionosphere, based on GPS observations from permanent stations near to the EGNOS Ranging and Integrity Monitoring Stations (RIMS) network. Interpolation/prediction techniques, such as kriging (KR) and the cubic B-spline, which are suitable for handling multi-scale phenomena and unevenly distributed data, were used to create total electron content (TEC) maps. Their computational efficiency (especially the B-spline) and the ability to handle undersampled data (especially kriging) are particularly attractive. The time series of the TEC maps can be used to derive average monthly maps describing major ionospheric trends as a function of time, season, and spatial location. While creating each map, a semivariogram and cross-semivariogram were calculated and introduced during the data interpolation. The applied approach enables creating the local ionosphere maps for every observational epoch. The comparison between the results obtained using this two methods shows good agreement. The differences in the TEC levels shown by both maps do not exceed 1 TECU.

TEC maps 2012-09-30 06:00:00 UT TEC maps 2012-09-30 12:00:00 UT TEC maps 2012-09-30 18:00:00 UT

Fig. 26. Ionospheric TEC maps created with Kriging (a) and cubic B-spline (b) interpolations methods.

(Oksana Grynyshyna-Poliuga, Iwona Stanisławska, Anna Świątek)

The observed auroral oval equatorward boundary during four magnetic superstorms was compared with the predicted convection boundary from Weimer2005 model for appropriately averaged solar wind conditions. Data on far ultraviolet aurora is from TIMED GUVI instrument. Dynamics of the oval is also compared with the change of Newell et al.'s coupling functions, the SYMH index, and the solar wind electric field. During quiet time preceding magnetic storm onset the statistical convection boundary is very close to the observed oval equatorward boundary at the level above 250 R in LBHL emission (equivalent to ~2 erg/(scm2 of precipitating electron energy flux). During the main phase both boundaries in general move in the phase toward lower latitudes, with statistical convection penetrating to middle latitudes well equatorward of the ultraviolet aurora boundary. At the beginning of recovery phase the aurora and convection equatorward boundaries may again be close to each other. We also compared the equatorward boundaries of statistical Kp-dependent model of the FUV aurora and Weimer2005 statistical model of solar-wind driven convection in the ionosphere. For analyzed 95 cases of ~ half-an hour superstorm intervals, in 75 cases the statistical convection pattern is confined within the area of Zhang-Paxton statistical model of auroral electron precipitation at the level above 0.2 erg/(scm2). These results suggest that Weimer2005 electric potential model may be used for prediction of aurora latitudinal extent with time resolution much better than Kp-dependent Zhang-Paxton model.

Fig. 27. Top: 20 November 2003 superstorm. Comparison of the equatorward boundary of LBH2 auroral emission (250 R level, black points) and the model equatorward boundary of solar-wind driven ionospheric convection (red dashed lines are +/-0.5 kV electric potential isolines). Solar wind input to Weimer2005 model corresponds to the time of the center of auroral oval passed over by TIMED. Auroral emission data are shown only when the relevant solar zenith angle is larger than 100 degrees. Bottom: Dynamics of oval boundary (points) and convection boundary (lines) during the main and recovery phase of the storm.

Fig. 28. Examples of comparison of the Zhang-Paxton Kp-dependent auroral precipitation model with the solar-wind driven ionospheric convection model of Weimer (2005), computed with the use of real solar wind parameters. Reference time for model convection is the time of oval center passage by TIMED.

(Maria Bojanowska and Barbara Popielawska)

Usually the main attention is paid to plasma turbulence investigation at well developed stage, when the wide spectrum of plasma wave is present. On the other side, it is well known that even system with finite number of interacting waves can realize a turbulent state in active media. In such cases, when the number of cooperating waves remains small due to a competition of processes of their instability and attenuation, the turbulence appears in the result of their stochastic behavior. The strong collisional damping of waves allow to assume that in the considering case a typical perturbed state of plasma can be described as finite set of interacting waves, some of which are unstable and other strongly damping.

Fig. 29. Scheme of 7 wave cascade.

Numerical study of 7 wave two step cascade demonstrates the possibility of different regimes of a few wave turbulence – periodic, multi periodic and stochastic regimes. As shown, the number of waves truly represent the turbulent state that is set according to the parameters that determine the initial instability in the system (the intensity of the power source). It is independent of the number of waves in the numerical simulations (if the number of waves included in the model is large enough). Thus, the simulation results with 7 waves show that the actual realization of the parameter data base is a cascade of 3 waves.

Fig. 30. The example of simulation.

(Barbara Atamaniuk)

We present measurements from the ESA/NASA Cluster mission that show in situ acceleration of ions to energies of 1MeV outside the bow shock. The observed heating can be associated with the presence of electromagnetic structures with strong spatial gradients of the electric field that lead to ion gyro-phase breaking and to the onset of chaos in ion trajectories. It results in rapid, stochastic acceleration of ions in the direction perpendicular to the ambient magnetic field. The electric potential of the structures can be compared to a field of moguls on a ski slope, capable of accelerating and ejecting the fast running skiers out of piste. This mechanism may represent the universal mechanism for perpendicular acceleration and heating of ions in the magnetosphere, in the solar corona and in astrophysical plasmas. This is also a basic mechanism that can limit steepening of nonlinear electromagnetic structures at shocks and foreshocks in collisionless plasmas.

Two ion trajectories superimposed on Φ contour-plot that represents the two-dimensional field of moguls. (Krzysztof Stasiewicz)

PHYSICAL AND GEODETIC STUDIES OF SOLAR SYSTEM BODIES AND EARTH

Planetology and Solar System Dynamics

The spectrometric research (modelling and interpretation of data) in VIS to far IR spectral range was being continued. The investigations were connected with the present and future space mission experiments: VIRTIS/VEX, PFS/MEX, HIFI/Herschel and VIRTIS/Rosetta. The spectra of Venus (mainly day-side) were simulated, and the searching for a new aerosols in the atmosphere of Venus was continued. However, the activity was mostly concentrated on the numerical modelling connected with the VIRTIS instrument – part of the payload of the Rosetta mission to the Comet 67P/Churyumov-Gerasimenko (In May 2014, the Rosetta spacecraft will enter orbit around the comet). The main purpose was to examine the influence of the comet state and dust parameters on the thermally emitted and scattered signal in various configurations of the measurements taken by VIRTIS instrument. Interpretation of the measurements requires modelling of the radiance from the nucleus and from the dusty/gas environment of the comet. The thermally emitted and scattered radiation from the dust and molecules was simulated. The emitted radiation is especially important part of the signal in the 2.5µm–5.0µm spectral range. The equation of radiative transfer in the range from 1.0µm to 5.0µm through the assembly of dust grains and gases were solved for various cases. The sizes and number density distribution of the dust grains around the coma are drawn using the recent theoretical simulations and Inner Coma Environment Simulation tools (ICES).

The role of dust and aerosols in the radiative transfer equation was analysed and new subroutines for “limb” geometry were successfully applied. Influence of dust on radiance spectra, the crucial point of interpretation the spectral measurements of Comet 67P/Ch-G, was carefully examined and analysed using various methods. As an example: the simulated radiances from the dust/water jets on Enceladus were compared with Monte-Carlo calculations performed by the Italian group from IAPS (Istituto di Astrofisica e Planetologia Spaziali). The influence of parameters of dust and the emittance of Valles Marineris and Hellas regions of Mars on spectra has been recalculated but comparison with the real data is still problematic. The comparison of the measurements of CO by PFS and HIFI was finished and the paper to Astronomy &Astrophysics journal is in preparation (authors: Maria I. Błęcka, Giuseppe Sindoni, Paul Hartogh, Christopher Jarchow, Emannuel Lellouch, Miriam Rengel and Herschel/HIFI TEAM). The problem of water on early Mars was continued in the grant team led by Hans Rickman. The paper on the age of phillosilicates entitled The age of the substances formed in the presence of water on Martian surface – the crucial point in the problem of possible existence of post Noachian water on Mars was finished and submitted to Origins of Life and Evolution of Biospheres. (Maria I. Błęcka)

Operation of CONSERT aboard Rosetta during the descent of Philae • The separation–descent–landing part of the Rosetta mission can be used by CONSERT. • The CONSERT instrument can perform classical radar sounding during descent. • The radar sounding performance is studied in detail. • Valuable data can be collected, which will support CONSERT's main goals. • Data of the direct path can be used to reconstruct the lander descent dynamics. Abstract: This paper presents a study investigating the performance of using the CONSERT instrument aboard the Rosetta spacecraft as a radar sounder during the Separation–Descent–Landing (SDL) phase of the Rosetta mission. Gathering scientifically valuable data during this phase will support CONSERT's primary target, the reconstruction of the 3D permittivity distribution within the comet 67P/Churyumov–Gerasimenko, by providing a permittivity map of the surface around the landing site. Simulation results will show the performance of the instrument, using a realistic setup including the antenna characteristics of both orbiter and landing unit as well as a realistic orbitography for the descent phase. It will show that operating the CONSERT instrument will indeed provide very valuable data, thereby providing tremendous aid to the experiment's main objective. Furthermore, by including knowledge of the antenna characteristics, it is possible to calculate attitude and descent profile of the Philae lander during descent, using the data of the line-of-sight propagation path and the echoes reflected from the comet's surface.

(S. Hegler, Ch. Statz, R. Hahnel, D. Plettemeier, A. Herique, Włodek Kofman)

A Herschel study of D/H in water in the Jupiter-Family Comet 45P/Honda–Mrkos– Pajdušakova Herschel Space Observatory observed water isotopologues in the atmosphere of the Jupiter-family comet 45P/Honda–Mrkos–Pajdušakova. Observations of comet 45P/H-M-P were carried out on the 13th of August 2011, when a geocentric distance was only 0.06 AU. The observing sequence consisted 18 of H2O, H2 O, HDO lines and three water emission maps (at 557 GHz and 988 GHz). The derived water production rate increased with time from 9×1026 s−1 to 1.0×1027 s−1. No HDO emission was 57 detected, with a 3σ upper limit of 0.0002 for the D/H ratio. This value is consistent with the earlier Herschel measurement in the Jupiter-family comet 103P/Hartley 2. In the later comet a low ratio of 0.000161 (at a 1σ level) similar to the Earth-ocean D/H ratio was determined (Hartogh at al. 2011). Twice the ocean water value of 0.0003 measured pre-Herschel in a sample of Oort-cloud comets can be excluded at a 4.5σ level. The D/H ratio in cometary water is an important indicator of the conditions under which comets formed and can also provide clues to the contribution of comets in the delivery of water to Earth. The earlier Herschel’s observations of long-period comet C/2009 P1 (Garradd) showed that the D/H in the water of Oort-cloud comets is not as high as previously thought, at least for a fraction of the population (Bockelée-Morvan et al. 2012). In that way the recent measurements clearly demonstrate that the high pre-Herschel D/H values are not representative of all comets and confirm that a diversity of D/H ratios exists in the comet population. Additional measurements with future ground-based facilities, in the post-Herschel era are needed. The results of comet 45P/H-M-P were published in the Astrophysical Journal Letters.

(Team of Herschel Solar System Observations (HssO) researchers and Sławomira Szutowicz)

Searches for HCl and HF in comets 103P/Hartley2 and C/2009P1 (Garradd) with the Herschel space observatory HCl and HF are expected to be the main reservoirs of fluorine and chlorine over a wide range of conditions, wherever hydrogen is predominantly molecular. They are found to be strongly depleted in dense molecular clouds, suggesting freeze-out onto grains in such cold environments. We can expect that HCl and HF were also the major carriers of Cl and F in the gas and icy phases of the outer solar nebula, and were incorporated into comets. We searched for the J(1–0) lines of HCl and HF at 626 and 1232 GHz, respectively, using the Heterodyne Instrument for the Far- Infrared (HIFI) on board the Herschel Space Observatory. HCl was searched for in comets 103P/Hartley2 and C/2009 P1 (Garradd), whereas observations of HF were conducted in comet 18 C/2009P1. In addition, observations of H2O and H2 O lines were performed in C/2009 P1 to measure the H2O production rate at the time of the HCl and HF observations. HCl was not detected, whereas a marginal (3.6 σ) detection of HF was obtained. The upper limits for the HCl abundance relative to water are 0.011% and 0.022%, for comet 103P/Hartley2 and C/2009P1 (Garradd), respectively, showing that HCl is depleted with respect to the solar Cl/O abundance by a factor more than 6 in 103P/Hartley 2. The marginal HF detection obtained in C/2009 P1 corresponds to an HF abundance relative to water of (0.00018±0.00005), which is approximately consistent with a solar photospheric F/O abundance. The inferred water production rate in comet C/2009P1 was (1.1±0.3)×1029s−1 and (0.75±0.05)×1029s−1 on the 17th and 23rd of February 2012, respectively. The observed depletion of HCl suggests that HCl was not the main reservoir of chlorine in the regions of the solar nebula where these comets formed. HF was possibly the main fluorine compound in the gas phase of the outer solar nebula. However, this needs to be confirmed by future measurements. These results were published in Astronomy & Astrophysics. (HssO team and Sławomira Szutowicz)

Activity of Comet 29P/Schwassmann–Wachmann 1 Comet 29P/Schwassmann–Wachmann 1 is a continually active object moving along nearly circular orbit at a large heliocentric distance ~6AU. The comet is famous for its repeated outbursts-sudden events in which the brightness increases by 1–5 mag. We look for structure and composition of the nucleus that leads to the observed frequent outbursts. We performed the series of numerical simulations dealing with evolution of the nucleus, including changes of the structure and of the CO gas 58 pressure. In our model the porous nucleus has layered structure. Outermost layer is composed of grains with nonvolatile cores mantled by crystalline water ice. Deeper the grains have three components: nonvolatile cores, amorphous water ice and, the carbon monoxide ice. The simulations include crystallization of amorphous ice in the nucleus, sublimation of the CO ice and local explosions. We have found, that for an equatorial location the explosions can be expected only in special case, when the nucleus is finely grained, fluffy and rich in CO. In polar regions explosions are possible for almost any composition and structure of the nucleus. Explosions can be either single, or multiple. The results were published in the Icarus. (Konrad J. Kossacki and Sławomira Szutowicz)

Fig. 31. Figure shows evolution of the CO gas pressure within the nucleus versus time for an area located at the south pole (the rotation axis lies in the orbital plane). The volume fraction of the CO ice is 0.10, the ratio CO:H2O is 32%, and the porosity of the nucleus is 0.4. The nucleus is moderate cohesive. The profiles demonstrate strong influence of the granulation of the cometary material on the number of explosions. Model predicts: two large explosions per orbital period for the coarse grained nucleus (rg=20µm); and multiple explosions for fine-grained nucleus (rg≤10µm). For the very finely- grained nucleus model predicts one large explosion followed by the long series of small, indistinguishable ones. Duration of the series of these outbursts is about 0.2 of the orbital period i.e. 3 years. (from Kossacki and Szutowicz, 2013, Icarus).

Surface properties of Comet 9P/Tempel 1 A 3D code for heat flow under a rough surface of a rotating and insolated, atmosphere-less object was developed by B.J.R. Davidsson and H. Rickman. This was used within an international collaboration focused on utilizing the close-up observations of the nucleus of Comet 9P/Tempel 1 performed by the Deep Impact and post-Stardust-NExT spacecraft. The observational material consisted of re-calibrated near-infrared spectroscopy, a global shape model and a spin pole solution. Surface heterogeneities in terms of both thermal inertia and roughness were clearly identified. Parts of the surface appear to be very rough, and the thermal inertia is generally very low but variable. This was published in Icarus (2013). (Hans Rickman & International team led by B.J.R. Davidsson)

Near-parabolic comets observed in 2006—2010. The individualized approach to 1/a- determination and the new distribution of original and future orbits Dynamics of a complete sample of small perihelion distance near-parabolic comets discovered in the years 2006–2010 were studied (i.e. of 22 comets of perihelion distance below 3.1AU). First, osculating orbits were obtained after a very careful positional data inspection and processing, including where appropriate, the method of data partitioning for determination of pre- and post-perihelion orbit for tracking then its dynamical evolution. The non-gravitational (NG) acceleration in the motion was detected for 50 per cent of investigated comets, in a few cases for the first time. Different sets of NG parameters are determined from pre- and post-perihelion data for some of them. The influence of the positional data structure on the possibility of the detection of NG effects and the overall precision of orbit determination is widely discussed. Secondly, both original and future orbits were derived by means of numerical integration of swarms of virtual comets obtained using a Monte Carlo cloning method. This method allows us to follow the uncertainties of orbital elements at each step of dynamical evolution. The complete statistics of original and future orbits that includes significantly different uncertainties of 1/a-values is presented, also in the light of our results obtained earlier. Based on 108 comets examined by us so far, we conclude that only one of them, C/2007W1 Boattini, seems to be a serious candidate for an interstellar comet (see also Fig. 32). We also found that 53 per cent of 108 near-parabolic comets is escaping from the Solar system in the future, and the number of comets leaving the Solar system as so called Oort spike comets (i.e. comets suffering very small planetary perturbations) is about 14 per cent. A new method for cometary orbit quality assessment is also proposed by means of modifying the original method, introduced by Marsden, Sekanina & Everhart. This new method leads to a better diversification of orbit quality classes for contemporary comets. These results were published in the Monthly Notices of the Royal Astronomical Society.

(Małgorzata Królikowska and Piotr A. Dybczyński)

Catalogue of orbits of 119 near-parabolic comets This Catalogue presents for the first time the osculating, original and future orbital elements of near- parabolic comets that were determined by myself, and in their majority, were further investigated in collaboration with Piotr A. Dybczyński from the Astronomical Observatory Institute at Poznań. In the series of papers, published in the Monthly Notices of the Royal Astronomical Society (years 2010, 2012, 2013; the latter article is reported above) and in Astronomy & Astrophysics (2012), we focused on the problem of the origin of near-parabolic comets with original reciprocal semimajor axes inside so-called Oort spike. When investigating the dynamical orbital evolution of these observed Oort-spike comets to the previous perihelion passage, we showed that the only part of them make their first visit into the planetary zone, i.e. we found that barely 50 per cent of these comets have previous perihelion distance below 15AU. It means that so called Jupiter-Saturn barrier is not as effective as previously thought. The Catalogue presents homogeneous set of osculating orbits of just such comets, the nongravitational (NG) effects were determined for more than 40 per cent of them. The full sample of 119 comets forming this Catalogue constitutes almost 70 per cent of all first class Oort spike comets (condition of -1 1/aori < 0.000150AU was taken with a spare) discovered during the period of 1801–2010, about 90 percent of those discovered in the years 1951–2010, for which observations were finished and completed at the end of 2013. The completeness of all three subsamples of these comets is presented in 60 more details in the paper. NG orbits are derived for 45 comets, including asymmetric NG solution for six of them. Additionally, the new method for cometary orbit quality assessment is applied for all these objects. The resulting catalogue is suitable for the investigation of the origin and the future of near- parabolic comets. This publication is accompanied by an online Catalogue (ssdp.cbk.waw.pl/LPCs; will be publicly available soon) also providing entries to full swarms of original and future virtual comets (VCs, for more details see original paper) that formed the basis for further analysis of dynamical evolution presented in our published papers. Thus, this Catalogue also allows to construct and analyse the observed distribution of Oort spike as well as to investigate the problem of cometary origin by the reader. This publication was submitted to Astronomy and Astrophysics in December 2013.

Fig. 32. Distribution of original 1/a (upper panel, before entering the planetary zone) and future 1/a (lower panel, after leaving the planetary zone) for 119 considered LPCs. The uncertainties of 1/a-determinations were incorporated into these 1/a-histograms by taking the full cloud of VCs for each comet. It means, that both distributions are composed of 119 individual normalized 1/a-distributions resulting from the dynamical calculations of 5001 Vcs (from Królikowska & Dybczyński, MNRAS).

In the following years the Catalogue will be supplemented by comets discovered long time ago as well as updated with newly discovered objects after 2010. In particular, the complete sample of comets discovered during the years 1901–1950 is under consideration as an independent project of the New Catalogue of One-Apparition Comets (authors: M. Królikowska, G. Sitarski, E. M. Pittich, S. Szutowicz, K.Ziołkowski, H. Rickman, R. Gabryszewski, B. Rickman) wherein its first part, that includes 38 comets with original 1/a < 0.000130AU-1 according to Marsden and Williams Catalogue of Cometetary Orbits (2008, 17th Ed.) is currently in preparation. (Małgorzata Królikowska)

A leaky barrier in the Solar System The “Jupiter-Saturn barrier” is a well-known concept for those who study the orbital evolution of long- period comets (see also sections given above on near-parabolic comets). It means that comets coming from the Oort Cloud and passing perihelia in the vicinity of Jupiter’s or Saturn’s orbits or in the range in between are “cleaned away” by the orbital perturbations inflicted by these two giant planets – these comets are either ejected into interstellar space or captured into orbits of shorter periods, from where they eventually get ejected in any case. This barrier has generally been considered to be extremely efficient, so that it would be practically impossible for Oort Cloud comets to reach into observable orbits with small perihelion distances without jumping across the barrier by a major reduction of the perihelion distance. This would reduce the rate of arrival of such comets into the vicinity of Earth’s orbit and has sometimes been interpreted to mean that we are protected by the giant planets from much of the impact hazard that Oort Cloud comets might cause. However, a new investigation of the statistical distribution of the perturbations on Oort Cloud comets caused by the giant planets, published in Icarus (2013), reveals that the risk of being lost by the above- mentioned process is overwhelming only for perihelion distances of about 5 AU or less, i.e., Jupiter- crossing orbits. In the classically considered J-S barrier with perihelion distances from 5 to 15AU, this risk falls rapidly from overwhelming to nearly negligible. This means increased chances for Oort Cloud comets to become observable by diffusing through the barrier and a possibility for the so-called “new comets” to be creepers instead of jumpers in terms of how they approach their observable orbits.

(Hans Rickman, M. Fouchard, Ch. Froeschlé and G.B. Valsecchi)

The “Oort spike” means an outstanding feature in the distribution of orbital energies of long-period comets, whereby these comets pile up close to the parabolic limit. It was the discovery of this spike that led Jan Oort to propose the existence of the distant “cloud” that carries his name. The comets making up the spike are interpreted as newcomers from the cloud, and the rest are returning comets. Previous investigations of how the new comets may be injected had shown that a large fraction should originate in the inner parts of the cloud by a diffusion of orbital energy caused by planetary perturbations – only to finally appear to come from the most distant parts. The most celebrated paper was published in Science by Kaib & Quinn (2009). A comprehensive study of comet injection was recently performed by applying a full model of Oort Cloud comet dynamics to simulate the evolution of clouds made up of four million fictitious comets over 5 billion years, including Galactic tides, passing stars and the action of the giant planets. This confirmed the importance of the Kaib-Quinn mechanism but also stressed the importance of creepers vs jumpers. Planetary perturbations at the preceding perihelion passages were identified as essential for 2/3 of the new comets, and the creepers were found to dominate over the jumpers. Interestingly, the creepers become observable much more easily, if they move on retrograde orbits (thereby reducing the risk of being prematurely ejected by the planets), so the new comets should have a 60/40 preference for retrograde over prograde orbits in apparent conflict with observations. The origin of this conflict may involve un-modeled features in the history of the cloud so that further investigations may lead to new insights. This investigation is described in an Icarus paper (in press, 2013).

(Hans Rickman together with M. Fouchard, Ch. Froeschlé and G.B. Valsecchi)

Long term evolution of the Oort Cloud From the same Monte Carlo simulations, a picture of the history of the cloud was also obtained. The loss of the initial cloud over five billion years was estimated to amount to roughly 25-40% when stellar passages were included but only about 6% when these were excluded. The reason for the losses was identified to be, to a large extent, the closest and most efficient stellar encounters, which impart large enough impulses to the Sun for most of the comets in the outer parts of the Oort Cloud to be ejected and a massive outward migration from the inner core to cause replenishment. This is like a miniature version of the effects proposed earlier to arise from encounters with Giant Molecular Clouds (GMCs). In connection with those dramatic episodes, lots of comets were also found to be injected from the inner parts of the cloud into the outer parts of the planetary system, from where the planetary perturbations would eventually capture them into relatively short-period orbits (semi-major axis less than 1000 AU). These objects are essentially decoupled from the external influences, and they form a source for centaurs and Halley-type comets. The simulations thus showed that the long-term production of such objects from the Oort Cloud has a spiky component in addition to a more stable one associated with the usual Oort spike. This investigation is described in another Icarus paper (in press, 2013).

(Hans Rickman together with M. Fouchard, Ch. Froeschlé and G.B. Valsecchi)

The origin of the Oort Cloud At Uppsala Astronomical Observatory, spectroscopic observations of so-called “solar twins” (i.e., stars that appear very similar to the Sun) had revealed that the old open cluster Messier67 hosts a star which elemental abundances are more sun-like than for any other star, leading to the suspicion that M67 could be the Sun’s birth cluster. A rich and thus long-lasting birth cluster is anyway preferred by isotopic evidence found in meteorites. This called for an investigation of what would happen to the Oort Cloud, if this was formed (as usually thought) in the nascent Solar System in connection with the growth of the giant planets. A King model for the young M67 was constructed and used to derive the encounter frequency of the Sun with other cluster stars as a function of its position within the cluster. An integration scheme was devised in order to calculate the perturbations on Oort Cloud comets inflicted by these passing stars. Thousands of simulations of Oort Clouds initially consisting of thousands of comets were performed in order to cover the time from when the Oort Cloud is considered to have been formed until the time of the Late Heavy Bombardment – i.e., a duration of 400 million years. This work shows that the chance of survival of such a primordial Oort Cloud is essentially zero, if the Sun was formed in M67. A paper is in preparation for Astronomy & Astrophysics. An extension of the work was done by considering the late formation of the Oort Cloud as a consequence of scattered disk formation at the LHB proposed by the Nice Model. Still assuming the Sun to be a M67 member at this time, simulations were carried out with the goal of explaining such Oort Cloud formation by Master students Athanasia Toliou and Georgios Tsirvoulis, with the participation of Ramon Brasser and Alessandro Morbidelli of the Nice Model team and Marc Fouchard of IMCCE, Paris. The results are still being analysed.

(Hans Rickman, Th. Nordlander, B. Gustafsson, A. Korn)

Calculating MOIDs Estimating impact probabilities in the Solar System is often done using standard, analytical formulae that involves certain assumptions as to the distribution of orbits in question. Numerical modelling offers a great advantage that can deal accurately with special cases, where the analytical model breaks down, and it may be tailored to meet the special needs of any particular investigation. In order to perform this task, it is very useful to be able to calculate Minimum Orbit Intersection Distances (MOIDs) quickly and accurately. A numerical tool to do this, based on geometrical arguments rather than analytic theory, has been developed. The principles of the tool, tests and comparisons with the standard method by Giovanni Gronchi were published in Acta Astronomica (2013). Its performance was found to be excellent and in practically all respects superior to anything presented earlier. The computer code and an executable on-line calculation tool has been installed at ssdp.cbk.waw.pl/MOID An example of results, obtained in a few minutes on an ordinary desk computer, is shown in the figure below, which is taken from the paper. This shows the statistics of MOIDs with respect to all asteroids in the IAU Minor Planet Center database for several chosen asteroids. (Tomasz Wiśniowski, Hans Rickman)

Calculating impact probabilities Armed with the MOID calculation tool, two methods to calculate the average impact probability with a target planet for a projectile population with a given type of orbit (in terms of semi-major axis, eccentricity and inclination) were derived. These are numerical and use a Monte Carlo approach. The third type of calculations involves the Hill sphere methods, which are described in the following paragraph. All three methods have been tested and compared with each other as well as with analytical results, found by integrating a classical formula by Wetherill (1967) to obtain the mean impact probability. A paper presenting these efforts and some results in terms of impact probability maps relevant to terrestrial planets and a comet-like population of projectiles is in preparation.

(Hans Rickman, Tomasz Wiśniowski, Paweł Wajer, Ryszard Gabryszewski, G.B. Valsecchi) 64

The Hill Sphere Method of impact probability estimations In this method, the collisional sphere of the real target is replaced by a much larger target (the Hill sphere). Knowing the ratio between areas of Hill sphere and collisional surface, the number of objects entering Hill sphere of the planet, the impact probability is estimated. The poster presents the models and results for the two different approaches. The former uses the unperturbed Keplerian orbit of the projectile, while the second uses the elliptic restricted threebody problem (Sun-target-projectile). By comparing the two methods, we have checked if longtime perturbations have any important influence on the results. The method can be applied to the modelling of small bodies dynamics during and after the LHB. The method was published in the Proceedings of the Meteoroids 2013 Conference which was held in Poznań.

(Paweł Wajer, Ryszard Gabryszewski)

Long term evolution of the Main Belt Comets The knowledge of resonance width in the Main Belt provides an important information that can help understand the dynamics of objects located in this place, especially Main Belt comets. Based on the circular restricted three body problem and the familiar pendulum approximation we calculated width of main MMRs with Jupiter, Saturn, Mars and Earth. The libration width is proportional to square root of the mass of planet, thus, we can see that resonances with Jupiter and Saturn are the most important and we analyze the mean motion resonances with Jupiter and Saturn only. The resonance width was calculated in the following cases: 2:1, 3:1, 3:2, 4:1, 5:2, 5:3 and 7:3 for resonances with Jupiter, and 4:1 and 5:1 for resonances with Saturn. That work allowed us to conclude on ejection mechanisms from the different parts of the Main Belt. Now, the results are statistically analysed. (Ryszard Gabryszewski, Janusz Włodarczyk, Paweł Wajer)

A study on Ganymede's surface topography: Perspectives for radar sounding Radar sounding of Jovian icy satellites has a great potential to address specific science questions such as the presence of subsurface liquid water. Radargrams acquired over Mars polar caps allow to observe clear echoes up to kilometers depth. However, Jovian icy satellites display dramatically different surface topographies. In order to assess possible issues arising from such surface topographies on radar sounding, we performed a study on different DEMs (Digital Elevation Models) obtained on Ganymede. Topographic data is derived using stereo and photoclinometric analysis of Galileo and Voyager images at resolutions of 16–629 m. Main results are presented in this paper. Overall we found that Ganymede's surface is quite rough, with mean slopes at 630 m scale varying from 3.5° to 8°, smoothest terrains being found within sulcii. This will be a major challenge for the design of radar sounders and parameters should be chosen accordingly in order to correctly sound this planetary body. Previous studies have shown similar concern for Europa. (This abstract was taken from the Planetary and Space Science journal.)

(Y. Berquin, Włodek Kofman, A. Henrique, G. Alberti, P. Beck)

RIME: Radar for Icy Moon Exploration Abstract: This paper presents the Radar for Icy Moons Exploration (RIME) instrument, which has been selected as payload for the JUpiter Icy moons Explorer (JUICE) mission. JUICE is one of the 65 most important missions chosen as a part of the ESA's Cosmic Vision 2015–2025, and is aimed to study Jupiter and to investigate the potentially habitable zones in the Galilean icy satellites. RIME is a radar sounder optimized for the penetration of Ganymede, Europa and Callisto up to a depth of 9 km in order to allow the study of the subsurface geology and geophysics of the icy moons and detect possible subsurface water. In this paper we present the main science goals of RIME, the main technical challenges for its development and for its operations as well as the expected scientific returns. This paper was presented at International Geoscience and Remote Sensing Symposium (IGARSS Melbourne 2013; http://www.igarss2013.org/) and is accepted for publication.

(L. Bruzzone, J. J. Plaut, G. Alberti, D. D. Blankenship, F. Bovolo, B. A. Campbell, A. Ferro, Y. Gim, Włodek Kofman, G. Komastu, W. McKinnon)

Analyses of potential analogues for Phobos matter. Analyses of carbonaceous chondrite Mighei (CM2 group) are performed for studying the evidence of its aqueous and thermal alteration, carbon-bearing phases, organic matter, inclusions, and, finally, parent body (Phobos?) identification. A piece of Mighei meteorite was cut in order to prepare a thin section. Polished thin section was used for analyses on polarizing microscope, Raman spectrometer and scanning electron microscope. Preliminary observations using polarizing microscope in reflected light let us identify specific areas within thin section for further investigations. The carbonaceous components of carbonaceous chondrites originally precipitated from a carbon-rich gas then accreted into parent bodies, and then were exposed to aqueous and thermal parent body alteration. A record of those formation and alteration processes is recorded in the chemistry and fine structure of the carbonaceous materials. Raman spectroscopy is sensitive for the carbon structure. Both the inorganic and organic phases can be identified with Raman. This study is focused on distribution of organic compounds in relation to the mineral phases and finding how they are affected by aqueous alteration on the parent body. In total, over 150 spectra of various phases were acquired using a Jobin-Yvon LabRam® spectrometer. Preliminary interpretation of these data shows olivine (forsterite) and pyroxene (diopside) bands. Investigation of water-bearing species in nominally anhydrous minerals can give information on the conditions of phase formation as well as further changes, e.g. provided by aqueous alteration. However, water bands were not found in the studied Raman spectra of olivine and pyroxene crystals; separation of olivine crystals will be necessary for analyses using Fourier transform infrared spectrometer, for obtaining the water content in olivine. Melilite has been found as the component of inclusions. Analyses using scanning electron microscope JEOL 6400F were focused on products’ alteration in chondrules or in matrix surrounding chondrules and allowed to identify specific spots for complementary Raman analyses. (Joanna Gurgurewicz) Modelling of the Martian dust spectra over Hellas area The mineral composition of dust tells us a lot about Martian surface. A minimum of dust in PFS emissivity spectra above Hellas area has two characteristic bands 1075 cm-1 and 1160 cm-1. The modelling of spectra by Deconvolution algorithm method in PFSLook software allows us to obtain results that 80% dust is composed of basalt components – pyroxene and amphibole, an additional 20% are sulfates and clay minerals. In some spectra above the deepest areas of Hellas, the sulfates (in the spectrum) may be even beyond 50%. (Natalia Zalewska)

Evidence of water from LHB on the largest Martian craters The age of the largest craters on Mars suggests that they have been formed during the LHB period (S. Werner 2008). The formation of craters Hellas, Isidis and Argyre happened during that period. Age of Hellas is determined on 3.99±0.01 billion years, Isidis to 3.96±0.01 and Argyre 3.85±0.01 which is already at the end of the Great bombardment. The comparison of the literature of three largest Martian craters: Hellas, Isidis, Argyre was conducted. The layer of clay minerals in each of the craters origins from Noachian age, but in Hellas crater those layers are converted by the glacier and may appear in subsequent ages. Clay minerals are unshakable proof of the existence of water. One can draw conclusions, that large amounts of water appeared at an early Noachian. In subsequent ages, there is no large amounts of these minerals. Formation of Hellas and Isidis craters is associated with the ingress of water on these terrains, in contrast Argyre formed after water left because the impact revealed layers of clay minerals. The analysis was provided within the grant team led by Hans Rickman. (Natalia Zalewska) SLR technique used to description of the earth elasticity

It is the final estimation of the global potential elastic parameters (k2 ,k3 ) derived from the analysis of Satellite Laser Ranging (SLR) data. SLR data for LAGEOS 1 and LAGEOS 2 and for two low satellites, STARLETTE and STELLA, collected over a period of two and half years, from January 1st 2005 to July 1st 2007, from 18 globally distributed ground stations was analysed. Were carry out a A sequential analysis for the all satellites was carried out, and the study of the stability of the estimates as a function of the length and accuracy of the data set used. The adjusted final values for all satellites are compared. Computations were performed using GEODYN II NASA/GSFC software.

9000 LAGEOS 1 8000 LAGEOS 2 7000 6000 5000 4000 3000 2000 1000 number of month 0 0 2 4 6 8 10 12 14 16 18 20 22 24 26 28 30 32

The number of normal points for LAGEOS 1 and LAGEOS 2 used in the solution. The database of normal points was processed in 30-day batches; in total 30 orbital arcs per satellite were used in analyses beginning from 01.01.2005. The horizontal axis gives the numbers of the orbital arcs. number of normal points STELLA 2400.00 2200.00 STARLETTE 2000.00 1800.00 1600.00 1400.00 1200.00 1000.00 800.00 600.00 400.00 200.00 number of arc 0.00 0 10 20 30 40 50 60 70 80 90 100 110 120 130

The number of normal points for STARLETTE and STELLA used in the solution. The database of normal points was processed in 7-day batches; in total 132 orbital arcs per satellite were used in analyses beginning from 01.01.2005. The horizontal axis gives the numbers of the orbital arcs used in solution.

0.30550 k2 0.30500 0.30450 0.30400 LAGEOS1 0.30350 LAGEOS2 0.30300 STELLA STARLETTE 0.30250 0.30200 0.30150 0.30100 0.30050 0.30000 0.29950 0.29900 0.29850 0.29800 0.29750 0.29700 NUMBER OF ARC AND MONTH 0.29650 1 2 3 4 5 6 7 8 9 101112131415161718192021222324252627282930

The sequential solution for the Love number k2 estimated for the analysis based on data for LAGEOS1 (black squares), LAGEOS2 (red squares), STELLA (blue squares) and STARLETTE (green squares). The final value of the Love number is equal to 0.301610.00011 for LAGEOS1, 0.300600.00011 for LAGEOS2, 0.300810.00019 for STELLA and 0.300410.00020 for STARLETTE data for a 2.5 years time interval from January 3, 2005 to July 1, 2007.

0.1610 k3 0.1495 LAGEOS1 0.1380 LAGEOS2 STELLA 0.1265 STARLETTE 0.1150 0.1035 0.0920 0.0805 0.0690 0.0575 0.0460 0.0345 0.0230 0.0115 0.0000 -0.0115 -0.0230 NUMBER OF ARC AND MONTH -0.0345 1 2 3 4 5 6 7 8 9 101112131415161718192021222324252627282930

The sequential solution for the Love number k3 estimated for analysis based on data for LAGEOS1 (black squares), LAGEOS2 (red squares), STELLA (blue squares) and STARLETTE (green squares). The final value of the Love number is equal to 0.09800.0048 for LAGEOS1, 0.08350.0050 for LAGEOS2, 0.08840.0068 for STELLA and 0.08580.0063 for STARLETTE data for a 2.5 years time interval from January 3, 2005 to July 1, 2007. (Mirosława Rutkowska, Marcin Jagoda)

Earth Rotation and Geodynamic Studies

The analysis of the results of the all SLR stations, which performed observations of LAGEOS-1 and LAGEOS-2 satellites in 1983-2012 was finished in 2013. The analysis included results of 74 fixed SLR stations and 63 sites of mobile stations. The station velocities and azimuths were determined for 90 sites for which time span was longer than 3 years. The range biases and RMS of fit independently for both LAGEOS satellites in five years span were determined for each site. The geocentric and topocentric coordinates in reference to ITRF2008 and their standard deviations, velocities and azimuths of all stations were also computed. The most important effect of this work was the estimation of quality of the best SLR stations (Fig. 33). The significant improvement of the results quality in 1983- 1997 was detected, from ±4 cm in 1983 to ±5 mm in 1997. After 1997 the quality of the best SLR stations was on the level ±5 mm with slight deterioration in 2005-2012. The main reasons of this deterioration effect were periodical systematical deviations of some stations, the jumps in the station position caused by changes in the SLR system, and mainly Earthquakes, which caused in the last several years position and velocity changes of the six important SLR stations, the largest for Concepcion (2010) and Koganei (2011). The analysis of the results of Zimmerwald SLR station showed annual dependence between laser light wavelength (423 nm and 846 nm) and station range bias with amplitude 5 mm same for LAGEOS-1 and LAGEOS-2 (Fig. 34). These results are especially important for future improvement of the SLR quality. The last year’s study concerning the determination of Riyadh SLR station position and velocity was extended on the results of the GNSS points on Arabian tectonic plate, which confirmed the results determined from SLR. The all above results were presented at the international conferences (EGU, AGU, IAG, 18th Laser Workshop) and also at the national conferences and meetings.

(Stansław Schillak)

3D RMS 1983 - 2012 50

25 [mm] 20

0 1983 1985 1987 1989 1991 1993 1995 1997 1999 2001 2003 2005 2007 2009 2011

Fig. 33. The accuracy of the best SLR stations in 1983 – 2012.

ZIMMERWALD - 7810 LAGEOS-1 Range Bias Blue - Range Bias Infrared LAGEOS-2 12

0 RB [mm] -2

-4

-6

-8

-10 2005.5 2006.0 2006.5 2007.0 2007.5 2008.0 2008.5

Fig. 34. The differences between Range Biases for blue (423 nm) laser beam and infrared (846 nm) laser beam for two satellites LAGEOS-1 and LAGEOS-2, Zimmerwald SLR station, 2006-2008. The work for comparison of the results of station positions and velocities determined from SLR and GNSS was continued in 2013. The positions and velocities were determined for all co-location of 34 stations, which performed observations by both techniques from 1996.0 to 2013.0. The station position was determined for SLR reference point by including local geodetic tie SLR-GNSS from IERS. It permitted the local geodetic ties verification by comparison with the results of the observations. The differences between the results of both techniques for the most stations in components N, E, U didn’t exceed 10 mm. The agreement of the station velocities were on the level of 1 mm/year. The use of the both techniques permitted the more accurate analysis of the position and velocity changed as the effect of the Earthquakes. These results were presented at the international conferences (EGU, IAG, 18th Laser Workshop) and also at the national conferences and meetings. The possibility of the Borowiec SLR station participation in the laser observations of space debris was estimated. The results of this estimation were shown in the two presentations on the ESA SSA meeting in Borowiec. ESA is interested in participation of the Borowiec SLR station in space debris programme.

(Stanisław Schillak, K. Szafranek)

The sea level anomalies based on AVISO satellite altimetry data were analyzed. The time frequency analysis showed that the annual oscillation in this data is not linear, has a broadband character, and it is mostly responsible for increase of short term prediction errors of sea level anomaly data. It creates oscillations with frequencies being an integer multiplicity of the annual frequency thus, amplitude maxima of all these shorter period oscillations are located almost in geographic regions of the annual oscillation amplitude maxima. The mean prediction errors for 2 weeks in the future of sea level anomaly data computed by the combination of the least-squares and autoregressive methods are usually big in geographic regions of annual oscillation amplitude maxima (Fig. 35).

The common signal in geocenter coordinates observed by the SLR and GNSS techniques was detected using the wavelet based semblance filtering. The most energetic part of this signal is the retrograde annual oscillation in the equatorial plane with amplitude of the order of 2-3 mm.

Fig. 35. The mean prediction error of the sea level anomaly data for 2 weeks in the future (upper map) and the mean amplitude of the annual oscillation (lower map). (Wiesław Kosek)

An attempt to use coefficient of the Earth gravity field to estimate the Chandler wobble parameters, period and damping parameter Q, was made. The input data were x, y geodetic coordinates of the pole and modeled geophysical or gravimetric excitation function. Variations at the annual frequency and its higher harmonics were removed from the observed polar motion. They were also removed from the modeled excitation functions. Observed-geodetic excitation functions are computed with different values for the period (420 – 450,) and Q (10 – 2000). Modeled excitation functions were then removed from the observed-geodetic excitation. The power within the Chandler band of the residual excitation was computed using the Multitaper method. This procedure was repeated until values for the period and Q that minimize the power of the residual excitation were found. In the study we used geophysical excitation functions from the ERA- 40 / ERA -Interim, coefficients of the gravitational field determined from observations of five laser satellites (SLR): LAGEOS laser -1 AND 2, Starlette, Stella Ajisai and coefficients of the gravitational field from Rl05 solution of GRACE mission observations. Estimated values are: sensitive to the length of data and very sensitive to accuracy of modelled excitation. In the case of SLR and GRACE data a motion term must be added. For longest

71 data span, best fit to observations in Chandler band was obtained for geophysical excitation functions (T=430.9 days, Q=127.5) (Nastula, Gross) (Fig. 36).

Fig. 36. Comparison of estimates of the period (top panel) and Q (middle panel) of the Chandler wobble and residual power of excitation (bottom panel).

In 2013, the software, which allows to determine equivalent water thickness (EWT ) from coefficients of expansion of the gravitational was prepared (Nastula, Popiński). The resulting EWT maps were then used to determine gravimetric excitation functions and its analysis. The computed gravimetric excitation functions are divided into contributions of the land hydrosphere over land and from the residual signal remaining over ocean areas after removing atmospheric and oceanic signals. Results show that the residual signal brings non-negligible contribution to the gravimetric excitation functions of polar motion (Nastula, Salstein, Popinski) (Fig. 36).

a) b)

Fig. 37. Equivalent water thickness variance maps computed from GAC (left panel) and from GSM (right panel) dealiasing coefficients from the CSR data. (Variance maps from the other two centers are similar.) Map on the left reflects merged atmospheric (AAM) and oceanic (OAM) mass variability, while that on the right reflects land- hydrosphere-based mass variability (units meters2/grid area).

Gravimetric excitation functions of polar motion were estimated the latest RL05 solution of the GRACE data from three research centers Center for Space Research (CSR), the Jet Propulsion Laboratory (JPL) and the GeoForschungsZentrum (GFZ). These studies included estimations of gravimetric excitation functions of polar motion from the GSM coefficient and comparison of these functions with each other. The next step was to compare the gravimetric excitation functions with hydrological signals in geodetic excitation function of polar motion. It turned out that the gravimetric excitation functions obtained from the latest RL05 from three considered data centers JPL, GFZ, CSR differ significantly, much more than in the case of the previous the RL04 solution. The gravimetric excitation function received from the GFZ data shows a greater degree of smoothing than obtained from the JPL and CSR data. The best agreement between the gravimetric excitation function of polar motion and geodetic residuals, representing hydrological signal is obtained using the of CSR data (Nastula) (Fig.38).The results have been described in manuscripts submitted to the Proceedings IAG2013 and Journées 2013.

Fig. 38. Comparison of gravimetric polar motion excitation functions computed from EWT maps estimated from GSM coefficients from three centers CSR, JPL, GFZ. The GSM-based series reflect hydrological excitation and are separated into contributions all over the globe (top panels), land area (middle panels) and residual ocean area (bottom panels). Trends and seasonal oscillations (annual, semi-annual, 120 days) are removed from the data.

(Jolanta Nastula)

The research work concerning perturbations in Earth rotation caused by the influence of external fluid layers, the atmosphere, the oceans and the land hydrology. Investigations concerning theoretical problems, including the methods of data modeling and interpretation as well as analysis of the available data derived either from space geodetic observations of Earth rotation or from global models of the

73 geophysical fluids. The main part of research was focused on the free oscillations in the equatorial component of rotation, the Chandler wobble (CW) and the free core nutation (FCN). Investigations included stochastic modeling of the free signals enabling determination of their parameters, the period T and the quality factor Q, on the base of available data (see Figure 39). Another part of the study was a search for the excitation mechanism of the observed free motions, by comparing them to the time variation of the angular momentum of the external geophysical fluids.

Fig. 39. Chandler wobble parameters estimation from simultaneous analysis of the polar motion (PM) and atmospheric angular momentum (AAM) data. The mean-squared value of residual excitation is shown as a function of the CW frequency F and quality factor Q (left), and of F and 1/Q (right). Period of analysis: 1948-2010, input data: PM -- Pole~2010 and AAM -- NCEP reanalysis.

(Aleksander Brzeziński)

Regional ionospheric corrections for improvement of position navigation with EGNOS

Continuation of the research conducted in completed PECS project - “EGNOS-EUPOS Integration”. Obtained results open the possibility of creating a regional augmentation system for navigation well- fitted for the boundary areas of the EGNOS system. Based on the original EGNOS corrections and the Internet transmission to users as well as permanent GPS measurements new version of EGNOS correction is prepared. Ionospheric delay is a part of EGNOS correction. The comparative analysis of TEC values obtained from EGNOS and regional permanent GNSS stations showed the systematic shift. The TEC from EGNOS correction is underestimated related to computed regional TEC value (see Fig. 40).

Fig. 40. Median TEC differences between regional and EGNOS data; DTEC>0 in1731 cases, DTEC<0 : 60 cases.

The results of navigation experiment showed that assumptions made at the beginning of the project are correct. The computed ionospheric corrections based on the regional model are more suitable for local conditions than those based on global data. The ‘improved’ EGNOS corrections, used for navigation improve the stability and value of appointed position by about 38% in horizontal position and from 26 to 38% in vertical position (Fig.41). It has to be noticed that errors of appointed positions with original EGNOS corrections drastically increase in Eastern Poland when with ‘improved’ EGNOS corrections only slightly. The results obtained for the EEI project showed a large potential in improvement of EGNOS corrections for regional purposes. The investigations of such kind of changes could result in general changes in EGNOS correction construction.

Fig. 41. Plots presenting the differences of the NMEA position for 'improved' EGNOS corrections (blue dots) and original EGNOS corrections (red dots) from the reference trajectories determined using TBC software. Two top graphs show the number of available satellites and number of satellites used for determining position.

(Leszek Jaworski, Anna Świątek, Łukasz Tomasik)

APPLICATIONS

Heliogeophysical prediction service

Heliogeophysical prediction service of the Space Research Centre, operating within the global ISES system, is responsible for measurements and predictions of solar activity and related Earth phenomena. The International Space Environment Service (ISES) – is an international organisation coordinating quick exchange of data on the Sun, Earth, and Earth's environment parameters between the participating observatories. The Warsaw centre has a special status of the Regional Warning Centre (RWC) (http://rwc.cbk.waw.pl/). Space Research Centre exchanges data with other Warning Centers, a large portion of data is received directly from various national observatories from different countries. Data from Polish observatories is also collected. Data on terrestrial magnetic field activity are supplied by the Central Geophysical Observatory PAS in Belsk, Poland. Solar radio flux at 10 frequencies is supplied by Observatory of Cracow. Both are available on the home page in near-real time as well as the Warsaw and Hornsund ionosonde data. The RWC in cooperation with the Geophysical Institute PAS provides data from polar region (Polish Polar Station Hornsund) – the ionosonde data is completed by riometers and scintillation measurements GISTM. SRC publishes a special daily bulletin URSIGRAM Warsaw on the basis of the continuous flow of data from Poland and abroad, and broadcasts it within the ISES. Methods and algorithms linked directly to the radio-communication prediction and forecast domain are developed and continuously improved. The fully operational real time Vertical Total Electron Content monitoring softwarte has been developed. The data source is selected from GNNS stations and EGNOS RIMS stations. The database was used for the new global expanded version of W-index, and for clonning missing ionospheric values like foF2 or M3000F2. The database can also be used for monitoring traveling ionospheric disturbances (TID), and prediction of TEC variations particularly in EGNOS boundaries.

Fig. 1. Sample VTEC map.

The variability of ionospheric parameters: foF2, hmF2, M3000F2, B0, B1 for middle latitude over Warsaw were analysed. For this study Warsaw ionosonde measurements since January 2009 to the end of 2012 were used. Specific term enabled to analyse ionospheric parameters in different conditions of solar activity. Selected data was modelled by International Reference Ionosphere IRI 2012 model. 76

Analysis contained: trend, month median differences in twenty-four-hour variability, local minimums and maximums of specified parameters and IRI submodels. The results of the study will enable to use the IRI submodels to prepare more accurate local and global ionospheric maps in the event of lack of parameters, and the more effective forecasts and predictions of ionospheric conditions.

Fig. 2. 2009 – 2012 comparison of foF2 months medians difference variation for Warsaw ionosonde and IRI 2012 URSI model, with specified solar 10.7 cm flux level.

Fig. 3. 2009 – 2012 comparison of hmF2 months medians difference variation for Warsaw ionosonde and IRI 2012 URSI model, with specified solar 10.7 cm flux level.

The new ionosonde has been developed for use in propagation research and associated studies of the ionosphere. The ionosonde is known as VISRC2D and will be installed in OPN-T in Olsztyn. It is a twin unit of Warsaw ionosonde so the GPS time synchronised shot allows to proceed oblique sounding.

Fig. 4. VISRC2D ionosonde – developer version.

Fig. 5. Antenna for VISRC2D ionosonde. The new ionosonde has been developed for use in propagation research and associated studies of the ionosphere. The ionosonde is known as VISRC2D and will be installed in OPN-T in Olsztyn. It is a twin unit of Warsaw ionosonde so the GPS time synchronised shot allows to proceed oblique sounding. The ionosonde works with standard two delta antennas 18 meters high. Due to a short distance between Olsztyn and Warsaw and designed propagation pattern the oblique sounding does not require additional antennas set. The impact of various space weather phenomena is studied. The forecast of sporadic E layer occurring locally and sometimes nontransparent is the crucial topic for radiocommunication. We propose the method of forecasting sporadic E layer appearance. This method is based on magnetic data and the changes of magnetic Eta parameter defined as the square root of a ratio of the energy of the external part of the vertical component to that of the horizontal components. The best correlation of sporadic E layer appearance occurs 1-2 hours after the increase of Eta value. The correlation between data from different European ionosondes and data from magnetic observatories lying close to the selected ionosonde was taken into account. We apply autocovariance method for prediction of the Eta index variations and in this connection the sporadic E layer appearance.

Fig. 6. Examples of ionograms when sporadic E layer appears. First ionograms illustrates the situation when eta index has maximal value and the second ionogram shows the formed blanketing sporadic E layer 1 h after the maximum of eta index.

Fig. 7. Correlation of the magnetic eta index with the critical frequency of the sporadic E layer, the best correlation appears 2 hours after the maximum value of eta.

The RWC/IDCE (The Ionospheric Despatch Centre in Europe) web service (http://rwc.cbk. waw.pl/idce) provides an on line access to data base of the critical frequency of F2 ionospheric layer forecast for all available sites. Continuous now-casting of regional ionospheric conditions over Europe, East Asia and Australia area is presented. Space Research Centre provides forecast service for the governmental and commercial communications HF radio signal intensity. The work is carried out using software packages HELGEO and Ray-Route (six-generation version) developed at SRC. The HELGEO is an automatic system of solar-geophysical data processing for analysis and forecast of solar-geophysical phenomena and the Ray-Route is a system of forecasting of HF communications conditions, including signal to noise ratio at recommended frequencies. It organises proper data base for operational data-driven models and runs the subroutines based on such models creating at the end a set of messages and files addressed to different users requirements.

Fig. 8. New features of the latest version of Ray-Route software: automation of operator tasks and the ability of radio propagation calculating for aviation.

In connection with the 24th solar maximum our laboratory reacts on every public need for clarification of extreme events. We respond to questions from reporters and write announcements on social networking of our Institute.

(Iwona Stanisławska, Beata Dziak-Jankowska, Łukasz Tomasik, Mariusz Pożoga, Michał Szwabowski, Maria Miłodrowska)

EARTH OBSERVATIONS

Earth Observation Group at Space Research Centre (ZOZ CBK PAN) specializes in remote sensing and geographic information systems (GIS). The Group is active in the 7th Framework Programme projects, pre-accession ESA programme PECS as well as in domestic research programmes. In 2013 ZOZ CBK PAN participated in several projects: B-First, G-NEXT, G-SEXTANT, EOPOWER, Multifractal Analysis of Satellite Images, SCARF, ArtISS, Globe. Since Poland has become an ESA member state in 2012 ZOZ CBK PAN succeeded in 2013 in applying for two ESA grants which start in 2014. Earth Observation Group handles developing innovative applications, software and algorithms as well.

B-First - Implementation of remote sensing data and models in optimizing the localization of renewable energy crops with respect to ecological constrains

The main goal of the project is to prepare the geoinformation system to support decision for biofuel crop localization. The project is implemented jointly by the three research teams: CBK PAN (leader), Astri Polska and Institute of Soil Science and Plant Cultivation (IUNG) Puławy. The project proceeds according to the schedule. ZOZ CBK PAN is responsible for processing of optical data: SPOT 5 and radar data: RADARSAT, TerraSAR-X. In 2013 the first classification of the SPOT5 satellite images was extended with regard to the research requirements for the project.

The legend of the classification map was enriched by new classes. Using the Corine Land Cover map it was possible to add class grassland to the final map. Extraction of this class is impossible when using only one image acquisition. Comparing to the first version of the classification map, class urban was refined. First of all miss-classifications of bare agricultural areas were filtered. Additionally, to fit into project needs, areas with the highest density of buildings were extracted from the built-up class. Drainage channels were added to class water. They were extracted from the hydrological map as it is not possible to derive them from the satellite image. This is due to the 10 m resolution of the SPOT5 image. It is expected that using finer resolution (i.e. 1 m) would allow extracting most of the drainage channels. Because the essential part of the classification procedure constitutes of verification and validation a set of randomly selected points was generated. An experienced user evaluated class membership for these points.

Fig. 9. Example of automatic land cover classification. Left image: first version, right image: second version with expanded legend and improved accuracy.

Radar classification - fully-polarimetric image - has been introduced to obtain the description of the scatter mechanism from different types of surfaces which is the base of this classification.

(Sebastian Aleksandrowicz, Edyta Woźniak, Stanisław Lewiński, Ewa Bilska)

EOPOWER - Earth Observation for Economic Empowerment

The aim of the project is to create conditions for sustainable economic development through the increased use of Earth observation products and services for environmental applications. CBK PAN is responsible for Work Package 8 “Empowering economic development Poland and Ukraine” so its’ share is focused on: building capacity of EO on individual and institutional level, promoting the increase use of EO products and services for environmental and related applications, upgrading the portfolio of EO applications for economic development and environmental management in Poland and Ukraine, integrating the EO community in Poland and Ukraine and creating an integrated source

81 of information about EO resources, capacity building opportunities and for exchange of experiences for stakeholders, as well as promoting participation of Poland in GEO and GEOSS. There were several activities to promote the increase use of EO products and services for environmental applications: Scientific festival in Warsaw 15.06.2013, IV Space Conference in Sieradz 08-09.10.2013, meeting with Governor of Mazovia 31.10.2013. There was a Polish-Ukrainian seminar organized on 5-6 of September 2013 in Warsaw by CBK PAN. The representatives of scientific and educational institutions and NGOs from Poland and Ukraine participated, i.e. Scientific Centre for Aerospace Research of the Earth National Academy of Sciences of Ukraine, National University of Life and Environmental Sciences of Ukraine, ULRMC - Ukrainian Land and Resource Management Centre, Military University of Technology, Environmental Information Centre UNEP/GRID-Warsaw, Institute of Technology and Science, Warsaw University of Technology. Its’ aim was to find and establish the fields of research and educational cooperation between parties: to get familiar with areas of research activity of each institution and to identify and discuss potential possibilities for future collaboration. The discussion has showed that there are few interesting ideas for scientific and educational Polish – Ukrainian activities. The idea of webinars in EO field, where Polish and Ukrainain educational and research institutions are involved is a significant outcome of the seminar. The technical capabilities for webinar have already positively passed the test during GIS Day in November 20th when the webinar on remote sensing, presented by ZOZ CBK PAN researcher from his office in Warsaw to students from Wrocław University of Technology, came out as a success. The Polish – Ukrainian webinar agenda for 2014 is being built.

Fig. 10. Polish – Ukrainian seminar participants.

(Ewa Bilska, Aleksandra Grzegorczyk, Stanisław Lewiński)

G-NEXT - GMES pre-operational security services for supporting external actions

According to the potential application areas identified under SEA (GMES Security working group in Support to External Actions), and the experience gained by the proposal consortium in Security and Emergency precursor projects (LIMES, G-MOSAIC, SAFER) this project is aimed at identifying and exploiting a set of Services able to provide reliable support to the EU External Action service and suitable to be integrated in the user working environment in an effective and reliable way. The research and development focus is on the enhancement of Crisis Management Response Services in rush and non-rush mode and in covering the relevant gaps identified in the perspective of a (pre-)operational approach. Reference Users for the service/products include the main actors and stakeholders involved in the context of EU Missions and Operations in support of the External Actions: European Union – EEAS (European External Action Service), EDA (European Defence Agency), National Institutions such as Ministries of Foreign Affairs and Ministries of Defence, Police Offices, Intelligence Centres, and also international institutions as UN bodies. The project aims at: 1) Demonstrating the effective contribution of an integrated geo-spatial service concept that can respond to the needs in SEA user-driven scenarios providing the User Community with an evolving set of security service/products. 2) Involving the main User organization in the Copernicus (GMES) Security domain in the use of the provided services. 3) Assuring the continuity of the work done in previous GMES projects specifically on security and emergency domains. 4) Implementing synergies with the other Copernicus (GMES) projects and initiatives (e.g. EU, ESA, EDA contexts) running in parallel with the project lifecycle. 5) Performing a comprehensive benefits’ analysis taking into account the main drivers for the set up of an operational framework. 6) Addressing the potential service evolution in 2014 onwards perspective.

CBK PAN is responsible for WP 320 Quality Check, which objective is the definition of the general principles of the service quality check activities to ensure the best deliverables quality, resulting in a quality check system establishment. The quality check covers issues like: monitoring processing chains, testing the final products, etc. CBK PAN shares participation in WP 610 as well. Gnocco - an online quality check protocol is CBK PAN contribution to the project output.

Fig. 11. GNOCCO - Interface of quality check protocol.

(Małgorzata Jenerowicz, Adam Włodarkiewicz, Ewa Bilska)

G-SEXTANT - Service Provision of Geospatial Intelligence in EU External Actions Support

The goal of the Project is to consolidate a portfolio of Earth Observation products and services that support the geospatial information (geo-information) needs of the EU External Actions. The exploration of the Security dimension of Copernicus (GMES), the definition of services and products to respond to the users’ demands, and the implementation of appropriate governance will be consolidated in G-SEXTANT from the lessons learned from previous projects. Focusing on the gaps identified in previous security projects, the major objectives of the G-SEXTANT are:

1) preparation and delivery of pre-operational services in user-driven support to external actions (SEA) scenarios; 2) further enhancement of already mature products and services demanded by the users; 3) reaching a standardized portfolio. Demonstrations will be conducted in different scenarios to cover the potential application areas of interest identified by the SEA working group and mentioned in the Call: humanitarian crisis, natural resources, land conflict situation awareness, nuclear activities, monitoring of illicit crops and border monitoring outside the EU. The G-SEXTANT production has been organized to exploit the experience and skills of the different stakeholders involved: industry (production and implementation capacity), institutional organizations (experience in R&D activities) and EU organizations (consistency with EU policy and operations and access to intelligence data). Involvement of users in validation activities will ensure the achievement of appropriate products and services and provide the exact measurement of the impact of G-SEXTANT in the security users’ community. CBK PAN is responsible for WP 620 Verification and validation coordination, and shares participation in WP 630, WP 720 Policy framework analysis, aimed at highlighting the relevance of G-SEXTANT for the EU external action (focus on SEA), by analysing the policies impacting and driving the project.

(Małgorzata Jenerowicz, Sebastian Aleksandrowicz, Ewa Bilska)

Satellite image classification using boosting A novel land cover classification method based on boosting has been developed for the purposes of binary classification. Boosting has been proven useful in image processing while it is still new to satellite remote sensing. It is a meta-algorithm, which builds a strong classifier from many weak ones. Our adaptation of boosting the remote sensing classification includes construction of a set of weak classifiers, selecting feature space and adaptation of Adaboost.M1 boosting algorithm. Its performance was investigated in the exemplary case of artificial area classification for IKONOS multispectral imagery. Obtained classification accuracy on independent validation set reached over 94%, what is a very good results taking into consideration that distinguishing between artificial and not artificial land cover is a difficult problem due to the spectral diversity of the classes. These results not only prove the performance of the method, but also give us new opportunities to apply boosting for other classification problems in remote sensing.

Fig. 12. Exemplary classification results: original image and result of classification of artificial area.

(Artur Nowakowski)

Multifractal Analysis of Satellite Images

In our research we have considered (multi-)fractal parameters in the context of the remote sensing applications. In particular, based on the analysis of large datasets of images we demonstrated the correlation between the degree of multifractality and the main forms of land cover. We have also compared the fractal dimension and the degree of multifractality of hundreds of Very High Resolutions satellite images with the most common texture measures in context of image classification. We have proved that the degree of multifractality used together with histogram-based parameters may be the most effective image content descriptor. In the second part of our analysis we have focused on the verification if the image filtration prior to the calculation of fractal and multifractal parameters may improve their efficiency as image content descriptors. In order to evaluate the effectiveness of the coupling of fractal and multifractal features

86 with the image filtration we have analysed the class separability measures and the classification accuracy. Our study results indicate that the degree of multifractality improves the classification accuracy in comparison to the fractal dimension, especially after Sigma filtration.

Fig. 13. General concept of multifractal image.

(Michał Krupiński, Anna Wawrzaszek)

SCARF - Satellite Cloud Climatology over Poland with Atmospheric Radiation Fluxes Estimation

Clouds play an important role in the Earth’s radiation budget. Due to the high albedo the shortwave radiation is being reflected by a clouds’ tops, what results in the negative radiative forcing. On the other hand the absorption of the Earth’s longwave radiation by clouds generates the cloud greenhouse effect and positive forcing. All existing studies dealing with cloud amount over Poland were performed with the traditional, manual, surface-based visual observations. This kind of observation is heavily burden with observer’s subjectivity and does not allow for studying the radiative properties of clouds. Since 80s of the last century, a satellite-based observations are considered as an alternative for traditional cloud cover observations. SCARF project develops the first high-resolution (1 km/pixel) cloud climatology over Poland with application of MODIS (Moderate-resolution Imaging Spectroradiometer) remotely sensed data. Mean monthly statistics of Cloud Amount, Cloud Optical Thickness, Cloud Top Pressure and Cloud Water Path are calculated for each month between 2003 and 2013. The mountains are of great interest. Previously not investigated with surface-based observations or investigated with significant limitations.

Fig. 14. Mean monthly daytime cloud amount over Poland Fig. 15. Mean monthly cloud amount over Tatra Mts., in in June 2003. July 2004.

(Andrzej Kotarba)

ArtISS - Artificial Impervious Surfaces detection with Snow-featured satellite imagery

Typically the land remote sensing operators interpret snow cover as a highly undesirable element, which prevents from observation of a „proper” land cover. However, the presence of snow increases the spectral contrast between artificial surfaces and other land cover classes. As a consequence, the spectral characteristics of artificial surfaces are far more distinguishable during winter-time, than during summer-time, when signatures overlap. This is especially important when discontinuous urban fabric surface is considered – typically classified with only 40-60% accuracy. The main goal of ArtISS project is to improve detection accuracy of artificial (impervious) surfaces with an application of winter-time, snow-featured satellite imagery.

Fig. 16. Snow-free (left; May 7, 2002) and snow-featured (right; November 11, 1999) Landsat ETM+ image at 0.63 - 0.69 µm (original resolution 30 m/pixel). Spectral contrast between artificial impervious surface and background is enhanced due to snow presence. (Andrzej Kotarba)

GLOBE - Explore climate with the GLOBE Explore climate with the GLOBE Program, led by Environmental Information Centre GRID-Warsaw, is the part of international Student Climate Research Campaign (SCRC). The program prepares a Satellite Lesson of Climate module dedicated to the development of the lesson scenarios, which will help educators to teach students at different level of education. Lessons will be dedicated to climate issues and satellite data are foreseen as the most significant source of the environmental information. CBK PAN is responsible for scientific part of the module – satellite remote sensing and climatology. ( Andrzej Kotarba)

Retrieval of atmospheric parameters from infrared spectra This study was dedicated to the retrieval of vertical temperature profiles in the Venus atmosphere. The goal was to create software in order to obtain single temperature profile. The venusian atmosphere is composed mainly of CO2 thanks to it, it is possible to find the thermal structure from 50 km to around 100 km. Below 50 km the thick layer of clouds occur and this prevents acquiring the information about

89 temperatures below this altitude. Clouds on Venus are mainly composed of H2SO4 which have significant scattering properties (single scattering albedo > 0.5). The retrieval of venusian atmospheric temperature is based on the another absorption band by CO2 at 4.3 micron. VIRTIS-M instrument measures radiation emerging from the atmosphere between 1 – 5 micron. In order to model the measured spectra by VIRTIS, the multiple scattering in the atmosphere is taken into account because of cloudy atmosphere and its optical properties. For this purpose we use the inversion method for radiative transfer equation based on the Bayesian formalism. The theorem applies the probability density functions to define a function of the state vector or the measurement vector. The fit of spectral calculated and measured radiances is presented in Fig.17. For this fit we obtain a temperature profile (dark blue line) (Fig.18) which is very close to the true temperature profile (red line). The vertical scale of retrieval extends from 700 mb to 0.1 mb which corresponds to around 52 km up to 95 km. Fig.19 presents atmospheric temperatures at around 70 km averaged zonally in a function of local time and latitude [Grassi et al., 2013].

Fig. 17. The fit of spectral calculated and measured. Fig. 18. Retrieved temperature profile radiances.

Fig. 19. Atmospheric temperatures at 34 mb (~70 km) versus LT and latitudes.

(Paulina Wolkenberg, Marek Banaszkiewicz)

Simulation of SAR images. The objective of the investigation is to create synthetic aperture radar (SAR) reflectivity maps of residential areas based on ray tracing method. In this method, each ”ray” is followed from the SAR sensor to the scene, scattered from the objects presented in this scene, and finally, backscattered to the

90 radar sensor. Residential areas are characterized by complex radar backscattering signal due to a wide variety of building structures interaction between different buildings in the scene, and different kinds of the surroundings of the buildings as paved streets, lawns and bushes. It implies existence of different scattering mechanisms (surface scattering, multiple reflections, volume scattering) in these types of areas. Simulation of scattering effects and SAR images for urban areas can support interpretation of SAR observations, layover effects, single and multiple bouncing appearing in urban scenes.

Fig. 20. Schematic illustration of the ray tracing algorithm.

Fig. 21. (a) Image of the gable-roof building. (b) Model 3D of this building. (c) SAR image of the building. (d) Simulated SAR image of the building (The speckle effect is not simulated). Figures (a), (b) and (c) are taken from Brunner, D.; Lemoine, G.; Greidanus, H.; Bruzzone, L., "Radar Imaging Simulation for Urban Structures," Geoscience and Remote Sensing Letters, IEEE , vol.8, no.1, pp.68,72, Jan. 2011. Figure (d) shows our simulation results.

(Paweł Wajer, Włodek Kofman)

Land cover classification based on scatter mechanism obtained from SAR data - radar polarimetry

In our work we analyzed the window size used in polarimetric image analysis’ impact on the image classification. We also check how the classification results are sensible to threshold accuracy. To fulfill

91 these goals we used the ALOS fully polarimetric image and after the pre-processing procedure (speckle removing, orthorectification) we decomposed the image using following methods: three-component Freeman-Durden and Van Zyl models, four-component Yamaguchi model and H/A/Alpha theorem. The decomposition was applied using 3 window sizes; 3x3, 5x5 and 7x7 pixels. The obtained decomposition parameters were used as the input data for the classification. The classification was done in two steps. In the first step we divided the terrain into two classes which represent two kind of surfaces: smooth and rough ones. Then the classes were subdivided into more specific classes: smooth areas -into water and agriculture, rough ones into forest and urban. The separation between smooth and rough areas can be done using volume scattering parameters and this is obtained with the accuracy higher than 95%. The differences in accuracy among different window size were insignificant – around 0,05%. The changes in threshold values (+/- 10% or +/- 20%) caused the changes in classification accurateness of about 1%-5%. For the more detailed areas, urban – forest and agriculture – water, we separated them the parameters, anisotropy and entropy, from H/A/Alpha theorem. The changes in the classification accuracy as a function of window size reached 2%. However the sensibility for the threshold value changes varies from 2% in the case of separation between forest and urban areas to 32%-61% in the case of agriculture and water areas. So to classify the agriculture and water the threshold must be calculated very precisely. Also it was pointed out the necessity to use different window size in different step of the classification. The maximum accuracy obtained was 86,43%. The obtained results permit to conclude that window size of the decomposition is not as important as the precision of the threshold value.

Fig. 22. Polarimetric decompositions (RGB) and land cover classification.

(Edyta Woźniak, Włodek Kofman, Stanisław Lewiński )

SOFTWARE & APPLICATIONS Several software development projects have been conducted in Earth Observation Group by its Programming Team. Many of them involve research and implementation of novel methods. Development efforts’ result in applications for satellite data analysis: segmentation, land cover classification, environmental indicators calculation and riparian zones localization. The web services were also developed for daily monitoring of land surface of Poland and for monitoring of water level in rivers of South Sudan. For data from hyper-spectral scanner designed and built in CBK PAN a software for two purposes have been prepared: simulations of influence of aircraft vibration on shifts of scanned hyperspectral data lines and creating image from shifted scanned lines. Additionally, software for license plate locatization and recognition was improved.

BooSIM - an application for land cover classification A novel land cover classification method based on boosting has been developed and tested for the purposes of binary classification. Real data tests and evaluations of the method result in high accuracy and reliability. Based on the method an independent standalone application has been built for land cover classification. It was designed to be user-friendly and it can operate with many popular data formats. This unique solution among software devoted to remote sensing data creates wide opportunities of applications to classification problems. (Artur Nowakowski)

Open Foris - collaboration with UN-FAO Since September 2013, the Earth Observation Group collaborates with the Food and Agriculture Organisation of the UN under the Programme FAO-FIN hosted by the Department of Forestry. The main area of collaboration is the creation of free software package for satellite data processing [(http://www.openforis.org/OFwiki/index.php/Open_Foris_Geospatial_Toolkit)], aimed primarily at developing countries which act actively to limit deforestation within their territories. The role of our group is to create and to implement an image segmentation algorithm. Segmentation is a key component of the processing the satellite imagery which subsequently is converted to vector maps and databases. The quality of segmentation determines time efficiency, quality and cost of the analysis of forest cover change.

Fig. 23. The first information about our input into Open Foris software.

(Przemysław Żelazowski, Artur Nowakowski, Krzysztof Stopa)

Web Services for flood early-warning system in Northern Bahr El-Ghazal in South Sudan The project has been developed in the scope of the Crisis Information Centre (ZOZ CBK PAN depended group) at CBK and founded by Polish development cooperation programme 2013 of the Ministry of Foreign Affairs of the Republic of Poland. Its principal aim is to construct and install a gird of water gauges that collects data about the water flow that enables to warn the local population early enough in case of flood. At the Earth Observation Group we have created a set of web services that collect data sent by the water gauges through satellite internet and stores it to a database. Then, this data can be analysed and used to monitor the level of the water and send alarms to the local authorities if is needed. Additionally a web portal has been developed where historical and current data can be visualized for each of the installed sensors.

Fig. 24. Web page for flood early-warning system in Northern Bahr El-Ghazal in South Sudan.

(Krzysztof Stopa) 94

IncSIM & IncSIM Batch Tool

IncSIM is a multithreading batch processing tool to enable processing of multiple image files and calculating multiple indicators at once - an application for calculation of landscape metrics over data sets with classification information. During 2013 the application has been considerably improved by adding new landscape metrics beating 50 available, and including new supported raster and vector file formats including GeoTIFF, Shapefiles and KML files. Thereby the application is a complete solution that can be used to produce professional results and can be applied in any landscape ecology study. There were new landscape metrics added in 2013: mean patch size, patch size standard deviation, patch size coefficient of variation, largest patch index, degree of coherence, degree of division, splitting index, effective mesh size, splitting density, net product, total landscape area, modified Simpson Diversity Index, shannon's evenness index, Simpson's evenness index, modified Simpson's evenness index, mean Nearest-Neighbour Distance, Nearest-Neighbour Standard Deviation, nearest-Neighbour Coefficient of Variation, mean Proximity Index, Class Area.

Fig. 25. Interface of IncSIM Batch Tool. (Krzysztof Stopa) Daily land surface monitoring The Earth Observation Group designed and launched a web service for daily land surface monitoring based on MODIS satellite images. The basic assumption was to create a system running fully automatically without the need of user interaction. The satellite data is transmitted from satellite to the ground receiving station and after pre-processing data sets are available via the Internet. A software procedure checks whether there is new data which is suitable for the system. The area of interest (the whole territory of the Poland) is determined automatically and downloaded to CBK PAN where further processing is also automatic. Subsets of the data are stored and then they are used to create products. In the first stage of system expansion vegetation indices are calculated (NDVI, NDII, EVI, VARI). The functionality of the system is expanded and in the near future, we plan to serve brightness temperatures (BT), cloud mask, water vapor content and land surface temperature. Also more complex algorithms

95 like Forest Fire Hazard Index will be applied. All calculated data is stored, and maps of their distribution are automatically published on geo-portal - examples are in figure. The monitoring system has been working since the beginning of 2013. Designed functions are checked and systematically improved and new functionalities of geo-portal are introduced. The monitoring system performs two basic functions: on-line monitoring of the Earth surface parameters and collecting data for future statistical analysis. Created data base will allow to compare actual data to typical conditions for making forecasts and also detecting natural hazards.

Fig. 26. A scheme of daily land surface monitoring.

Fig. 27. Examples of automatically generated maps for day 22.04.2013: EVI, VARI indices, land surface temperature.

(Stanisław Lewiński, Edyta Woźniak, Adam Włodarkiewicz, Krzysztof Stopa)

Crisis Information Centre

In September 2013 the Crisis Information Centre of SRC (CIC), which previously existed as an ad hoc operational structure, has been transformed into an operational unit of SRC with permanent employees. Throughout the year CIC has been involved in planning and requirements’ definition of the GECCO system, which will combine: analytical competence of providing crisis management and capabilities of rescue organizations with satellite-derived analysis; an IT platform to share geospatial data; and solutions to inform the public about potential hazards. In April CIC participated in the large- scale international urban search and rescue field training in Żagań, Poland. CIC prepared and coordinated demonstration of the use of Unmanned Aerial Vehicles to support coordination of such operations. Different UAVs were successfully used to provide reconnaissance information, working directly within the command structure of both national and UN headquarters.

As part of an operational support for Polish authorities, CIC conducted four activations in 2013. In February, immediately after receiving information about meteoroid explosion over Czelabinsk, CIC was requested to advise the Minister of Internal Affairs and his public affairs office about potential risks. CIC coordinated information flow about a possible relation between that event and the forecasted close pass of Duende asteroid 16 hours later. Since August till October CIC monitored a flood situation in northern provinces of Southern Sudan. As a part of the activity of the Polish Centre for International Aid (PCPM) and the Ministry of Foreign Affairs, CIC published 13 products presenting extent of flood, of which 9 were incorporated into information mechanisms of UN agencies and international NGOs operating in the region. In addition CIC responded to direct requests for information and analysis from Southern Sudan government. In November CIC provided advisory service for Polish crisis management authorities during re-entry of the GOCE satellite. In late December, responding to the request from the National Centre for Rescue Coordination after heavy winds in Tatry mountains, CIC and the Novelty company conducted experimental mapping with UAV and analysis of damage around Zakopane.

Fig. 28. UAV image used as an update for satellite map Fig. 29. Example of reconnaissance image of destroyed (provided in the command centre by Astri Polska). building acquired by UAV during the field training.

Fig. 30. Map of flood extent in Southern Sudan.

Fig. 31. Analysis of forest destruction in Tatry mountains after heavy winds, based on UAV-derived map.

(Jakub Ryzenko) SPEKTROP

The main goal of the project is the development of the family of the spectro-imaging systems for remote sensing needs. The systems should work in spectral range from 0,4 –to 20µm. The systems are designed for different specific condition of measurements. Measurements can be done from space, airborne, and from ground mobile platforms. Every platform has different technical requirements and different types of systems are developed for them. The systems are equipped in anti-vibration and stabilization modules. The systems consist of TMA (Three Mirror Anastigmat) telescopes cooperating with CCD detectors matrix (type of matrix depends on application), front–end electronic module, controlling unit with data collecting and processing module. In 2013, in the frame of the project we focused on testing the system at the small plane SONEX. We introduced improvements in the electrical and mechanical modules according to the achieved results. The flight tests have been carried out since the end of June till the mid of October. The final tests showed that the prototype of the hyperspectral spectrometer achieved required parameters and the stabilization system require redesign. Below the iphot of the prototype placed in the plane and row image taken from the system without any processing are presented.

Fig. 32. Prototype during test. Fig. 33. Row image.

(Mirosław Rataj) 98

DATA EXPLORATION AND DISSEMINATION

EXPLOITATION OF SPACE SCIENCE AND EXPLORATION DATA

THE POP-DAT FP7 PROJECT: Problem-oriented Data Processing and Database Creation for Ionosphere Exploration. 1

Earth's ionosphere plays a very important role in the solar-terrestrial processes. Its dynamics, that is an important element of the Space Weather, is strongly influenced by solar activity. The actual state of the ionosphere is described by a set of various parameters, and it's nowcasting and forecasting is rather complex. The exact monitoring of those parameters needs both of the sophisticated data analysis and the utilization of measurements performed by the different missions. In that context POPDAT project was aimed at developing and deploying new methods of processing and representation of the ionosphere data received from the series of the completed ionospheric satellite missions. The output of the project is the Ionosphere Waves Service that makes third level data available for great number of scientists. We believe that with its approach POPDAT will help to enhance our understanding of the rich physical processes taking place in Earth's surroundings.

Introduction

POP-DAT was a collaborative project under FP7 Framework Programme that has started on the 1st June of 2011 and successfully ended on the 31st of May 2013. The project is an attempt to answer several questions: How can the reprocessed data of earlier ionospheric missions provide more profitable results? How could the scientific community be provided with a new insight on wave processes that take place in the ionosphere? The answer is a unique data mining service, that allows for accessing a collection of topical catalogues that characterize a huge number of Whistler-like Electromagnetic Wave Phenomena, Atmosphere Gravity Waves and Travelling Ionosphere Disturbances. Based on the detailed catalogue of ionospheric wave phenomena the Ionosphere Waves Service regroups databases of specific events extracted by specific software systems from data records of the selected satellite missions, which the end user can access by making specific search queries and use statistical modules in their domain of interest.

Objectives

 Collection of datasets from different sources which concern the wave-like phenomena in the upper atmosphere and ionosphere to form an input data field for further processing

1 http://popdat.org 99

(Atmosphere Explorer-E/AE-E, DEMETER, VARIANT, DYNAMIC EXPLORER 2/DE, GPS, etc.).  Appropriate design of the flexible software tools for the search of wavelike and/or any other anomalous behaviours detected in the satellite datasets, that have known, supposed or unknown origin.  Implementation of Ionosphere Waves Service (IWS) accessible to scientific communities and public users. The service is now hosted by SRC PAS and available at: http://popdat.cbk.waw.pl/  Creation of thematic catalogues of ionosphere perturbations, that have known, supposed or unknown origin.  Dissemination and promotion of the Ionosphere Waves Service at topical conferences and in scientific and public press.

IWS concept IWS concept is based on the relational database. The search is performed against metadata, which enables service to perform an efficient search through millions of records. It requires the contributor to submit to the system third level (processed data) in NetCDF format with the metadata prepared in the XML format. On the other side the End User is be able to:  perform the search for events according to certain criteria i.e.:geographical coordinates, magnetic coordinates, time (UT), event name, contributor name, and many others;  perform the visualisation and/or extraction of data containing those events.

Event types incorporated to the service (examples) From the data taken into account for the project purposes two main classes of wave processes were identified: electromagnetic waves and atmospheric waves. In the first group 14 classes are known: 7 are different types of whistler-like propagating signals, 2 other classes are directly connected to whistlers. Other types have noise-like character (triggered emission, signals recorded over seismic regions). Figure 1 (first from left) presents an example of the ducted whistler measured on board of Compass-2 satellite. In the group of atmospheric waves three classes were identified: atmospheric gravity waves (AGWs) and two types of travelling ionosphere disturbances (TIDs). Figure 1 (middle) is an example of AGW recordings and Figure 1 (right) presents medium scale TID induced by atmospheric acoustic waves generated by seismic surface waves.

Fig. 1. Event types incorporated to IWS.

100

Output and capabilities IWS interface resembles desktop environment. User can open many windows and perform different actions such as running search, viewing submission log etc. Figure 2 (left). User can perform a search using various criteria: geographic coordinates (can be marked on the map (Figure 2 (left)) or set using numerical values), geomagnetic location, event ID, catalogue ID, time range or contributor name, and many others (Figure 2 (right)). The search term can be saved on the users disk and uploaded later on. The search term can be made as combination of different criteria.

Fig. 2. Interface mock-up of the Ionosphere Waves Service.

Data can be visualised with quicklook: Figure 3 (left). User can display the location of the event found on the map. It is also possible to make a~histogram of occurrences of certain value (Figure 3 (right)). The analysis can be run for all found files or for selected number of files. The NetCDF file can be downloaded to the users disk. In case when system returns no files it also gives an information why performed search was unsuccessful. There are two possibilities:  there are no files that fulfil the search terms, or  there are files that fulfil the search terms, but the searched event was not identified there.

Fig. 3. IWS quicklook and basic statistical capabilities.

Acknowledgements The research leading to this results has received funding from the European Community's Seventh Framework Programme ([FP7/2007-2013]), under grant agreement n 263240.

Bibliography

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Ferencz Cs., Lizunov G., Crespon F. Price I., Bankov L., Przepiórka D., Brieß K., Dudkin D., Girenko A., Korepanov V., Kuzmych A., Skorokhod T., Marinov P., Piankova O., Rothkaehl H., Shtus T., Steinbach P., Lichtenberger J., Sterenharz A., Vassileva A., Ionosphere Waves Service (IWS) – A problem-oriented tool in Ionosphere and Space Weather research produced by POPDAT project, J. Space Weather Space Climate, 2014 (submitted).

(Dorota Przepiórka, Hanna Rothkaehl)

102

SPACE MECHATRONICS AND ROBOTICS

SPACE EXPLORATION – SCIENCE AND TECHNOLOGY

Space exploration is a global endeavor with many technical challenges. The sample return missions are one option to extend our knowledge about the extra-terrestrial materials, processes occurring on surface and subsurface level, as well as interactions between such materials and developed technology. This knowledge is supporting scientific investigations connected with detailed characterization of the Moon, Mars and NEO (Near-Earth Objects) and discussion about the origin of the Solar System. The most effective solution developed at LMRS which was and will be used in several space missions is our involvement in special drives for penetrator devices. This year Rosetta lander, with designed by CBK MUPUS penetrator onboard, will start to operate on the comet 67P. Another launched system was the CHOMIK instrument with sampling acquisition container. Recently we were invited by DLR to produce a new mole penetrator driving mechanism and participate in the science package for the American InSight mission to Mars, and by IKI RAN to participate in the mission Luna-Resurs 1 with penetrator HEEP, also considered as a tool. The LMRS is also actively involved in analyzing the dynamic interactions between satellites during final phase of the rendezvous maneuver. Currently the main effort is focused on control system development for application in robotic arm working in on-orbit environment. The very important and crucial point in analysis and development of new ideas and technologies is discussion on national and international forums. To strengthen the Polish space robotics community, CBK organizes conference on aerospace robotics. In July 2013 a two-day international II Conference on Aerospace RObotics (CARO) took place at CBK PAN. It was organized by CBK PAN, Wrocław University of Technology and Military University of Technology in Warsaw. The conference was devoted to presenting and discussing the ongoing international activities connected with aerospace robotics, to discussing the Polish contribution to European Space Agency programs and space technology transfer. CARO attracted over 70 attendees from Poland and abroad. During six sessions, 32 presentations were given by representatives of over 25 institutes, universities and industry. Two lectures were given by ESA envoys: Gian- franco Visentin (ESA Technical Di- rectoriate) and Sanjay Vijendran (ESA Science Directoriate). Apart from thematic sessions, a Mars Ro- botic Exploration Program (MREP) panel talk moderated by Mr Zbigniew Kłos took place.

(Jerzy Grygorczuk, Karol Seweryn)

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Mole penetrator driven by an electromagnetic direct drive

The project is devoted to the development of a new generation of mole type penetrator driven by an electromagnetic direct drive. EMOLE will be a low-speed penetrator capable of soil/regolith underground motion/mobility. Its principle of operation is based on interaction of three masses of the device (hammer, casing and counter-mass), between which the energy exchange is performed and as a result hammering action is achieved. EMOLE is the first mole type penetrator in which the electromagnetic linear drive system will be implemented. The major novelty of EMOLE concept is twofold – the penetrator will have much higher reliability of the drive, and its new drive system is feasible to have power settings. The first advantage would be a consequence of a mechanical simplicity of the drive. Only one linear motion of the hammer instead of a number of motions is foreseen. Additional common disadvantageous feature of the existing mechanisms is their permanent, maximum stroke setting without gradation of the stroke value. In the electromagnetic drive being developed, equipping it with the power settings function can be realized through electrical power supply. Since the mole penetrator is foreseen as a carrier of a sample return system, electronics and sensors, its power settings regulation will allow accommodating the power to the concrete soil mechanical properties and in many cases saving sensitive components from the higher, more destructive overloads. The first steps of the project were numerical simulations and optimization of EMOLE’s electro-magnetic drive system. To accomplish this task the Finite Element Method (FEM) was applied. The parametric field-circuit coupled model was created in Ansys software. The purpose of the analysis was to select a configuration which would ensure the highest value of kinetic energy of a hammer stroke. To determine those values, various values of design parameters were investigated. Fig. 1 shows examples of results obtained from the model.

Fig. 1. Magnetic flux density (Tesla) for selected time steps, capacitor voltage and coil current density.

To verify the simulations and technological concept, a test model which possesses two driving segments and most crucial components of future EMOLE design, i.e., hammer and counter-mass linear guidance, was developed (shown in Fig. 1). 104

Fig. 2. Two segments drive test model. The measurement of the masses movements was executed using a fast-acquisition camera. From the hammer velocity, the stroke energy was derived. Results of the tests confirmed the simulation.

(Jerzy Grygorczuk, Bartosz Kędziora, Łukasz Wiśniewski)

High Energy and Efficiency Penetrator (HEEP) The HEEP (Fig. 3) that was developed between 2012 and 2013 enjoys a spectrum of innovations implemented that are dedicated to the increase of energy. In 2013 a test campaign of the prototype took place.

Fig. 3. Penetrator HEEP with crossed-profile tip.

The rod with multi-elements tip was used in tests. The penetrator was delved into two types of materials: loose quartz sand and lunar regolith analogue AGK-2010. The test demonstrated that HEEP is capable of penetrating soil materials up to the depth of about 1m within few minutes (Fig. 4).

105

Fig. 4. Penetrator HEEP during the tests and depth progress in two different materials.

The penetrator has eight power settings, which correspond with energy of penetration. The material Foamglass T4 was used for testing the functionality of these PSs. As previously several strokes were performed using each PS, and then average progress per stroke per PS was calculated. Results are given in Table 1. For this test the crossed-profile tip was used.

Tab. 1. Hammering to Foamglass T4 material with monolith cross profile rod on different gears.

PS 1 2 3 4 5 6 7 8

Av. progr. 0.2 1.9 8.1 13.0 17.8 27.8 37.4 40.5 /stroke [mm]

Another test proved HEEP’s ability of penetration in various porous (foamed glass and YTONG) and high strength materials (granite) (see Figure 5). It was also confirmed that HEEP with energy of the stroke of 3,7J penetrates much better all comparable mediums than any penetrator developed before at CBK.

a) b)

Fig. 5. a) Moment of breaking Ø30x57mm block of YTONG captured on a high speed camera, b) breaking the granite (on the right side ejected granite over 1cm). (Jerzy Grygorczuk, Bartosz Kędziora, Łukasz Wiśniewski)

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Specialized hybrid rolling bearings for use in the space industry (ROLOKOS)

CBK is a leader of the ROLOKOS project conducted jointly with Warsaw University of Technology: Faculty of Materials Science and Engineering and Faculty of Mechatronics, and with the Institute for Sustainable Technologies NRI.

The primary objective of the project is to transfer the accumulated knowledge and patents in Poland onto a specific product – a specialized hybrid rolling bearing. The studies conducted so far show that the proposed solution can provide lower friction and longer life of bearings working without lubricant. The projected properties meet the demands imposed on bearings used in space applications where, often due to vacuum and extreme temperatures, lubricants cannot be applied. Gathered team, will execute and test specialized hybrid bearings and will introduce significant changes in relation to the existing solutions as far as construction design and material engineering is concerned. It is assumed that only using the analysis conducted within the project along with comprehensive research, one can select the best design and material solutions for the novel bearings. The project will provide a tangible opportunity to produce new solutions in the field of high technologies.

In the year 2013 CBK designed a device for testing bearings in simulated space conditions and conducted the first tests of coatings on samples of titanium and stainless steel using vacuum Pin-on- Disk tribometer.

Fig. 6. Ceramic balls for newly developed hybrid bearing.

(Jerzy Grygorczuk, Marcin Dobrowolski, Monika Ciesielska)

Orbital deployer DRAGON

An Orbital Deployer called DRAGON for ejection of the Polish scientific nanosatellite BRITE-PL Heweliusz was developed and is shown in (Fig. 7). The device has three unique mechanisms including adopted and scaled lock and release mechanism from ESA Rosseta mission MUPUS instrument. Heweliusz will be launched from China by Long March 4B rocket. DRAGON project was subjected to a very tight schedule. Nevertheless, the deployer passed a full series of tests, beginning from functional and ending with environmental. Fig. 7. DRAGON Orbital Deployer and BRITE-PL Heweliusz S/C (in a safety box). 107

Functional tests were carried out on the existing test bench located at CBK to actively simulate the lack of gravity and were recorded by high speed camera. Next functional test was performed in the thermal- vacuum chamber. Time of mechanism open and mass model ejection was less than 1 sec in -20°C. DRAGON also passed all required vibration and shock tests. No change was observed in resonance frequencies after sine and random vibration. Finally a fit check was performed on a launch vehicle. DRAGON was attached to the bracket on the adapter ring between the rocket and the main satellite. Deployment signal was sent from the launch vehicle and the deployer opened safely. Telemetry with sensor confirmation of deployment was sent to the rocket computer. The overall dimensions of the deployer are 282×320×287 mm and its mass is 7.2 kg. It is able to deploy a small cuboid BRITE-PL Heweliusz spacecraft of dimensions 200×200×200 mm and mass of 7 kg.

Fig. 8. Integration of BRITE-PL Heweliusz S/C on the DRAGON Orbital Deployer.

(Marcin Dobrowolski, Jerzy Grygorczuk, Marta Tokarz )

ROBOTIC TECHNOLOGIES FOR ON-ORBIT SERVICING

In October 2013 CBK PAN finalized the Polish National Centre for Research and Development LIDER program project entitled: ‘Design and construction of the satellite manipulator prototype as a key element of on-orbit servicing systems.’ The research done in the frame of the project is connected with active debris removal, satellite servicing and especially highly dynamically disturbed object working in on-orbit environment. Tangible results of the project include, i.a.: 1) A prototype of the 7DoF manipulator arm (WMS LEMUR) designed to perform automatic on- orbit capture maneuvers during servicing mission. Manipulator's structure consists of links, joints and interfaces between them. Manipulator's links were made from carbon fiber composite material. Chosen solution is based on one high modulus tape and two carbon sleeves, and resulted in the maximum deflection of 6.15mm and high torsional stiffness. The joint's design is based on the torque motor and backlash free epicycloid gear. Both the chosen gear and motor allow having a central placed hole with a large diameter so it is possible to route the cables inside the joint. The whole mass of the manipulator is less than 20kg and its workspace is half sphere with diameter of about 3m.

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Fig. 9. WMS LEMUR manipulator and the LIDER team.

2) Planar air-bearing microgravity simulator: test-bed that allows experimental verification of control algorithms for free-floating satellite-manipulator system and also allows validation of numerical simulations of such systems. Test-bed consists of the 2x3 meter flat and precisely leveled granite table. A model of the satellite with 2 DoF manipulator moves on the table using flat round air- bearings based on porous media technology. Air-bearings provide coefficient of friction of the magnitude of 10-5, which allows free planar motion of the satellite-manipulator system and allow investigations of nonholonomic nature of its motion. 3) New version of CBK PAN „Simulation Tool for Space Robotics”, which allows numerical simulations of the orbital capture maneuver.

4) Space manipulator control system was developed. This system is based on the fixed-base Jacobian inverse with addition of satellite velocity feedback (i.e., feedback from measurements of manipulator-base velocity, which is resultant from manipulator motions and depends on system parameters). To allow avoidance of dynamic Fig. 10. Planar air-bearing microgravity singularities of the free-floating manipulator new trajectory simulator. planning algorithm was developed and implemented. In this algorithm Bézier curves are used for path planning.

During the LIDER project realization the need to define and develop the dedicated vision system to recognize target satellite motion was recognized. In that context CBK PAN takes part, as a subcontractor, in the European Space Agency’s PECS project ‘Robust, unsupervised visual motion recognition of non-cooperative satellite for on-orbit capture’ led by the Industrial Research Institute for Automation and Measurements (PIAP). The main goal of this project is the development of motion recognition system using results obtained from new test-bed developed in this project and numerical simulations of the orbital rendezvous maneuver. Prototypic hardware realization of the proposed motion recognition system and verification of its performance on specially prepared test-bed will be conducted. This proposed motion recognition system is another key component necessary for performing orbital rendezvous and capture.

(Karol Seweryn, Tomasz Rybus, Monika Ciesielska and LIDER/Observer team)

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AUTONOMOUS CORE DRILLING SYSTEM

Subsurface exploration of Mars, Moon and other bodies in the Sun System will bring new possibilities for planetology and exobiology research. Similarly, the future commercial utilization (e.g, in terms of mining) of an asteroid will require mineral characterization of the selected bodies. Both these needs (scientific and commercial) could be supported by core drilling systems which are able to deliver non- contaminated sample from subsurface regions to landers for future processing. Therefore, since 2012, CBK PAN has been working on the development of autonomous core drill for extreme environments. Such solution could be also used in barely accessible places on Earth using mobile robot and UAV. In 2013, the drilling process was tested in normal and in vacuum conditions tests in normal conditions which confirmed the initial assumptions connected with power requirements as well as bore dust removal. In parallel, the CAD model of the whole system was designed, and in 2014 it is planned to manufacture the first laboratory model.

Fig. 11. The artistic vision of the core drilling system.

The project ‘Development of the automatic core drill working in extreme conditions, especially space environment’ is financed by the Polish National Centre for Research and Development Applied Research Program. It is being executed within a consortium with CBK PAN as a leader, and two faculties of AGH University of Science and Technology (Faculty of Drilling, Oil and Gas and Faculty of Mechanical Engineering and Robotics, The Department of Robotics and Mechatronics) as partners.

(Karol Seweryn, Tomasz Kuciński and Wiertnica team)

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NEW MATERIAL DEVELOPMENT – CHERENKOV TELECOPE ARRAY (CTA) PROJECT AT CBK PAN

The CBK PAN is a member of the Polish Consortium of Cherenkov Telescope Array Project. This consortium was formed by seven Polish scientific units, and it’s a part of the international consortium. Cherenkov Telescope Array (CTA) stands for an initiative to build the next generation of ground-based gamma-ray instruments which will provide the deepest ever insight into the non-thermal high-energy universe. The current baseline design of CTA foresees a factor of 5-10 improvement in sensitivity in the current energy domain of about 100 GeV to some 10 TeV and an extension of the accessible energy range well below 100 GeV and to above 100 TeV.

Fig. 12. SMC mirror developed at CBK PAN.

CBK PAN is responsible for design and development of new material technologies for optical mirrors. The main requirements are connected with the size of PSF and durability for site environment. Since the observatory requires thousands of such mirrors the huge effort is focused on production costs. As a result of 3 year development process the new mirrors manufacturing technique, based on Sheet Moulding Compound (SMC) material and special intermediate layer was developed. PMC is a proven technology in the automotive industry and some of its many advantages include: possible one-step process to obtain the structure, quick forming process which takes only 3 min and possibility to obtain 0% shrinkage. The intermediate layer needed to meet strict optical requirements, including the reflectivity higher than 85% in the range of 300-600 nm. Our composite mirrors are made without the use of glass, thanks to that they are lighter, more robust and manufacturing is less time consuming, compared to traditional glass mirrors.

(Karol Seweryn, Paweł Paśko, Michał Karczewski and CTA@CBK team)

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PUBLICATIONS

* Total number of publications in 2013: 108 (including 59 in the journals from JCR) * Papers in refereed international and national science journals, books, and proceedings: 70 * Monographs, reviews in international and national publications: 7 * Papers accepted or submitted for publication in refereed international science journals in 2013: 7 * Reports delivered at international and national science conferences and meetings: 117 (including 79 invited talks)

Papers in refereed international and national science journals and proceedings:

 Acharya, B. S.; […]GRYGORCZUK, J; KARCZEWSKI, M; MORDALSKA, M; NICOLAU- KUKLIŃSKI, J; PŁATOS, L; RATAJ, M; SEWERYN, K; SIDZ, M; TOKARZ, M; WAWER, P; WAWRZASZEK, R; WIŚNIEWSKI, Ł; […]; CTA Consortium; Introducing the CTA concept; ASTROPARTICLE PHYSICS; vol. 43, pp. 3–18, 2013.  Adams, JH; Ahmad, S; Albert, JN; Allard, D; Ambrosio, M; Anchordoqui, L; Anzalone, A; Arai, Y; Aramo, C; Asano, K; Ave, M; Barrillon, P; Batsch, T; Bayer, J; Belenguer, T; Bellotti, R; Berlind, AA; Bertaina, M; Biermann, PL; Biktemerova, S; Blaksley, C; BŁĘCKI, J; Blin-Bondil, S; Blumer, J; Bobik, P; Bogomilov, M; Bonamente, M; Briggs, MS; Briz, S; Bruno, A; Cafagna, F; Campana, D; Capdevielle, JN; Caruso, R; Casolino, M; Cassardo, C; Castellini, G; Catalano, O; Cellino, A; Chikawa, M; Christi, MJ; Connaughton, V; Cortes, JF; Crawford, HJ; Cremonini, R; Csorna, S; D'Olivo, JC; Dagoret-Campagne, S; de Castro, A; De Donato, C; de la Taille, C; del Peral, L; Dell'Oro, A; De Pascale, MP; Di Martino, M; Distratis, G; Dupieux, M; Ebersoldt, A; Ebisuzaki, T; Engel, R; Falk, S; Fang, K; Fenu, F; Fernandez-Gomez, I; Ferrarese, S; Franceschi, A; Fujimoto, J; Galeotti, P; Garipov, G; Geary, J; Giaccari, UG; Giraudo, G; Gonchar, M; Alvarado, CG; Gorodetzky, P; Guarino, F; Guzman, A; Hachisu, Y; Harlov, B; Haungs, A; Carretero, JH; Higashide, K; Iguchi, T; Ikeda, H; Inoue, N; Inoue, S; Insolia, A; Isgro, F; Itow, Y; Joven, E; Judd, EG; Jung, A; Kajino, F; Kajino, T; Kaneko, I; Karadzhov, Y; Karczmarczyk, J; Katahira, K; Kawai, 112

K; Kawasaki, Y; Keilhauer, B; Khrenov, BA; Kim, JS; Kim, SW; Kim, SW; Kleifges, M; Klimov, PA ; Ko, SH ; Kolev, D; Kreykenbohm, I; Kudela, K; Kurihara, Y; Kuznetsov, E; La Rosa, G; Lee, J; Licandro, J; Lim, H; Lopez, F; Maccarone, MC; Mannheim, K; Marcelli, L; Marini, A; Martin-Chassard, G; Martinez, O; Masciantonio, G; Mase, K; Matev, R; Maurissen, A; Medina- Tanco, G; Mernik, T; Miyamoto, H; Miyazaki, Y; Mizumoto, Y; Modestino, G; Monnier-Ragaigne, D; de los Rios, JAM; Mot, B; Murakami, T; Nagano, M; Nagata, M; Nagataki, S; Nakamura, T; Nam, JW; Nam, S; Nam, K; Napolitano, T; Naumov, D; Neronov, A; Nomoto, K; Ogawa, T; Ohmori, H; Olinto, AV; ORLEAŃSKI, P; Osteria, G; Pacheco, N; Panasyuk, MI; Parizot, E; Park, IH; Pastircak, B; Patzak, T; Paul, T; Pennypacker, C; Peter, T; Picozza, P; Pollini, A; Prieto, H; Reardon, P; Reinabi, M; Reyes, M; Ricci, M; Rodriguez, I; Frias, MDR; Ronga, F; ROTHKAEHL, H; Roudil, G; Rusinov, I; Rybczyriski, M; Sabau, MD; Cano, GS; Saito, A; Sakaki, N; Sakata, M; Salazar, H; Sanchez, S; Santangelo, A; Cruz, LS; Palomino, MS; Saprykin, O; Sarazin, F; Sato, H; Sato, M; Schanz, T; Schieler, H; Scotti, V; Scuderi, M; Segreto, A; Selmane, S; Semikoz, D; Serra, M; Sharakin, S; Shibata, T; Shimizu, HM; Shinozaki, K; Shirahama, T; Siemieniec- Ozigbio, G; Lopez, HHS ; Sledd, J; SŁOMIŃSKA, K; Sobey, A; Sugiyama, T; Supa-nitsky, D; Suzuki, M; Szabelska, B ]; Szabelski, J; Tajima, F; Tajima, N; Tajima, T; Takahashi, Y; Takami, H; Takeda, M; Takizawa, Y; Tenzer, C; Tibolla, O; Tkachev, L; Tomida, T; Tone, N; Trillaud, F; Tsenov, R; Tsuno, K; Tymieniecka, T; Uchihori, Y; Vaduvescu, O; Valdes-Galicia, JF; Vallania, P; Valore, L; Vankova, G; Vigorito, C; Villasenor, L; von Ballmoos, P; Wada, S; Wata-nabe, J; Watanabe, S; Watts, J; Weber, M; Weiler, TJ; Wibig, T; Wiencke, L; Wille, M; Wilms, J; Włodarczyk, Z; Yamamoto, T; Yamamoto, Y; Yang, J; Yano, H; Yashin, IV; Yonetoku, D; Yo- shida, K; Yoshida, S; Young, R; Zamora, A; Marchi, AZ; An evaluation of the exposure in nadir observation of the JEM-EUSO mission; ASTROPARTICLE PHYSICS; vol. 44, pp. 76-90, 2013.  Bąk-Stęślicka, U; Kołomański, S; MROZEK, T; Coronal Mass Ejections Associated with Slow Long Duration Flares; SOLAR PHYSICS; vol. 283, pp. 505-517, 2013.  Bednarz, S.; Rzyczniak, M.; Gonet, A.; SEWERYN, K.; Research of Formed Lunar Regholit Analog AGK-2010/Badania wytworzonego analogu gruntu księżycowego AGK-2010; ARCHIVES OF MINING SCIENCES; vol. 58, pp. 551-556, 2013.  Ben-Jaffel, L., STRUMIK M., RATKIEWICZ R., GRYGORCZUK J.; The existence and nature of the interstellar bow shock; ASTROPHYSICAL JOURNAL; vol. 779, doi: 10.1088/0004-637X/779/ 2/130, 2013.  Björn J.R. Davidsson, Pedro J. Gutiérrez, Olivier Groussin, Michael F. A’Hearn, Tony Farnham, Lori M. Feaga, Michael S. Kelley, Kenneth P. Klaasen, Frédéric Merlin, Silvia Protopapa, HANS RICKMAN, Jessica M. Sunshine, Peter C. Thomas; Thermal inertia and surface roughness of Comet 9P/Tempel 1; ICARUS; vol. 224, pp. 154–171, 2013.  Bogusz, J; Kłos, A; KOSEK, W; Wavelet decomposition in the Earth's gravity field investigation; ACTA GEODYNAMICA ET GEOMATERIALIA; vol. 10, pp. 47-59, 2013.  BZOWSKI, M; SOKÓŁ, JM; KUBIAK, MA; Kucharek, H; Modulation of neutral interstellar He, Ne, O in the heliosphere. Survival probabilities and abundances at IBEX; ASTRONOMY & ASTROPHYSICS; vol. 557, doi:10.1051/0004-6361/201321700, 2013.  Chen, JH; Mobius, E; Gloeckler, G; Bochsler, P; BZOWSKI, M; Isenberg, PA; SOKÓŁ, JM; Observational study of the cooling behavior of interstellar helium pickup ions in the inner heliosphere; JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS; vol. 118, pp. 3946-3953, 2013.  Davidsson, BJR; Gutierrez, PJ; Groussin, O; A'Hearn, MF; Farnham, T; Feaga, LM; Kelley, MS; Klaasen, KP; Merlin, F; Protopapa, S; RICKMAN, H; Sunshine, JM; Thomas, PC; Thermal inertia and surface roughness of Comet 9P/Tempel 1; ICARUS; vol. 224, pp. 154-171, 2013.  Desai M.I., F.A. Allegrini, M. BZOWSKI, M.A. Dayeh, H. Funsten, S.A. Fuselier, J. Heerikhuisen, M.A. KUBIAK, D.J. McComas, N.V. Pogorelov, N.A. Schwadron, J.M. SOKÓŁ, G.P. Znak, E.J. 113

Zirnstein; Energetic neutral atoms measured by the Interstellar Boundary Explorer (IBEX): evidence for multiple heliosheath populations; ASTROPHYSICAL JOURNAL; doi:10.1088/0004-637X/780/1/98, 2013.  Dudnik, OV; Kurbatov, EV; Avilov, AM; Prieto, M; Sanchez, S; Spassky, AV; Titov, KG; SYLWESTER, J; GBUREK, S; PODGÓRSKI, P; Results of the first tests of the SIDRA satellite-borne instrument breadboard model; PROBLEMS OF ATOMIC SCIENCE AND TECHNOLOGY; issue: 3, pp. 297-302, 2013.  Dudnik, OV; Prieto, M; Kurbatov, EV; Sanchez, S; Titov, KG; SYLWESTER, J; GBUREK, S; PODGÓRSKI, P; Runctional capabilities of the breadboard model of SIDRA satellite-borne instrument; PROBLEMS OF ATOMIC SCIENCE AND TECHNOLOGY; issue: 3, pp. 289-296; 2013.  Figura, P; MACEK, WM; Model of line preserving field line motions using Euler potentials; ANNALS OF PHYSICS; vol. 333, pp. 127-135, 2013.  Fouchard, M; RICKMAN, H; Froeschle, C; Valsecchi, GB; Planetary perturbations for Oort Cloud comets. I. Distributions and dynamics; ICARUS; vol. 222, pp. 20-31, 2013.  Frandsen, S; Lehmann, H; Hekker, S; Southworth, J; Debosscher, J; Beck, P; Hartmann, M; Pigulski, A; Kopacki, G; Kołaczkowski, Z; STĘŚLICKI, M; Thygesen, AO; Brogaard, K; Elsworth, Y; KIC 8410637: a 408-day period eclipsing binary containing a pulsating giant star; ASTRONOMY & ASTROPHYSICS; vol. 556, doi: 10.1051/0004-6361/201321817, 2013.  Frisch, PC; BZOWSKI, M; Livadiotis, G; McComas, DJ; Moebius, E; Mueller, HR; Pryor, WR; Schwadron, NA; SOKÓŁ, JM; Vallerga, JV; Ajello, JM; Decades-Long Changes of the Interstellar Wind Through Our Solar System; SCIENCE; vol. 341, pp. 1080-1082, 2013.  Galli, A; Wurz, P; Kollmann, P; Brandt, PC; BZOWSKI, M; SOKÓŁ, JM; KUBIAK, MA; Grigoriev, A; Barabash, S; Heliospheric energetic neutral hydrogen measured with ASPERA-3 and ASPERA-4; ASTROPHYSICAL JOURNAL; vol. 775, doi: 10.1088/0004-637X/775/1/24; 2013.  García Muñoz A., P. WOLKENBERG, A. Sánchez-Lavega, R. Hueso, and I. Garate-López; A model of scattered thermal radiation for Venus from 3 to 5μm; PLANETARY and SPACE SCIENCE; vol. 81, pp. 65-73, 2013.  GBUREK, S; SYLWESTER, J; KOWALIŃSKI, M; BĄKALA, J; KORDYLEWSKI, Z; PODGÓRSKI, P; PŁOCIENIAK, S; SIARKOWSKI, M; SYLWESTER, B; TRZEBIŃSKI, W; Kuzin, SV; Pertsov, AA; Kotov, YD; Farnik, F; Reale, F; Phillips, KJH; SphinX: The Solar Photometer in X-Rays; SOLAR PHYSICS; vol. 283, pp. 631-649, 2013.  Grzegorzewski Marek, Anna Świątek, Stanisław OSZCZAK, Adam Ciecko, Janusz Cwiklak; Study of EGNOS safety of life service during the period of solar maximum activity; ARTIFICIAL SATELLITES, JOURNAL OF PLANETARY GEODESY;vol. 47, pp. 137-145, 2013.  GRZĘDZIELSKI, S; SWACZYNA, P; BZOWSKI, M; Heavy coronal ions in the heliosphere II. Expected fluxes of energetic neutral He atoms from the heliosheath; ASTRONOMY & ASTROPHYSICS; vol. 549, doi: 10.1051/0004-6361/201220104, 2013.  GULYAEVA, T; Arikan, F; STANISŁAWSKA, I; Poustovalova, L; Symmetry and asymmetry of ionospheric weather at magnetic conjugate points for two midlatitude observatories; ADVANCES IN SPACE RESEARCH; vol. 52, pp. 1837-1844, 2013.  GULYAEVA, T; STANISŁAWSKA, I; Deformation of the ionosphere structure during the space weather events on October-November 2003, DVANCES IN SPACE RESEARCH; vol. 51, pp. 683-690, 2013.  Gulyaeva, TL; Arikan, F; Hernandez-Pajares, M; STANISŁAWSKA, I; GIM-TEC adaptive ionospheric weather assessment and forecast system; JOURNAL OF ATMOSPHERIC AND SOLAR- TERRESTRIAL PHYSICS; vol. 102, pp. 329-340, 2013.

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 Hegler Sebastian, Christoph Statz, Ronny Hahnel, Dirk Plettemeier, Alain Herique, Włodek KOFMAN; Operation of CONSERT aboard Rosetta during the descent of Philae; PLANETARY AND SPACE SCIENCE; vol. 89, pp. 151-158, 2013.  Huenemoerder, David P.; Phillips, Kenneth J.H.; SYLWESTER J.; SYLWESTER B.; Stellar coronae, solar flares: a detailed comparison of sigma Gem, HR 1099, and the Sun in high-resolution X-rays (vol. 768, 135, 2013); ASTROPHYSICAL JOURNAL; vol. 776, doi: 10.1088/0004-637X/776/2/139, 2013.  Huenemoerder, DP; PHILLIPS, KJH; SYLWESTER, J; SYLWESTER, B; Stellar coronae, solar flares: a detailed comparison of sigma Gem, HR 1099, and the Sun in high-resolution X-rays; ASTROPHYSICAL JOURNAL; vol. 768, doi: 10.1088/0004-637X/768/2/135, 2013.  Jagoda, M; RUTKOWSKA, M; Estimation of the Love and Shida numbers: h(2), l(2) using SLR data for the low satellites; ADVANCES IN SPACE RESEARCH; vol. 52, pp. 633-638, 2013.  Kaczorowski, M; Unrecognized origin signals disturbing water-tubes tiltmeters measurements in Geodynamic Laboratory of SRC in Książ; ACTA GEODYNAMICA ET GEOMATERIALIA; vol. 10, pp. 323- 333, 2013.  Katushkina, OA; Izmodenov, VV; Quemerais, E; SOKÓŁ, JM; Heliolatitudinal and time variations of the solar wind mass flux: Inferences from the backscattered solar Lyman-alpha intensity maps; JOURNAL OF GEOPHYSICAL RESEARCH - SPACE PHYSICS; vol. 118, pp. 2800-2808, 2013.  Kossacki, KJ; SZUTOWICZ, S; Activity of Comet 29P/Schwassmann-Wachmann 1; ICARUS; vol. 225, pp. 111-121, 2013.  KRÓLIKOWSKA M., P.A. Dybczyński; Near-parabolic comets observed in 2006-2010. The individualized approach to 1/a-determination and the new distribution of original and future orbits; MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY; vol. 435, pp. 440-459, 2013.  Krucker, S; Benz, AO; Hurford, GJ; Arnold, NG; ORLEAŃSKI, P; Grobelbauer, HP; Casadei, D; Kobler, S; Iseli, L; Wiehl, HJ; Csillaghy, A; Etesi, L; Hochmuth, N; Battaglia, M; Bednarzik, M; Resanovic, R; Grimm, O; Viertel, G; Commichau, V; Howard, A; Meuris, A; Limousin, O; Brun, S; Vilmer, N; SKUP, KR; GRACZYK, R; STOLARSKI, M; MICHALSKA, M,; NOWOSIELSKI, W; CICHOCKI, A; MOSDORF, M; SEWERYN, K; BIAŁEK, A; SYLWESTER, J; KOWALIŃSKI, M; MROZEK, T; PODGÓRSKI, P; Mann, G; Onel, H; Aurass, H; Bauer, SM; Bittner, W; Dionies', F; Paschke, J; Pluschke, D; Popow, E; Rendtel, J; Warmuth, A; Woche, M; Wolter, D; Van Beek, HF; Farnik, F; Lin, RP; The spectrometer/telescope for imaging X-rays on board the ESA Solar Orbiter spacecraft; NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT; vol. 732, pp. 295-298, 2013.  KUBIAK, MA; BZOWSKI, M; SOKÓŁ, JM; Mobius, E; Rodriguez, DF; Wurz, P; McComas, DJ; Assessment of detectability of neutral interstellar deuterium by IBEX observations; ASTRONOMY & ASTROPHYSICS; vol. 556, doi: 10.1051/0004-6361/201321166, 2013.  Kucharski D., SCHILLAK S., Hyung-Chul Lim, Otsubo T.; Spectral analysis of Borowiec SLR data for spin determination of geodetic satellite EGP; ARTIFICIAL SATELLITES, JOURNAL OF PLANETARY GEODESY; vol. 48, pp. 15-23, 2013.  Leszek JAWORSKI, Anna ŚWIĄTEK, Ryszard ZDUNEK; EGNOS limitations over central and eastern Poland - results of preliminary tests of EGNOS-EUPOS integration project; vol. 48, pp. 93-102, 2013.  Lis, DC; Biver, N; Bockelee-Morvan, D; Hartogh, P; Bergin, EA; Blake, GA; Crovisier, J; de Val- Borro, M; Jehin, E; Kuppers, M; Manfroid, J; Moreno, R; Rengel, M; SZUTOWICZ, S; A Herschel study of D/H in water in the Jupiter-family comet 45P/Honda-Mrkos-Pajdusakova and prospects for D/H measurements with CCAT; ASTROPHYSICAL JOURNAL LETTERS; vol. 774, doi: 10.1088/2041- 8205/774/1/L3, 2013. 115

 MACEK W.; WAWRZASZEK A.; Voyager 2 observation of the multifractal spectrum in the heliosphere and the heliosheath; NONLINEAR PROCESSES IN GEOPHYSICS; vol. 20, pp. 1061-1070, 2013.  Majcher, A; Sokołowski, M; Batsch, T; Castro-Tirado, AJ; Czyrkowski, H; Cwiek, A; Cwiok, M; Dąbrowski, R; Kasprowicz, G; Majczyna, A; Malek, K; Mankiewicz, L; Nawrocki, K; Obara, L; Opiela, R; Piotrowski, LW; Siudek, M; WAWRZASZEK, R; Wrochna, G; Zaremba, M; Zarnecki, AF; Parallax in "Pi of the Sky" Project; ADVANCES IN SPACE RESEARCH; vol. 52, pp. 1349- 1354, 2013.  Molotkov, IA; ATAMANIUK, B; Popov, AV; Interaction of oblique wave beam with ionospheric layer F2; ADVANCES IN SPACE RESEARCH; vol. 51, pages: 2333-2341, 2013.  Moreno, DFR; Wurz, P; Saul, L; BZOWSKI, M; KUBIAK, MA; SOKÓŁ, JM; Frisch, P; Fuselier, SA; McComas, DJ; Mobius, E; Schwadron, N; Evidence of direct detection of interstellar deuterium in the local interstellar medium by IBEX; ASTRONOMY & ASTROPHYSICS; vol. 557, doi: 10.1051/0004- 6361/201321420, 2013.  NIEDZIELSKI, T; Miziński, B; Automated system for near-real time modelling and prediction of altimeter- derived sea level anomalies; COMPUTERS & GEOSCIENCES; vol. 58, pp. 29-39, 2013.  Osiecki L., T. ZAWISTOWSKI, B. Zylinski, J. Piechna; Simulation of Fluid Structure Interaction in a Novel Desigh of High Pressure Asial Piston Hydraulic Pump; ARCHIVE OF MECHANICAL ENGINEERING; vol. 3, AME-D-12-00040, 2013.  Piotrowski, LW; Batsch, T; Czyrkowski, H; Cwiok, M; Dąbrowski, R; Kasprowicz, G; Majcher, A; Majczyna, A; Małek, K; Mankiewicz, L; Nawrocki, K; Opiela, R; Siudek, M; Sokołowski, M; WAWRZASZEK, R; Wrochna, G; Zaremba, M; Zarnecki, AF; PSF modelling for very wide-field CCD astronomy; ASTRONOMY & ASTROPHYSICS; vol. 551, doi: 10.1051/0004-6361/201219230, 2013.  Priyadarshi, S; WERNIK, AW; Variation of the ionospheric scintillation index with elevation angle of the transmitter; ACTA GEOPHYSICA; vol. 61, pp. 1279-1288, 2013.  RICKMAN HANS; The Oort Cloud and long-period comets; METEORITICS & PLANETARY SCIENCE; vol. 49, pp. 8-20, 2013.  Saul, L., BZOWSKI, M., Fuselier, S., KUBIAK, M.A., McComas, D., Möbius, E., SOKÓŁ, J.M., Rodríguez, D., Scheer, J., Wurz, P.; Local interstellar hydrogen's disappearance at 1 AU: four years of IBEX in the rising solar cycle; ASTROPHYSICAL JOURNAL; vol. 767, doi: 10.1088/0004- 637X/767/2/130, 2013.  Schwadron, NA; Moebius, E; Kucharek, H; Lee, MA; French, J; Saul, L; Wurz, P; BZOWSKI, M; Fuselier, SA; Livadiotis, G; McComas, DJ; Frisch, P; Gruntman, M; Mueller, HR; Solar radiation pressure and local interstellar medium flow parameters from interstellar boundary explorer low energy hydrogen measurements; ASTROPHYSICAL JOURNAL; vol. 775, doi:10.1088/0004-637X/775/ 2/86, 2013.  SŁOMIŃSKA, E; ROTHKAEHL, H; Mapping seasonal trends of electron temperature in the topside ionosphere based on DEMETER data; ADVANCES IN SPACE RESEARCH; vol. 52, pp. 192-204, 2013.  Soffitta, Paolo; Barcons, Xavier; Bellazzini, Ronaldo; Braga, Joao; Costa, Enrico; Fraser, George W.; GBUREK SZYMON; Huovelin, Juhani; Matt, Giorgio;… ; XIPE: the X-ray imaging polarimetry explorer; EXPERIMENTAL ASTRONOMY; vol. 36, pp. 523-567, 2013.  SOKÓŁ, JM; M. BZOWSKI; M. Tokumaru; K. Fujiki; D.J. McComas; Heliolatitude and Time Variations of Solar Wind Structure from in situ Measurements and Interplanetary Scintillation Observations; SOLAR PHYSICS; vol. 285, pp. 167-200, 2013.

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 STASIEWICZ, K; Markidis, S; Eliasson, B; STRUMIK, M; Yamauchi, M; Acceleration of solar wind ions to 1 MeV by electromagnetic structures upstream of the Earth's bow shock; EPL (Europhysics Letters); vol. 102, doi: 10.1209/0295-5075/102/49001, 2013.  STRUMIK, M; CZECHOWSKI, A; GRZĘDZIELSKI, S; MACEK, WM; RATKIEWICZ, R; Small-scale local phenomena related to the magnetic reconnection and turbulence in the proximity of the heliopause; ASTROPHYSICAL JOURNAL LETTERS; vol. 773, doi: 10.1088/2041-8205/773/2/L23, 2013.  SYLWESTER, B; Phillips, KJH; SYLWESTER, J; KĘPA, A; Silicon Abundance from RESIK Solar Flare Observations; SOLAR PHYSICS; vol. 283; pp. 453-461; 2013.  Usowicz, B; Lipiec, J; Usowicz, JB; MARCZEWSKI, W; Effects of aggregate size on soil thermal conductivity: Comparison of measured and model-predicted data; INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER; vol. 57, pp. 536-541, 2013.  WIŚNIOWSKI, T; RICKMAN, H; Fast Geometric Method for Calculating Accurate Minimum Orbit Intersection Distance; ACTA ASTRONOMICA; vol. 63, pp. 293-307, 2013.  Zaalov, NY; ROTHKAEHL, H; Stocker, AJ; Warrington, EM; Comparison between HF propagation and DEMETER satellite measurements within the mid-latitude trough; ADVANCES IN SPACE RESEARCH; vol. 52, pp. 781-790, 2013.  ZALEWSKA (ANDRZEJEWSKA), N; Hellas Planitia as a potential site of sedimentary minerals; PLANETARY AND SPACE SCIENCE; vol. 78, pp. 25-32, 2013.

Papers accepted or submitted for publication in 2013

 Alothman A.O., SCHILLAK S; Recent results for the Arabian plate motion using satellite laser ranging observations of Riyadh SLR station to LAGEOS-1 and LAGEOS-2 satellites; ARABIAN JOURNAL FOR SCIENCE AND ENGINEERING; vol. 39, pp. 217-226, 2013.  P. Bochsler; H. Kucharek; E. Mobius; M. BZOWSKI, J.M. SOKÓŁ, L. Didkovsky, S. Wieman; Solar photoionization rates for interstellar neutrals in the inner heliosphere: H, He, O, and Ne, THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, (10pp), doi:10.1088/0067- 0049/210/1/12, 2014.  Bockelée-Morvan, D.; Biver, N.; Crovisier, J.; Lis, D. C.; Hartogh, P.; Moreno, R.; de Val-Borro, M.; Blake, G. A.; SZUTOWICZ, S.; Boissier, J.; Cernicharo, J.; Charnley, S.B.; Combi, M.; Cordiner, M.A.; de Graauw, T.; Encrenaz, P.; Jarchow, C.; Kidger, M.; Küppers, M.; Milam, S.N.; Müller, H.S P.; Phillips, T.G.; Rengel, M.; Searches for HCl and HF in comets 103P/Hartley 2 and C/2009 P1 (Garradd) with the Herschel space observatory; ASTRONOMY & ASTROPHYSICS; doi:10.1051/0004-6361/201322939, 2014.  M. Fouchard, H.RICKMAN, Ch. Froeschlé, G.B. Valsecchi; Planetary perturbations for Oort Cloud comets. II. Implication for the origin of the observable comets; ICARUS, vol. 231, pp. 110-121, 2014.  M. Fouchard, H. RICKMAN, Ch. Froeschlé, G.B. Valsecchi; Planetary perturbations for Oort Cloud comets. III. Evolution of the cloud and production of Centaurs and Halley type comets; ICARUS; vol. 231, pp. 99-109, 2014.  Savin S., E. Amata, V. Budaev, L. Zelenyi, E.A.Kronberg, J. Buechner, J. Safrankova, Z. Nemecek, J. BŁĘCKI, L. Kozak , S. Klimov, A. Skalsky, L. Lezhen; On nonlinear cascades and resonances in the outer magnetosphere; JETP LETTERS; vol. 99, pp. 19-24, 2014.  ŚWIĄTEK Anna, Iwona STANISŁAWSKA, Zbigniew ZBYSZYŃSKI, Beata DZIAK- JANKOWSKA; Extension of EGNOS Ionospheric Correction Coverage Area; ACTA GEOPHYSICA; vol. 62, pp. 259-269, 2014.

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Monographs, reviews in international and national publications

 BANASZKIEWICZ MAREK, Geoffrey M. Smith, Javier Gallego, SEBASTIAN ALEKSANDROWICZ, STANISŁAW LEWIŃSKI, ANDRZEJ KOTARBA, Zbigniew Bochenek, Katarzyna Dąbrowska-Zielińska, Konrad Turlej, Andrew Groom, Alistair Lamb, Thomas Esch, Annekatrin Metz, Markus Törmä, Vassil Vassilev, Gedas Vaitkus; European Area Frame Sampling based on Very High Resolution images; Land Use and Land Cover Mapping in Europe, practices and trends, 2013.  BZOWSKI M., J.M. SOKÓŁ, M. Tokumaru, K. Fujiki, E. Quémerais, R. Lallement, S. Ferron, P. Bochsler, D.J. McComas; Solar parameters for modeling the interplanetary background; Cross-Calibration of Past and Present Far UV Spectra of Solar System Objects and the Heliosphere; ISSI Scientific Report Series 13, pp. 67-138, 2013.  Izmodenov, V.V.; O.A. Katushkina; E. Quémerais; M. BZOWSKI; Distribution of interstellar hydrogen atoms in the heliosphere and backscattered solar Lyman-?, Chapter 2 in "Cross-Calibration of Past and Present Far UV Spectra of Solar System Objects and the Heliosphere", ISSI Scientific Report Series 13, ed. R.M. Bonnet, E. Quémerais, M. Snow, Springer Science+Business Media, New York, pp. 7-65, 2013.  Kwiatkowski Mirosław, WOŹNIAK EDYTA, Kołakowski Bartłomiej; Wykorzystanie satelitarnych wskaźników roślinności do szacowania obciążenia ogniowego drzewostanów sosnowych; Zagrożenia lasów zależne od stanu atmosfery; vol. 1, pp. 30-41, 2013.  LEWIŃSKI STANISŁAW, Zbigniew Bochenek, Konrad Turlej; Application of an object-oriented method for classification of VHR satellite images using a rule-based approach and texture measures; Land Use and Land Cover Mapping in Europe, practices and trends, 2013.  ROTHKAEHL H., M. Morawski, M. KRZEWSKI, G Lizunow; Диагностика спектра плазменных ви с использованием радиочастотного анализатора RFA (Diagnostyka spektralna fal plazmowych z wykorzystaniem analizatora częstotliwości radiowych RFA); КОСМИЧЕСКй ПРОЕКТ "ИОНОСАТ- МИКРО"; ISBN 978-966-360-228-8, pp. 101-108, 2013.  WOŹNIAK EDYTA, Kwiatkowski Mirosław; Modelowanie udziału wybranych typów siedliskowych lasu na podstawie map pokrycia Corine Land Cover i numerycznych modeli terenu; Zagrożenia lasów zależne od stanu atmosfery; vol. 1, pp. 42-55, 2013.

Other articles in international and national publications

 Barciński, Tomasz; LISOWSKI JAKUB; RYBUS TOMASZ; SEWERYN KAROL; Controlled Zero Dynamics Feedback Linearization with Application to Free-Floating Redundant Orbital Manipulator; 2013 AMERICAN CONTROL CONFERENCE (ACC) Book Series: Proceedings of the American Control Conference; pp. 1834-1839, 2013.  Batsch, T.; Czyrkowski, H.; Cwiok, M.; Dąbrowski, R.; Kasprowicz, G.; Majcher, A.; Majczyna, A.; Malek, K.; Mankiewicz, L.; Nawrocki, K.; Opiela, R.; Piotrowski, L.W.; Siudek, M.; Sokołowski, M.; WAWRZASZEK R.; Wrochna, G.; Zaremba, M.; Zarnecki, A.F.; Status of pi of the sky telescopes in spain and chile gamma-ray bursts: 15 years of GRB afterglows - progenitors, environments and host galaxies from the nearby to the early universe; Book Series: EAS Publications Series; vol. 61, pp. 479-481, 2013.  BIAŁEK AGATA (AGATA PRZEPIÓRKA); KAROL SEWERYN; Nicolas Arnold; Svend M. Bauer; Adeline Bernet; Luc Blecha; KAMIL GRASSMANN; Oliver Grimm; Hans Peter Grobelbauer; Gordon Hurford; Sam Krucker; Olivier Limousin; Gottfried Mann; Jerome Martignac; Aline Meuris; PIOTR ORLEAŃSKI; Hakan Onel; KONRAD R. SKUP; Thermal simulations of the STIX instrument for ESA Solar Orbiter mission; Proceedings of 43rd International Conference on Environmental Systems, 2013.

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 BŁĘCKA M.I., L. Zasova; Influence of dust and aerosols on radiance spectra of various astronomical objects; First Planetary Science meeting Warsaw 15-16 January 2013 – webpage CBK, 2013.  Brandt S., M. Hernanz, M. Feroci, L. Amati, Alvarez, P. Azzarello, D. Barret, E. Bozzo, C. Budtz- Jørgensen, R. Campana, A. Castro-Tirado, A. Cros, E. Del Monte, I. Donnarumma, Y. Evangelista, J.L. Galvez Sanchez, D. Götz, F. Hansen, J.W. den Herder, A. Hornstrup, R. Hudec, D. Karelin, M. van der Klis, S. Korpela, I. Kuvvetli, N. Lund, P. ORLEANSKI, M. Pohl, A. Rachevski, A. Santangelo, S. Schanne, C. Schmid, L. Stella, S. Suchy, C. Tenzer, A. Vacchi, J. Wilms, N. Zampa, J.J.M. in’t Zand, A. Zdziarski; Observing GRBS with the loft wide field monitor; EAS Publications Series - Proceedings of " Fall Gamma Ray Burst Symposium on 15 years of Gamma- Ray Bursts afterglows: Progenitors, Environments and Host Galaxies from the Nearby to the Early Universe"; vol.61, pp. 617-623, 2013.  Buczek Ł., J. Kołodziej, P. Krehlik, M. Lipiński, Ł. Śliwczyński, P. DUNST, D. LEMAŃSKI, J. NAWROCKI, P. NOGAŚ, A. Czubla, W. Adamowicz, J. Igalson, T. Pawszak, J. Pieczerak, Binczewski, W. Bogacki, P. Ostapowicz, M. Stroiński, K. Turza; OPTIME – Time and Frequency Dissemination System Based on Fiber Optical Network – PIONIER; Proc. 2013 Joint UFFC, EFTF and PFM Symposium, vol.1, pp. 317-320, 2013.  Chmaj G., T. Buratowski, T. Uhl, K. SEWERYN, M. BANASZKIEWICZ; The Dynamic Influence of the Attached Manipulator on Unmanned Aerial Vehicle; AEROSPACE ROBOTICS Book Series: GeoPlanet: Earth and Planetary Sciences; pp. 108-118, 2013.  Chmielewska E., Tomczak M., MROZEK T.; Simultaneous Yohkoh/SXT and TRACE observations of solar plasma ejections; Cent. Eur. Astrophys. Bull.; vol. 37, pp. 597-608, 2013.  Cwiek, A.; Batsch, T.; Czyrkowski, H.; Cwiok, M.; Dabrowski, R.; Kasprowicz, G.; Majcher, A.; Malek, K.; Mankiewicz, L.; Nawrocki, K.; Obara, L.; Opiela, R.; Piotrowski, L.W.; Siudek, M.; Sokołowski, M.; WAWRZASZEK R.; Zarnecki, A.F.; Pi of the Sky - robotic telescope; PHOTO-NICS APPLICATIONS IN ASTRONOMY, COMMUNICATIONS, INDUSTRY, AND HIGH- ENERGY PHYSICS EXPERIMENTS 2013; Book Series: Proceedings of SPIE; vol. 8903, 2013.  Czubla A., M. Lipiński, R. Osmyk, J. NAWROCKI, P. Szterk, P. NOGAŚ, Ł. Śliwczyński, D. LEMAŃSKI, P. Krehlik, P. Dunst, Ł. Buczek; Precyzyjny światłowodowy transfer czasu i częstotliwości w relacji GUM-AOS (420 km); PAK; nr 59/6, 2013.  DRZEWIECKI Wojciech, Anna WAWRZASZEK, Michał KRUPIŃSKI, Sebastian ALEKSANDROWICZ, Katarzyna Bernat; Comparison of Selected Textural Features as Global Content- Based Descriptors of VHR Satellite Image – the EROS-A Study; Proceedings of the 2013 Federated Conference on Computer Science and Information Systems; pp. 43–49, 2013.  Gian-Paolo Tozzi; Blecka, M.; Capaccioni, F.; Faggi, S.; Filacchione, G.; Fink, U.; Rinaldi, G.; Dust observations of comet 67P/Churyumov-Gerasimenko and comparison with ICES model; American Astronomical Society, DPS meeting #45; Bibliographic Code: 2013DPS. 4541307T, 2013.  GRYCIUK M., S. GBUREK, M. SIARKOWSKI, P. PODGÓRSKI, J. SYLWESTER, F. Farnik; Comparison of Solar Activity During Last Two Minima on turn of Cycles Activity 22/23 and 23/24; Proceedings IAU Symposium; vol. 294, pp. 65-66, 2013.  GRYGORCZUK J., B. KĘDZIORA, M. TOKARZ, K. SEWERYN, M. BANASZ-KEWICZ, M. DOBROWOLSKI, P. Łyszczek, T. RYBUS, M. SIDZ, K. SKUP, R. WAWRZASZEK; Prototype of ultra-light planetary manipulator – design, tests and simulations; Proceedings of ASTRA Conference, 2013.  GRYGORCZUK J., B. KĘDZIORA, M. TOKARZ, K. SEWERYN, M. BANASZKIEWICZ, M. DOBROWOLSKI, P. Łyszczek, T. RYBUS, M. SIDZ, K. SKUP, R. WAWRZASZEK; Ultra-Light Planetary Manipulator: Study and Development; AEROSPACE ROBOTICS Book Series: GeoPlanet: Earth and Planetary Sciences; pp. 129-141; 2013.

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 GRYGORCZUK Jerzy, Marek BANASZKIEWICZ, Karol SEWERYN, Łukasz WIŚNIEWSKI, Roman WAWRZASZEK; Space Penetrators – Rosetta case study; Proceedings of MMAR; 2013.  JAWORSKI J., K. Bobrowski, Ł. Boruc, K. Gedroyć, K. Macioszek, T. RYBUS; New Low-Cost Video Camera Pointing Mechanism for Stratospheric Balloons: Design and Operational Tests; GeoPlanet: Earth and Planetary Sciences; pp.:95-107, 2013.  JUCHNIKOWSKI, G; LISOWSKI, J; SKUP, K; WAWRZASZEK, R; BARCIŃSKI, T; ZAWISTOWSKI, T; Simulation and Visualization of Attitude Control System Operations for BRITE-PL Satellite; AEROSPACE ROBOTICS Book Series: GeoPlanet: Earth and Planetary Sciences; pp. 21-33, 2013.  Knap Ewa; GRYGORCZUK JERZY; Pyrzanowski Paweł; The Project of a Simple Drive for CCD Observation Cameras; AEROSPACE ROBOTICS Book Series: GeoPlanet: Earth and Planetary Sciences; pp. 51-59, 2013.  LEJBA P., J. NAWROCKI, D. Lemański, P. Nogas, P. DUNST; Precise Point Positioning Technique for Short and Long Baselines Time Transfer; Proceedings of Joint UFFC, EFTF and PFM Symposium; UFFC2013-001428, pp. 815-818, 2013.  Lilensten Jean, Mathieu Barthélémy, Pierre-Olivier Amblard, Hervé Lamy, Cyril Simon Wedlund, Véronique Bommier, Joran Moen, Hanna ROTHKAEHL, Julien Eymard, Jocelyn Ribot; The thermospheric auroral red line polarization: confirmation of detection and first quantitative analysis; Journal of Space Weather and Space Climate; vol. 3, 2013.  MROZEK T., S. GBUREK, M. SIARKOWSKI, B. SYLWESTER, J. SYLWESTER, A. KĘPA, M. GRYCIUK; Solar flares observed simultaneously with SphinX, GOES and RHESSI; Proceedings of IAU Symposium; vol. 294, pp. 571-572, 2013.  Müller H.R, M. BZOWSKI, E. Möbius, G. P. Zank; Interstellar helium in the heliosphere; Proc. Solar Wind 13 Conference, AIP CP; vol. 1539, pp. 348-351, 2013.  NASTULA Jolanta, David Salstein, Richard Gross; Regional Multi-Fluid-Based Geophysical Excitation of Polar Motion; IAG Proceedings; vol.139, pp. 467-472, 2013.  Pareschi G.; T. Armstrong; H. Baba; J. Bähr; A. Bonardi; G. Bonnoli; P. Brun; R. Canestrari; P. Chadwick; M. Chikawa; P.-H. Carton; V. de Souza; J. Dipold; M. Doro; D. Durand; M. Dyrda; A. Förster; M. Garczarczyk; E. Giro; J.-F. Glicenstein; Y. Hanabata; M. Hayashida; M. Hrabovski; C. Jeanney; M. Kagaya; H. Katagiri; L. Lessio; D. Mandat; M. Mariotti; C. Medina; J. Michalowski; P. Micolon; D. Nakajima; J. Niemiec; A. Nozato; M. Palatka; M. Pech; B. Peyaud; G. Pühlhofer; M. RATAJ; G. Rodeghiero; G. Rojas; J. Rousselle; R. Sakonaka; P. Schovanek; K. SEWERYN; C. Schultz; S. Shu; F. Stinzing; M. Stodulski; M. Teshima; P. Travniczek; C. van Eldik; V. Vassiliev; Ł. WIŚNIEWSKI; A. Wörnlein; T. Yoshida; Status of the technologies for the production of the Cherenkov Telescope Array (CTA) mirrors; Proc. SPIE 8861, Optics for EUV, X-Ray, and Gamma-Ray Astronomy VI; 886103, 2013.  PODGÓRSKI P.; SCISLOWSKI D.; KOWALIŃSKI, M.; MROZEK, T.; STĘŚLICKI, M.; BARYLAK, J.; BARYLAK, A.; SYLWESTER, J.; Krucker, S.; Hurford, G.J.; Arnold, N.G.; ORLEAŃSKI P.; Meuris, A.; Limousin, O.; Gevin, O.; Grimm, O.; Etesi, L.; Hochmuth, N.; Battaglia, M.; Csillaghy, A.; Kienreich, I.W.; Veronig, A.; Bloomfield, S.; Byrne, M.; (Massone, A.M.); Piana, M.; Giordano, S.; SKUP R.; GRACZYK, R.; MICHALSKA, M.; NOWOSIELSKI, W.; CICHOCKI A.; Mosdorf, M; Hardware simulator of Caliste-SO detectors for STIX instrument; PHOTONICS APPLICATIONS IN ASTRONOMY, COMMUNICATIONS, INDUSTRY, AND HIGH-ENERGY PHYSICS EXPERIMENTS 2013, Book Series: Proceedings of SPIE, vol. 8903, 2013.  RYBUS Tomasz, Janusz NICOLAU-KUKLIŃSKI, Karol SEWERYN, Tomasz BARCIŃSKI, Monika CIESIELSKA, Kamil GRASSMANN, Jerzy GRYGORCZUK, Michał KARCZEWSKI, Marek KOWALSKI, Marcin KRZEWSKI, Tomasz KUCIŃSKI, Jakub LISOWSKI, Rafał 120

PRZYBYŁA, Konrad SKUP, Tomasz SZEWCZYK, Roman WAWRZASZEK; new planar air- bearing microgravity simulator for verification of space robotics numerical simulations and control algorithms; Proceedings of ASTRA Conference, 2013.  RYBUS Tomasz, Tomasz BARCIŃSKI, Jakub LISOWSKI, Karol SEWERYN, Janusz NICOLAU-KUKLIŃSKI, Jerzy GRYGORCZUK, Marcin KRZEWSKI, Konrad SKUP, Tomasz SZEWCZYK, Roman WAWRZASZEK; Experimental Demonstration of Singularity Avoidance with Trajectories Based on the Bézier Curves for Free-Floating Manipulator; Proceedings of ROMOCO, 2013.  RYBUS, T; SEWERYN, K; Trajectory Planning and Simulations of the Manipulator Mounted on a Free- Floating Satellite; AEROSPACE ROBOTICS Book Series: GeoPlanet: Earth and Planetary Sciences; pp. 61-73; 2013.  SEWERYN Karol, Kamil GRASSMANN, Monika CIESIELSKA, Tomasz RYBUS, Michał TUREK; Optimization of the robotic joint equipped with epicyloidal gear and direct drive for space applications; Proceedings of ESMATS Conference, 2013.  SEWERYN Karol, Tomasz BARCIŃSKI, Monika CIESIELSKA, Jerzy GRYGORCZUK, Tomasz RYBUS, Konrad SKUP, Roman WAWRZASZEK; Validation of the control strategy of the free flying robot – application to the rendezvous manoeuvres; Proceedings of ASTRA Conference, 2013.  SEWERYN, K; BANASZKIEWICZ, M; Bednarz, S; CIESIELSKA, M; Gonet, A; GRYGORCZUK, J; KUCIŃSKI, T; RYBUS, T; Rzyczniak, M; WAWRZASZEK, R; WIŚNIEWSKI, L; Wójcikowski, M; The Experimental Results of the Functional Tests of the Mole Penetrator KRET in Different Regolith Analogues; AEROSPACE ROBOTICS Book Series: GeoPlanet: Earth and Planetary Sciences; pp. 163-171, 2013.  SKUP Konrad R., Paweł GRUDZIŃSKI, Piotr ORLEAŃSKI, Witold NOWOSIELSKI; A Digital Controller for Satellite Medium Power DC/DC Converters;18th International Conference on Methods and Models in Automation and Robotic (MMAR); pp. 566 – 571, 2013.  WAWRZASZEK A., KRUPIŃSKI M., ALEKSANDROWICZ S., DRZEWIECKI W.; Formalizm multifraktalny w analizie zobrazowań satelitarnych; ARCHIWUM FOTOGRAMETRII, KARTO- GRAFII I TELEDETEKCJI; vol. 25, pp. 261-272, 2013.  WAWRZASZEK R., M. STRUMIK, K. SEWERYN, M. SIDZ, M. BANASZKIEWICZ, L. Rossini, E. Onillon; Electromagnetic Compatibility Problems of ELSA - Novel Component for Spacecraft Attitude Control System Based on Concept of Spherical Actuator; Proceedings of MMAR, 2013.  Weis W., A.Moffat, A.Schwarzenberg-Czerny, O.Kudelka, C.Grant, R.Zee, R.Kusching, St.Mochnacki, S.Ruciński, J.Matthews, P.ORLEAŃSKI, A.Pamyatnykh, A.Pigulski, J.Alves, M.Guedel, G.Handler, G.Wade, A.Scholtz, BRITE Constellation: Nanosatellites for Precision Photometry of Bright Stars; Precision Astroseismology Proceedings IAU Symposium; vol. 301, 2013.  Woźniak, Grzegorz; STOLARSKI MARCIN; Telemetry beacon for Polish payload on BRITE-PL-2 satellite; PHOTONICS APPLICATIONS IN ASTRONOMY, COMMUNICATIONS, INDU- STRY, AND HIGH-ENERGY PHYSICS EXPERIMENTS 2013 Book Series: Proceedings of SPIE, vol. 8903, 2013.  Zawadzki Jarosław J., Karol Przeździecki, Karol Szymankiewicz, Wojciech MARCZEWSKI; Simple Method of Forest Type Inventory by Joining Low Resolution Remote Sensing of Vegetation Indices with Spatial Information from the Corine Land Cover Database; ISRN Forestry; 2013.

121

Grants and Contracts

EU Framework Programme Grants

 EEGS-2: Poszerzenie systemu EGNOS na wschodnią Europę (EEGS- EGNOS Extension to Eastern Europe), J.B. Zieliński (47)  Sieć nauczania, badania i zastosowań metod redukcji zagrożeń związanych z jonosferą (Training, Research and Applications Network to Support The Mitigation of Ionospheric Threats), A. Wernik (64)  Tworzenie baz danych procesów dla celów eksploracji jonosfery POPDAT, (POPDAT - Problem- oriented Processing and Database Creation for Ionosphere Exploration), H. Rothkaehl (100)  ESPAS - Infrastruktura danych z najbliższego otoczenia Ziemi dla e-Science, (ESPAS- Near-Earth Space Data Infrastructure for e-Science), I. Stanisławska (105)  BRIDGES - tworzenie relacji i współdziałania dla rozwoju GMES dla potrzeb bezpie-czeństwa Europy (BRIDGES –Building Relationships and Interactions to Develop GMES for European Security), Z. Kłos (106)  eHEROES wpływ warunków środowiska kosmicznego na ludzi i automaty (eHEROES – Environment for Human Exploration and Robotic), J. Sylwester (109)  Europejski projekt lewitującej Magnetycznie Sfery Reakcyjnej dla Systemów Kontroli Orientacji – ELSA (European Levitated Spherical Actuator ELSA), R. Wawrzaszek (110)  Turbulencja plazmy Układu Słonecznego: obserwacje, intermitencja i multifraktalne, (Solar system plasma Turbulence: Observations, intermittency and Multifractals STORM), W. Macek (132)  GMES przedoperacyjne serwisy bezpieczeństwa dla wsparcia działań zewnętrznych Unii Europejskiej/G-NEXT (GMES- pre-operational security services for supporting external action/G-NEXT), S. Lewiński (135)  Zastosowanie systemów eksploatacji i analizy obrazów i informacji geoprzestrzennych we wsparciu działań zewnętrznych Unii Europejskiej/G-SEXTANT (Service provision of geospatial intelligence In EU external action support /G-SEXTANT), S. Lewiński (136)  EOPOWER - Obserwacje Ziemi jako wzmacnianie potencjału ekonomicznego, (EOPOWER – Earth Observation for Economic Empowerment), S. Lewiński (151)  Przeciwdziałanie wpływom zaburzeń jonosferycznych na działanie precyzyjnych procedur wykorzystujących systemy pozycjonowania satelitarnego w Brazylii – CALIBRA (Countering GNSS high Accuracy applications Limitations due to Ionospheric disturbances In BRAZIL - CALIBRA) (subcontract), M. Grzesiak (152)  Zintegrowanie zastosowania GALILEO z VANET (GLOVE) (Galileo Integrated Optimization with VANET Enhancements - GLOVE), J. Nawrocki (157) EDEN - End-user driver Demo for cbrNe (EDEN), J. Ryzenko (163)

122

ESA Grants

 Realizacja fazy C/D i E projektu systemu pozycjonowania MPOI eksperymentu MERTIS w ramach misji BEPI COLOMBO (Realisation of chase C/D and E of the Project of the MERTIS POInting Unit (MPOI) for BEPI COLOMBO mission), M. Rataj (18)  PSU MXGS/ASIM faza C/D (Atmosphere-Space Interactions Monitor (ASIM) Phase C & D), (subcontract), P. Orleański (65)  Interfejs użytkownika oraz ogólna koncepcja softwerowego symulatora Italian Spring Accelerometer dla misji kosmicznej BepiColombo (User interface and general topology concept for the software simulator of Italian Spring Accelerometer for BepiColombo mission), M. Kalarus (103)  Dopasowanie polskiego systemu monitoringu i prognozy wybranych elementów pogody kosmicznej do ESA (Architecture of Space Weather Situation Awarness - SSA), I. Stanisławska (115)  Opracowanie metody wykorzystania satelitarnych obserwacji Ziemi w optymalnym z punktu widzenia środowiska rozmieszczeniu źródeł energii odnawialnej na przykładzie upraw roślin biopaliwowych, (Implementation of remote sensing data and models In optimizing the localization of renewable energy sources on the example of biofuel crops with respect to ecological constraints), S. Lewiński (123)  STIX Wczesna Faza C (Polish Technical Participation in early C of STIX /Solar Orbiter Project), P. Orleański (137)  Penetrator typu KRET z bezpośrednim napędem elektromagnetycznym (EMOLE), (Mole penetrator driven by an electromagnetic direct drive (EMOLE), J. Grygorczuk (138)  Krzepkie, nienadzorowane wizualne rozpoznawanie ruchu niekooperacyjnego satelity do przechwytywania na orbicie - OBSERVER (Robust, unsupervised Visual motion recognition of non- cooperative satellite for on-orbit capture - OBSERVER), subcontract, T. Rybus (147)  SACC - Satelitarny adaptacyjny kanał komunikacyjny (SACC – Satellite Adaptive Communication Cannel), subcontract, M. Stolarski (158)  Analiza przeniesienia procedur SCOS-2000 na platformę 64B (Study of the migration to 64-BITS of SCOS-2000), subcontract GMV Innovating Solutions, Sp. z o.o., M. Michalska (165)  Ultralekka wiertnica rdzeniowa przeznaczona do eksploracji Księżyca (Ultra light drilling rig for planetary exploration), subcontract AGH, K. Seweryn (168)  Opracowanie konstrukcji opartych na nanokompozytach polimerowych aktywnych w polu elektrycznym (Development of structures based on polimer nanocomposites active for electrical stimulation), J. Grygorczuk (170)  Zintegrowane środowisko geoinformacyjne na potrzeby zarządzania kryzysowego i koordynacji działań (Space-derived Geoinformation for Crisis management and Coordination –GECCO), subcontract, A. Foks-Ryznar (176)  Multikonstelacyjne, multiczęstotliwościowe, multisystemowe oprogramowanie do transferu czasu za pomocą systemów nawigacji satelitarnej (Multi-Costellation, Multi-Frequency, Multi-Signal GNSS Time Transfer Software- MuSTT), subcontract, J. Nawrocki (177)

123

EU Structural Funds Grants

 Zintegrowany mobilny system wspomagający działania antyterrorystyczne i antykryzysowe – PROTEUS (Integrated Mobile System for Counterterrorism and Rescue Operations), A. Foks-Ryznar (30)  Ochrona technologii kosmicznych poprzez zgłoszenia patentowe kluczowych wynalazków z dziedziny mechatroniki i robotyki kosmicznej (Patent protection of space technology key inventions in the field of space mechatronics and robotics), M. Wachowicz (161)

National Science Centre Grants

 Porównanie skal czasu przy pomocy pomiaru fazy sygnałów GNS z sub-nanosekundową precyzją (Time scale comparison with the use of GNSS phase signals with sub-nanosecond precision), P. Lejba (76)  Multifraktalna analiza zobrazowań satelitarnych (Multifractal analysis of satellite images), A. Wawrzaszek (77)  Co widzi IBEX - próba interpretacji pierwszych wyników z Interstellar Boundary Explorer (What does IBEX see + attempt to interpret first observations from Interstellar Boundary Explorer), M. Bzowski, (78)  Analiza zjawisk nieliniowych w środowisku kosmicznym (Analysis of Nonlinear Phenomena in the Space Environment), W. Macek (81)  Wyznaczenie parametrów sprężystości Ziemi na podstawie laserowych obserwacji satelitarnych SLR (Determination of the Earth's elasticity parameters using satellite laser ranging (SLR) observations), M. Rutkowska (91)  Badania ruchów własnych Laboratorium Geodynamicznego w Książu przy pomocy techniki GPS w celu zastosowania we wspólnej interpretacji z rejestrowanymi sygnałami geodynamicznymi (Research of station movements of Geodynamic Laboratory in Książ using GPS technique for employment in common interpretation with registered geodynamic signals), R. Zdunek (92)  Wyznaczanie i analiza pozycji i prędkości wszystkich stacji laserowych z 30 lat obserwacji satelitów LAGEOS (Determination and analysis of the positions and velocities of the all SLR stations from 30 years of the LAGEOS satellites observations), S. Schillak (93)  Wyznaczenie i analiza funkcji pobudzenia ruchu bieguna na podstawie obserwacji grawimetrycznych misji satelitarnych GRACE oraz dostępnych modeli hydrosfery lądowej kalibrowanych przez obserwacje satelitarne misji GOCE (Determination and analyses of polar motion excitation function based on gravimetric observations from the GRACE satellite mission and land hydrosphere models calibrated by gravimetric observations from the GOCE satellite mission), J. Nastula, (94)  Badanie elektrodynamicznych związków górnej atmosfery z jonosferą i magnetosferą – TARANIS (TARANIS Project - strategy of experiment and development of instruments), P. Orleański (95)  Określenie i zbadanie nowych charakterystyk modelowania stanu pogody jonosferycznej i ich eksperymentalne testy i aplikacje (Elaboration of new characteristics for space weather modelling – tests and applications), I. Stanisławska (111)

124

 Badanie warunków fizycznych w strukturach korony słonecznej na podstawie analizy ich promieniowania rentgenowskiego (Examination of the physical conditions in the structures of the solar corona on the basis of their X-ray radiation), B. Sylwester (113)  Analiza zmian pola elektrycznego o częstotliwościach z zakresu ELF nad obszarami silnych trzęsień Ziemi (Analysis of changes in the electric field in the ELF range over seismic active regions), M. Kościesza (116)  Wielkie bombardowanie w Układzie Słonecznym: kratery uderzeniowe, problem dostarczania substancji lotnych (Late Heavy Bombardment: Cratering and Volatile Delivery), H. Rickman (117)  Satelitarna ocena zachmurzenia nad Polską wraz z szacunkiem atmosferycznych strumieni promieniowania (Satellite Cloud Climatology over Poland with Atmospheric Radiation Fluxes Estimation), A. Kotarba (128)  Badanie struktur nieliniowych i procesów przyspieszania cząstek w otoczeniu ziemskiej fali uderzeniowej (Investigation of nonlinear structures and acceleration processes in plasma and the bow shock), K. Stasiewicz (139)  Detekcja Sztucznych powierzchni nieprzepuszczalnych z zastosowaniem obrazów satelitarnych zawierających pokrywę śnieżną (Artificial Impervious Surface detection with Snow-featured satellite imagery - ArtISS), A. Kotarba (141)  Modelowanie nieregularnych zmian ruchu obrotowego Ziemi z wykorzystaniem geodezyjnych wyznaczeń parametrów orientacji przestrzennej planety oraz najnowszych modeli geofizycznych (Modelling irregular changes in Earth rotation by the use of geodetic determinations of spatial orientation and recent geophysical models), A. Brzeziński (142)  Polski udział w misji kosmicznej NASA Interstellar Boundary Exploret (IBEX): astronomia atomów neutralnych (Polish participation in the NASA space mission interstellar Boundary Exploret (IBEX): astronomy of neutral atoms), M. Bzowski (143)  RESONANCE - badanie fundamentalnych procesów w plaźmie okołoziemskiej, multi punktowa nowatorska metoda diagnostyki pól elektromagnetycznych (RESONANCE – Fundamental study of physical processes In near Earth’s space plasma, an innovative method of multipoint diagnostics of electromagnetic fields), H. Rothkaehl (162)  Synteza metod sterowania adaptacyjnego dla układów z dynamiczną stabilizacją położenia – robot typu ballbot (Synthesis of adaptive control methods for and under actuated dynamically stable mobile robot - ballbot type), Ł. Wisniewski (167)  Instrument CHOMIK misji Phobos Sample Return – badania naukowe i eksploracyjne (CHOMK Instrument for the Phobos sample return mission – scientific and exploratory research), J. Grygorczuk (97)  ChemiX: opracowanie założeń naukowych i konstrukcji (faza B) nowego spektrografu Bragga na misję międzyplanetarną Interhelioprobe – IHPM (ChemiX: formulation of the science goals and construction design (phase B) of the new Bragg spectrophotometer for the Interhelioprobe interplanetary mission – IHPM), M. Siarkowski (112))  Retgenowski spektrometr obrazujący STIX: zdefiniowanie szczegółowych celów naukowych i sposobu prowadzenia obserwacji na podstawie modelowania matematycznego przyrządu oraz jego

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systemu testującego (X-ray imaging flare spectrometer STIX: definition of detailed science operation modes based on results of numerical modeling of its expected response and its dedicated test unit), J. Sylwester (114)  Realizacja fazy przygotowawczej projektu "Cherenkov Telescope Array" przez Polskie Konsorcjum CTA (Realization of the preparatory phase of the “Cherenkov Telescope Array” project by the Polish CTA Consortium), K. Seweryn (120)  Misja Herschel/HIFI – badanie wody w atmosferach planet i komet (HIFI/Herschel mission – studies of water in the atmospheres of planets and comets), S. Szutowicz

National Centre for Research and Development Grants

 Modelowanie propagacji i rozpraszania sygnałów elektromagnetycznych w przestrzeni okołoziemskiej metodami analizy nieliniowej, fraktalnej i frakcjalnej (Modelling of propagation and scattering of electromagnetic signals in space around Earth using nonlinear analysis methods, fractal and fractional), B. Atamaniuk (88)  Opracowanie i budowa prototypu manipulatora satelitarnego jako kluczowego elementu orbitalnych systemów sewisujących – LIDER (Design and construction of the satellite manipulator prototype as a key element of on-orbit servicing systems-LIDER), K. Seweryn (102)  Spektralno-obrazujacy system do zdalnych pomiarów z wykorzystaniem statku powietrznego (Spectro-imaging system for remote sensing measurements from aircraft), M. Rataj (125)  Specjalistyczne hybrydowe łożyska toczne do zastosowania w przemyśle kosmicznym – ROLOKOS (Specialized hybrid rolling bearings for use in the space – ROLOKOS), J. Grygorczuk (129)  Opracowanie modelu automatycznej wiertnicy rdzeniowej do pracy w ekstremalnych warunkach, w szczególności w środowisku kosmicznym (Development of the automatic core grill working in extreme conditions, especially space environment), K. Seweryn (133)  Dystrybucja wzorcowych sygnałów czasu i częstotliwości w optycznych sieciach telekomunikacyjnych (Distribution of precise time and frequency signals in telecommunication optical network), J. Nawrocki (148)  Komercjalizacja Kosmosu – przygotowanie Centrum Badań Kosmicznych PAN do utworzenia, prowadzenia i rozwoju spółki celowej, SPIN-TECH (Commercialization process in Space Research Centre Polish Academy of Sciences – preparing the Institute to establish, maintain and develop the SPV), M. Wachowicz (169)  Nowe, zaawansowane materiały warstwowe Al-Ti o podwyższonej odporności balistycznej na konstrukcje lotnicze i kosmiczne (Modern, advanced composite materials AI-Ti of heightened ballistic resistance intended for aerospace structures), J. Grygorczuk (174)

Ministry of Science and Higher Education Grants

 Badania z udziałem ludzi i automatów w środowisku kosmicznym – eHEROES (Environment for Human Exploration and Robotic Experimentation in Space), J. Sylwester (121)

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 Tworzenie baz danych procesów dla celów eksploracji jonosfery – POP-DAT (POP-DAT - Problem-oriented Processing and Database Creation for Ionosphere Exploration), H. Rothkaehl (124)  Europejski Projekt Lewitującej Magnetycznie Sfery Reakcyjnej dla Systemów Kontroli Orientacji – ELSA (European Levitated Spherical Actuator ELSA), R. Wawrzaszek (131),  Poszerzenie Systemu EGNOS na Wschód - Aplikacje (EEGS2) (EGNOS Extension to Eastern Europe – Applications (EEGS2)), J.B. Zieliński (134)  Turbulencja plazmy Układu Słonecznego: obserwacje, intermitencja i multifraktalne (Solar system plasma Turbulence: Observations, inteRmittency and Multifractals – STORM), W. Macek (149)  ESPAS - infrastruktura danych z najbliższego otoczenia Ziemi dla e-Science (ESPAS - Near-Earth Space Data Infrastructure for e-Science), I. Stanisławska (160)  Zastosowanie systemów eksploatacji i analizy obrazów i informacji geoprzestrzennych we wsparciu działań zewnętrznych Unii Europejskiej G-SEXTANT (Service provision of geospatial intelligence in EU external action suport - G_SEXTANT), S. Lewiński (172)  GMES przedoperacyjne serwisy bezpieczeństwa dla wsparcia działań zewnętrznych Unii Europejskiej G-NEXT (GMES- pre-operational security services for supporting external action/ G-NEXT), S. Lewiński (173)  Obserwacje Ziemi czynnikiem stymulującym wzrost gospodarczy – EOPOWER (EOPOWER – Earth Observation for Economic Empowerment), S. Lewiński (178)

Other Grants

 Ortorektyfikacja zdjęć radarowych RADARSAT-2 (Orthorectification of RADARSAT-2 images), E. Woźniak (181)  Budowa Polskich stacji europejskiego interferometru radiowego LOFAR (Polish LOFAR action – subcontract), H. Rothkaehl (166)  BRITE: Pierwszy Polski Satelita (BRITE: First Polish Scientific Satellite), T. Zawistowski (71)  Opracowanie i wykonanie testów termicznych instrumentu STIX STM (Imager i DEM) - STIX- TT (Thermal tests of The STIX STM (Imager and DEM) - STIX-TT), K. Seweryn (153)  Symulator softwarowy Champ LCU (Champ LCU Software Simulator), M. Michalska (159)  Wykonanie elementów mechanicznych napędu dla HP3 MOLE (Offer to manufacture mechanical parts for The HP3 MOLE drive), R. Przybyła (171),  Analiza układu optycznego dla stanowiska laboratoryjnego pomiarów spektralnych (Analysis of The optical system for The laboratory spectra measurements), P. Wawer (175)  Techniczna obsługa stacji EGNOS – RIMS (Technical operations of The EGNOS system – RIMS), L. Jaworski (13)  Jonosonda LAERT (LAERT Ionosonde), H. Rothkaehl (68)  Jonosonda Olsztyn (Olsztyn Ionosonde), M. Pożoga (150)

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 Raport o występowaniu pokrywy śnieżnej w pasie linii kolejowej E-20 od Sochaczewa do Swarzędza (The report on the occurrence of snow cover in the E-20 railway line from Sochaczew to Swarzędz), A. Kotarba (154)  Wektoryzacja pokrycia i zagospodarowania terenów zalewowych w miastach nad Odrą (Vectorization of the land cover and land use of flood areas in the cities on the Odra river), S. Lewiński (155)  Świadczenie usług informatycznych dla projektu SatAgro.pl – nowatorska platforma umożliwiająca monitoring terenów rolnych przy wykorzystaniu automatycznie przetworzonych danych satelitarnych (IT services for SatAgto.pl - an innovative Internet platform for the monitoring of agricultural lands using automatically processed satellite data), S. Lewiński (164)  Dostarczanie danych obserwacyjnych GPS, pochodzących ze stacji referencyjnej BOR1 znajdującej się w Borowcu (GPS data service from Borowiec), M. Lehmann (7)  Dostarczanie danych obserwacyjnych GPS, pochodzących ze stacji referencyjnej WLAD znajdującej się we Władysławowie (GPS data service from Władysławowo), R. Zdunek (8)  Bieżące opracowanie zestawu danych heliogeofizycznych do prognozowania warunków łączności radiowej oraz rozwój metodyki i systemów prognozowania warunków łączności radiowej (Space weather forecasting for radio wave transmissions – data analysis and development of new methods and systems), B. Dziak-Jankowska (67)  Wyrównanie podstawowej osnowy wysokościowej I i II klasy na obszarze kraju w europejskim układzie odniesienia EVRF2007 (Adjustment of the I and II order of The fundamental levelling Network of The Poland In European verdical reference Frome EVRF2007), L. Jaworski (179)  Analiza objętości wskazanych hałd i kierunków spływów na podstawie numerycznego modelu terenu (Analysis of volume and run-off of mine waste dumps), E. Woźniak (180)  Rekonfigurowane, oparte o struktury FPGA, systemy przetwarzania sygnałów wykorzystywane w satelitarnych systemach wysokiej niezawodności (Reprogrammable systems for Signac transformation based on FPGA structures, designer for use In satellite systems of high reliability), P. Orleański (6)  Układ Elektroniczny pre-EM Attenuator Electronics i jego model STM (STIX STM pre – EM Attenuator Electronics), K. Skup (140) Analiza i projektowanie radaru bistatycznego dla projektu Fantina B.Assert System (Analysis and design communication radar system for Fantina B/Assert System – bistatic radar), M. Stolarski (144)

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GENERAL INFORMATION

Staff

At the end of 2013 the Space Research Centre employed 191 persons of whom 15 professors, 13 habilitated doctors and 38 PhD research associates. ANNA FOKS-RYZNR and MAŁGORZATA WIŃSKA were advanced with PhD degree. STANISŁAW SCHILLAK received professor title from the President of the Polish Republic.

(Halina Żurek)

Finances – preliminary estimates

The state budget of Space Research Centre in 2013 was 6 236 thousand PLN while total was 18 179 thousand PLN. The budget structure was following: basic allocation – 31%, national grants – 32%, EU framework projects – 5%, contracts (national and international, PECS) – 28%, other sources – 4%.

(Wioletta Roszkowska)

Grants and Contracts

In the Space Research Centre 100 projects including 9 from the Ministry of Science and Higher Education, 25 from the National Science Centre, 8 from the National Centre for Research and Development, 14 from ESA, 14 from EU Framework Programme and 2 including funded by the EU Structural Funds, and 21 other grants.

(Anna Kamińska)

Intellectual Rights Management Policy

CBK PAN develops and implements Intellectual Rights Management Policy, specially executing tasks of two main projects concerning IPR in CBK PAN. The first one "Protection of space technology through key patent inventions in the field of mechatronics and robotics space" implemented under the Operational Programme Innovative Economy 2007-2013 provides the patent protection applications in Poland for selected space robotic and mechatronics inventions and protecting inventions abroad, in Europe and USA. Already, in 2013, 7 European and polish patent applications (mechatronics an robotics inventions) have been made. The aim of the project is to use the intellectual potential of CBK PAN to implement developed technologies for space industry and terrestrial applications. Intellectual property strategy will contribute to more efficient commercialization process in CBK PAN on the European market and will accelerate the building process of the space industry sector in Poland. Implicitly, the project will increase significantly the patent protection of Polish companies in the space sector and thus enable to equal opportunities in competition with foreign space entities. The institute aims to identify, report, secure, and deploy patents, copyrights, and trademarks consistent with CBK PAN’s mission of research and technology development. The second project “Commercialization 129 process in CBK PAN - preparing the Institute to establish, maintain and develop the SPV” financed by NCBR, prepares the Institute for the efficient commercialization of science, in particular, by building a portfolio of products in CBK PAN and by implementing various business strategies, taking into account the valuation of IP for the selected products and technologies.

(Marta Wachowicz)

Awards

Dr. Marcin Stolarski took first place in the popular science competition FameLab 2013 at national level and he was in the finale at the international level. The idea of the contest this consists in providing complex scientific issues in a manner accessible to each recipient.

Activities inside and outside of Poland

1. Specialist from The Space Research Center SRC of Polish Science Academy took part in creating a “Program of Activities designed for the development of cosmic technologies and satellite systems in Poland”. The program was presented to the Polish government and to the Ministry of Economy. The Council of Ministers agreed on it in June 2012. The program states conditions needed for effective use of these technologies in Poland:  full membership in European Space Agency (ESA),  creating Polish Space Agency,  launching National Program of Cosmic Activity,  intensifying Polish participation in European Space Policy and European Defence Agency.

2. In the context of Polish membership in ESA The Space Research Centre PAN approached the Ministry of Science with a proposal, supported by many universities, to create a new discipline: Cosmic and Satellite Engineering in the field of Polish Technical Sciences and to promote specialist in this field as it becomes essential need in our economy.

3. Together with government institutions (National Centre of Emergency Management) the Centre started working over creating The Centre of Satellite Information about natural disasters.

4. SRC organized meetings with the representatives of polish industry to introduce them to possibilities and ways of joining the cooperation with European cosmic industry under contracts of European Space Agency.

5. SRC carries out 4 contracts of scientific collaboration with foreign partners; without a formal agreement the centre works with circa 250 scientific institutions; collaboration with foreign agencies focuses on around 130 research subjects.

6. In 2013 Centre’s employees organized and co-organized 12 scientific conferences, out of which 8 were international (STIX Team Meeting 15-19.04.2013, 16-17.10.2013; VII Meeting of the Polish- Russian Group of the Executive in the field of basic space research 20-25.10.2013, Warszawa, Wrocław, XVI Consultations on Solar Physics 22-25.05.2013, Wrocław II Conference on Aerospace Robotics (CARO) 1-2.07.2013, Warszawa, EOPOWER Networking - Polish – Ukrainian Meeting 5.09.2013, Warszawa, Late Heavy Bombardment in the Solar System 23- 26.06.2013, Kraków EChO Payload Consortium Meeting 10-12.06.2013, Warszawa

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7. In 2013 Centre’s employees took part in 79 international conferences. Many of them were directly involved in organisation of particular sessions.

8. Centre’s employees took part in meetings with representatives of institutes and institutions, domestic and foreign companies interested in cooperation and the promotion of scientific and business application of SRC.

9. SRCs employees in 2013 submitted 7 polish and 1 international patents.

10. Institute’s employees were actively involved in laboratory work, diagnostic stations and observatories operating within the Centre structures:  RIMS station of EGNOS system (Warsaw) – permanent GNSS observation for the purpose of creating EGNOS correction;  JONOSONDA (Warsaw) – monitoring the ionosphere over Warsaw for the purposes of telecommunication and navigation;  Service of Time and Frequency - (Astrogeodynamic Observatory in Borowiec) –AOS Borowiec time distribution on the Internet; providing master frequency for POLKOMTEL S.A.;  BOR1 station (Astrogeodynamic Observatory in Borowiec) – permanent GPS observations; station working in IGS, EPN and ASG-EUPOS structures; data used to determine a global reference system ITRF, regional regional development in Europe, and to define the national spatial reference system;  CBKA station (Warsaw)– permanent GPS observations for national network ASG-EUPOS; used for the purpose of calculating precise RTK corrections for the system users; station defines the national spatial reference system;  Mobile GNSS Laboratory – examining accuracy and quality of EGNOS corrections in the field;  Presence on the Polish Polar Station HORNSUND – local monitoring of conditions in the space around the Earth using: ionosond, GPS receiver and receivers to measure the absorption;  Regional Warning Centre Warsaw – branch of International Space Environment Service (ISES);  International forecasting centre for cosmic weather;  IDCE (Ionospheric Dispatch Centre in Europe) – European centre for gathering and distribution of ionospheric data;  GWAR station – permanent GPS and GALILEO observations; station working in experimental network of stations tracking GALILEO system;

11. The Center is part of 14 scientific networks:  AirClim-Net; 2002; problems of air pollution and climate change; http://www.airclim-net.eu/;  “Polish Research Network of Global Geodetic Observation System” GGOS-PL; 2011; integrates the activities of observatories operating in the GGOS-PL. The subject of the network is the basic scientific research, application and implementation activities of innovation and development in the field of research related to the monitoring of the Earth's atmosphere, including, in particular, those associated with a) the extension of the observation base, b) the integration of satellite and ground-based observing techniques; coordinator of the network is the University of Environmental and Life Sciences in Wroclaw; the network also includes:

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University of Warmia and Mazury in Olsztyn, Institute of Geodesy and Cartography, Warsaw University of Technology, Military University of Technology and the University of Science and Technology;  COST ES0803; 2011; cosmic weather, http://w3.cost.esf.org/index.php?id=205&action_number=ES0803;  COST MP1104; 2011; cosmic weather, telecommunication, http://www.cost.esf.org/domains_actions/mpns/Actions/MP1104?management;  ISMN TUWIEN; 2007; international cooperation to establish and maintain a global database of ground soil moisture, http://www.ipf.tuwien.ac.at/insitu/;  Polish network of the project „Cherenkov Telescope Array”; 2007; astronomy research of gamma radiation;  SWEX; 2010; Earth observation in the hydrological range of conditions;  Geoinformation Systems; 2006; geoinformation infrastucutre and the electronic library supporting the spatial research on environmental and socio-economic development, spatial analysis methodology and geovisualization of the results of these analyses;  ESSEM COST Action ES1001; 2012; the use of SMOS observations in the seas and oceans, lead by UPC  International Laser Ranging Service; 1997; coordination of satellite and lunar stations, analytic centres, banks of laser technique databases; 42 laser stations, 29 analytic station, 2 banks of database http://ilrs.gsfc.nasa.gov/about/news/index.html;  Satellite Geophysics; 2005; satellite geophysics;  National Centre for Space Engineering and Satellite; 2013  HECOLS; 2013; astronomy, astrophysics, cosmology, stars, solar system;  Polish Research Network Global Geodetic Observation System "GGOS-PL; 2011 Scientific research, innovation and Implementation in the field of development studies related to the monitoring of the Earth; and 36 scientific consortia:  "geoland2" - Consortium for the FP7 Collaborative Project; 2007 r.; remote sensing, geophysics;  AeroFast; 2009; satellite technologies;  BRIDGES; 2011; for the BRIDGES project, analysis of management models for GMESin teh field of cosmic policy;  BRITE PL; 2009; building Polish Satellite; astroseismology, satellite technologies;  BRITE; 2005; astronomy;  Discorsi Galilei; 2007; subjects connected with the project of European satellite system Galileo;

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 EEGS; 2009; expanding EGNOS system for East Europe;  eHEROES; 2011; examining the influence of cosmic “conditions” on equipment and human functioning;  ELSA; 2010; for the realization of the project connected with creating the prototype of “reaction sphere” in a form of a sphere levitating in a magnetic field, which can be set in rotating motion in any direction;  ESPAS; 2011; integration of e-science data in space;  EUROLAS; 1989; coordination or observatory and research of satellite laser measuring; all European laser stations EUROLAS Data Centre, EUROLAS Analysis Centre;  GeoPlanet; 2011; geophysics, oceanography, geology, space physics;  GLOVE; 2012; implementation of dynamic network of synchronization vehicles on the move;  G-mosaic; 2008; use of photos taken by satellites for the safety purposes;  Herschel Solar System Observations; 200T; the atmosphere of planets and comets; observation program on cosmic telescope Herschel: Water and related Chemistry in the Solar System- A Guaranteed Time Key Program;  ISMN; 2011; ISMN http://www.ipf.tuwien.ac.at/insitu/ is a global network of SMOS support lead by TUWIEN, it leads a global bank of SM ground data (Soil Moisture). Their main activity focuses on taking part in conferences connected with EGU2011 and EGU2012, providing and updating SM data to the bank of ISMN;  JEM-EUOS; 2007 r.; astronomy, geophysics, satellite technologies;  Consortium for the implementation of the project “Developing the model of automatic drill core for working in extreme conditions, especially in space environment”; 2012;  Consortium for the implementation of the project “Developing the method of using the satellite Earth’s observations in an optimal, from the point of view of environmental requirements, deployment of renewable energy sources on the example of biofuel plants”; 2012;  Consortium for the implementation of the project „Ultralight drilling rig for planetary exploration”; 2013;  Consortium for the implementation of the project “Solar system plasma turbulence: observations, intermittency and multifractals – STORM”; 2012;  Consortium for the application and implementation of the project “Spektral-imagining system for remote measurements using aircraft” for the Ist contest of PBS; 2012.; satellite technologies;  Lunar Net; 2010; implementation of project Lunar Net for the call for medium sized missions in ESA's Science Programme for launch in 2022;  MUPUS; 2005; space technology;  National Centre of Radioastronomy and Engineering; 2012; technical science, space exploitation, transfer, dating processing and radioastronomy;

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 OPTIME; 2012; distribution of master signals of time and frequency in the optical networks of telecommunication webs;  POLFAR; 2010; radioastronomy and space physics;  Polish Consortium of Project "Cherenkov Telescope Array" 2009; astrophysics of gamma radiation of the highest energies;  POPDAT; 2012; promoting cosmic research http://www.popdat.org/index.php/about-popdat/consortium;  PROTEUS; 2008; automatics, satellite navigation;  Radio & Plasma Waves Investigation Consortium – JUICE; 2011; preparing equipment for the ESA JUICE mission and development of related scientific issues;  STIX for Solar Orbiter; 2006; X-ray examination of the Sun;  SVRT (SMOS Validation and Retrieval Team); 2005; study the Earth's ground environment;  SWEX; 2005; environmental studies;  Virtual Institute for Sustainable Agriculture 2003; activities for sustainable agriculture;  Consortium for the implementation of the project ”The study mechatrinics of modern tectonic events using the new measurement methodology and instruments Lab.Geod. CBK in Książu” 2013;  SMOS-MODE ESSEM ES1001; Action SMOS-MODE COST ESSEM ES1001 for integration Oceanographic EO SMOS gobal http://www.cost.eu/domains_actions/essem/Actions/ES1001; http://www.cost.eu/domains_actions/essem/Actions/ES1001?parties.

(Anna Kamińska)

Educational and promotional activity

 There were 26 students in the Doctoral Studies in Space Research Centre in 2013, and 4 new students were admitted in 2010;  SRC cooperates with universities and high schools in student training 71 students had their practice in SRC;  56 Centre employees lead classes with students in 24 universities and other national and foreign institutions;  employees took part in expert sessions of Polish Sejm, Ministry of Economy and European Space Agency; helped establish space policy, direction of research and the scope of application for polish organization;  SRC employees' participation in the work of an advisory body of the European Space Agency ESA - European Space Weather Working Team;  SRC employees' participation in national and international Union of Radio Science URSI; 134

 participation of SRC’s employees in international science organizations;  SRC employees participation in PAN science committees, institutes’ science councils;  co-organization of 4th Space Conference in Sieradz “Poland in the European Space Agency. Earth observations” (8-9.10.2013) and also an accompanying contest for high school students;  XVIth edition of Science Festival in Warsaw (21-22.09.2013) – lectures and popular science talks, conducting created by the centre workshop;  participation in 18th Science Picnic of Polish Radio and Copernicus Science Centre (15.06.2013 Warszawa) – positionwith observations of the spectrum of the Sun, the presentation of geodynamic phenomena on the basis of research conducted at the Laboratory Geodynamicznym in Książu, photo interpretation of satellite imagery high distribution - an interactive quiz, participation in shows;  Interactive Picnic of Knowledge “The Day of Explorers” in Rzeszów (7.08.2013);  Polish edition of ,,Scientist for a Day" contest (contest was dedicated to kids and teenagers, December 2012/January 2013) - SRC employee was a jury in NASA contest organized in Poland under the auspieces of SRC;  involvement in Europlanet activiy for cosmos popularization;  4th Cosmic conference in Sieradz (8-9.10.2013) – preparing questions for a teenage Contest, popular-science lectures;  XIIth School Astronomic Workshops (25.09.2013) – popular science lecture;  Regional Competition in physics and astronomy for students of middle and primary schools in 2013 (11.03.2013) - SRC employee was a chairman of the jury; a competition has been organized for many years in cooperation with the Marshal of the Kuyavian- Pomeranian province.  Contest of cosmic knowledge for high school youth:– participation of SRC worker in the work of the jury;  organization of events related to the location on the orbit of the first Polish scientific satellite BRITE-PL "Lem; 21.11.2013;  15th Dolnośląski Festival of Science (21.09.2013) - employees of SRC PAN conducted workshops for children and popular scientific lectures, demonstrations, organization of exhibitions; happening;  Cosmic Press Review – press and online review, general and specialist, dedicated to cosmos research. (http://biblio.cbk.waw.pl/pliki/prasa.html);  Facebook CBK PAN – internet social portal helping promote SRC PAN. (http://www.facebook.com/CentrumBadanKosmicznychPAN);  media about SRC PAN –located on the SRC PAN Library online list of publications which are being published in media (press, radio, TV, internet) about SRC (http://biblio.cbk.waw.pl/pliki/prasa%20o%20nas.html);

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 campaign "Send a photo into space" – organized by Spółdzielnia „Fajna Sztuka”; campaign’s main focus was to promote the start of polish satellites Lem and Hevelius (7-31.01. 2013);.  Active and permanent involvement of the SRC employees in interviews, TV and radio broadcasts.  AstroNautilus - CBK employee worked as editor in chief of Poland's only popular science magazine devoted to the exploration of space;  Cassini Scientist for a Day, December 2013 – polish competition organized by the NASA /ESA;  a series of meetings of experts, organized by the Planetarium Copernicus Science Centre - a lecture by CBK employee;  SRC employers participated in followings events (popular-science lectures and speeches): - days of space explorers, 25.05.2013, Warszawa - Day of Science 18.05. 2013 - Elektronik 2013, 18.04.2013 - Event organized in Zespole Szkól technicznych w Ostrowie Wielkopolskim; - Kopernikalia 2013, 22.02.2013 - Picnic with comets,4.05.2014, Świeradów Zdrój - Night in the the Aviation Institute, 18.10.2013, Warszawa - National Astronomy Meeting, OSA2013,28.08.2013 - Children's University, 20.04.2013 - Summary Climate Summit, 28.11.2013 - School Workshops in Astronomy, 14-17.05.2013 Szklarska Poręba - Days of Science in Kórnik, 23-24.05.2013 - Meetings of astronomy in LO No. XIII,13.06.2013, Wrocław - VIII Astronomical Day in IPCN, 28.09.2013, Świeradów Zdrój - VIII National Meeting of the Astronomical IZERY’2013, 30.08.2013 - III Summer School of Polish branch EAAE, 10.07.2013, - Youth Observatory, Niepołomice - IV Conference Space in Sieradz, 8-9.10.2013 – work in jury in the National Competition Knowledge about Space "Poland in the European Space Agency. Observations of the Earth";  European Space Expo, 4-9.05.2013 – exhibition presents the two largest space programs - Galileo (satellite navigation on) and Copernicus ( observations of the Earth);  II Robots Night PIAP, 24.05.2013 – demonstrations of instruments built by the Laboratory of Mechatronics and Robotics Satellite SRC;  IV Forum of Innovation in Rzeszów, 14-15.05.2013;  EDUSCIENCE project – participation of workers from SRC Observatory in Borówiec in popularizing the project "Raising student competence in the field of mathematics and natural sciences and engineering using innovative methods and technologies – EDUSCIENCE". The project is co-funded by the European Union;  Involvement SRC to edition second stamp in series devoted to Polish scientific satellites.

(Maria Miłodrowska, Zenona Sawicka)

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Some press releases on SRC PAS activity in 2013

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CONTENTS

03 ...... ACHIEVEMENTS 2013

05 ...... SPACE PROJECTS

20 ...... DATA ACQUISITION

27 ...... INTERPRETATION AND MODELING

76 ...... APPLICATIONS

99 ...... DATA EXPLORATION AND DISSEMINATION

103 ...... SPACE MECHATRONICS AND ROBOTICS

112 ...... PUBLICATIONS

122 ...... GRANTS AND CONTRACTS

129 ...... GENERAL INFORMATION

Cover: ZENONA SAWICKA

Edited by: MAŁGORZATA TOMASIK KRZYSZTOF ZIOŁKOWSKI

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

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