SPACE RESEARCH CENTRE

2008

POLISH ACADEMY OF SCIENCES

ANNUAL REPORT

WARSAW

SPACE RESEARCH CENTREPolish Academy of Sciences

Bartycka 18A, 00-716 Warsaw, PolandPhone: (48-22) 840 37 66

Fax: (48-22) 840 31 31e-mail: cbk@cbk.waw.pl

SUMMARY 2008

The year 2008 was, for many reasons, significant for Space Research Centre. We have proved our engineering and scientific competence in space experiments by contribution to the payload and the software of two space missions launched in 2008, Chandrayaan-1 and IBEX.

The Indian Chandrayaan-1 mission to the Moon, launched on October 22, 2008 carries the sophisticated near-infrared spectrometer SIR-2 (financed by ESA and Max-Planck Society), for which Polish engineers were contracted to design and manufacture the power supply system and the housekeeping system. The instrument was successfully commissioned on the orbit and is actually providing detailed mineralogical maps of the Moon surface.

The NASA mission IBEX (Interstellar Boundary Explorer, launched on October 19, 2008) is a first attempt to directly measure fluxes of interstellar neutral hydrogen passing through the solar system. The SRC team has written a number of packages of the data processing software for determining the composition of the local interstellar medium surrounding our solar system.

In 2008, another two space missions were in the last phase of preparation to their launches, the Russian Koronas-Photon and the ESA Herschel.

The Koronas-Photon solar observatory payload (launched on 30 January 2009) includes the SphinX instrument built in the SRC Solar Physics Division in Wroc³aw. The instrument will measure the soft X-ray radiation emitted by the solar corona. Data obtained from the instrument will enable the scientists to determine the abundances of elements in the corona as well as to measure in the soft X-ray range how the Sun luminosity varies during the solar cycle. The mission started its observations in the period of very low solar activity with a relatively small number of X-ray generating solar flares, but soon the activity should increase to a level warranting flare activity strong and frequent enough to precisely find out abundances of argon, calcium, iron, and nickel.

The ESA Herschel mission will be launched in April 2009. SRC participated in building the HIFI instrument, the most sensitive infrared heterodyne system ever launched in space, designed to collect long-wavelength infrared radiation from some of the coolest and most distant objects in the Universe. During 2008 the maintenance process was sustained of the flight model of HIFI Local Oscillator Control Unit designed and built by SRC engineers.

SRC has been very active in carrying out the existing and acquiring new research projects. In total, 88 projects are now carried out, with 31 grants from the Ministry of Science, 10 SPUBs (Special Research Projects to support international cooperation), 23 foreign as well as 24 national contracts. The scientific output comprises 290 publications, out of which 54 are papers in the JCR-listed journals. More than 180 presentations were delivered at the conferences (19 invited). In 2008, the Scientific Council of SRC awarded our researchers with one PhD and two Doctor Habilitatus scientific degrees.

Three main international events organized with participation of SRC include:th16 International Workshop on Laser Ranging organized in Poznañ by the Astrogeodynamic

Obserwatory of SRC (located in Borowiec near Poznañ) that gathered almost 150 participants from all around the world (20 countries were represented). Altogether more than 120 papers were presented;The Heliophysics SRC branch in Wroc³aw has organized two workshops, STIX-SphinX event and Coronas-Photon & SphinX workshop that were attended by altogether 60 researchers who presented about 60 talks; The SRC co-organized Polish Science Days in Russia and together with the Space Research Institute RAS prepared an exhibition illustrating 30 year long cooperation in space between Polish and Russian institutes and the seminar for young scientists in St. Petersburg.

3

The main achievements of SRC in 2008, selected for this Summary, are:Scientific support of the NASA IBEX mission: The SRC team led by doc. dr hab. Maciej Bzowski (IBEX co-I) has prepared detailed numerical simulations on the IBEX's instrument response to the flux of interstellar neutral deuterium. The simulations have proved that due to radiation pressure effect the neutral deuterium is lost at a much slower rate than the neutral hydrogen. This will, most probably, enable to detect directly the neutral deuter of the interstellar origin for the first time. The predicted best season for such measurements was found to be February – March.Interesting effects in the motion of a small Earth-approaching asteroid 2002 AA29 have been discovered in the course of numerical simulations by Mr Pawe³ Wajer, PhD student working under supervision of prof. Grzegorz Sitarski. The asteroid becomes from time to time a temporary Earth satellite. Its motion followed in a long time interval shows a number of peculiarities that are also evidenced in another, recently discovered asteroid 2009 BD. The trajectory of the latter shows several encounters (collisions) with the Earth, but the firm conclusion cannot yet be drawn because of not too precisely determined initial condition.Successful participation of SRC as a subcontractor in building the near-infrared spectrometer SIR-2 on the Indian Chandrayaan-1 mission to the Moon. The team led by Dr Piotr Orleañski cooperated in this project with collegues from the University of Bergen, Norway. The instrument works on the orbit as planned and is providing data for detailed geological studies of lunar surface.

JÓZEF JUCHNIEWICZ (1944-2008)

Dr. Józef JUCHNIEWICZ suddenly passed away on 21 December 2008. The Space Research Centre unexpectedly has lost one of the most distinguished staff

members and a dear colleague.

4

SPACE PROJECTS

BepiColombo

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 2019 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 dominated by its magnetic field. Space Research Centre is involved in the MPO-MERTIS experiment.

In the frame of the project titled "The pointing system for orienting of a measure-ment direction of the MERTIS spectrometer of the BepiColombo mission for spectral measurements of the Mercury surface and calibration" following tasks were performed in 2008: the Development Model 1 was designed and manufactured, functional and thermal tests were carried out using two types of the Electronic Ground Support Equipment’s (one based on Geisler board for simulation FPGA behaviour and a clasical one for environmental tests) developed for this model. Basing on results of tests the Development Model 2 was designed and is under manufacturing. (P. Orleañski, M. Rataj)

Cross-section of the MERTIS Pointing Unit

Chandrayaan-1

5

Chandrayaan-1 is an Indian Space Research Organisation (ISRO) mission (with ESA participation) that will study the Moon in great detail. Using a wide range of electromagnetic wavelengths, it will analyse the lunar surface as well as its crust in high resolution, so as to gain a deeper understanding of the origin, evolution and composition of Earth's only natural satellite. The mission will also drop a lunar probe onto the surface, to test the properties of the surface upon impact. Chandrayaan-1 was successfully launched on 22 October 2008 from the Satish Dhawan Space Center in Sriharikota, India, using ISRO's four-stage PSLV launch rocket.

In the frame of India/ESA Chandrayaan-1 Project to the Moon the IR spectrometer SIR-2 has been designed and manufactured in MPS/Lindau, University of Bergen and Space Research Centre of PAS. SIR-2 uses a linear InGaAs photodiode array (900 to 2550 nm). It

has 256 pixels with a pixel pitch of 50 micrometers. The SIR-2 detector is clocked with frequencies up to 1.5 MHz and the analogue signal is converted with 16-bits resolution. A two-stage cooling system consisting of the detector's thermoelectric

Coronas-Photon

The Coronas is the Russian program for studying the solar physics and solar-terrestrial relations using a series of satellites that provides for three solar-oriented spacecraft to be placed on the near-earth orbit. The Coronas-Photon, third spacecraft of this series, was successfully launched on 30 January 2009. Two previous missions of the Program are Coronas-I (launched on 2 March 1994) and Coronas-F (launched on 31 July 2001). The Coronas-Photon is designed to investigate the processes of energy accumulation and transformation into the accelerated particle energy during solar flares, to study the acceleration mechanisms, propagation and interaction of high-energy particles in the solar atmosphere, and to study the correlation of the solar activity with physical-chemical processes in the Earth's upper atmosphere.

In the Space Research Centre, an X-ray PIN (Si) spectrophotometer has been deve-loped, along with spectral analysis methods allowing for diagnostics as regards the elemental composition of hot (million– degree) plasmas. Such plasmas are abundant in the coronae of stars like the Sun, as well as in the controlled thermonuclear reactions (Toka-maks). Our SphinX X-ray spectrophotometer was launched aboard the Coronas-Photon satellite, in order to study solar spectra in the range 0 – 12 keV with a resolution of 300 eV. Measured spectra will be used to determine the composition of coronal plasma for elements between Mg and Ni. For the first time the measurement's absolute accuracy will be better than 5%. The analysis will yield new information of importance to solar physics. The measurement and analysis methods can easily be adapted for investigations of laboratory hot plasma. The SphinX instru-ment will be taking measurements of solar X-ray spectra between 2009 and 2014, i.e. during the rise phase of solar activity cycle 24.

Over this period, we expect to collect ~200 GB of data. We will investigate the abundance variability (discovered by us using X-ray spectroscopy methods) with the in situ abun-dance measurements of the solar plasma taken from other satellites.

In 2008, the SphinX Project was in its third year of development. Hardware development was concentrated on the Flight Model (FM) of the instrument. A lot of construction, testing and programming work has been accom-plished including the end-to- end tests and

cooler (TEC) and a passive radiation system is implemented. Digital part of the instrument bases on LEON processor IP core implemented into Actel anti-fuse FPGA. SRC was responsible for delivery of 10W Power Supply Unit (PSU), the Programmable Current Source for IR detector cooler and the House-keeping System. The maintenance of the Flight Model of PSU Unit has been performed during the whole year of 2008.

(P. Orleañski)

6

SphinX FM has been delivered to Russia and mounted on the Coronas-Photon satellite payload ( launch on 30 January 2009).

In a view of a possible future experimental opportunities, a prototype of a compact digital X-ray spectrometer has been developed based on FPGA technology. The unit has been tested using specially designed software.

(J. Sylwester)

absolute calibration performed at the BESSY synchrotron in Berlin. Development of the flight on-board software has been accom-plished as well as the related software of the EGSE unit used in various ground tests of the instrument. The most important were the interface tests at the FIAN, Moscow, where SphinX has been connected to his “mother” instrument TESIS.

Herschel

Exploring formation of stars and galaxies, ESA's Herschel space observatory will give astronomers their best view yet of the universe at far-infrared and sub-millimetre wavelengths, bridging the gap in the spectrum between what can be observed from ground and earlier space missions of this kind. Herschel will be launched in 2009 on an Ariane-5 rocket. In less than six months, Herschel will reach its operational orbit around a point in space known as the second Lagrangian point (L2), situated at 1.5 million kilometres away from the Earth. Herschel has been designed to perform routine science operations for a minimum of 3 years at L2. The mission will end when the helium used to cool the focal plane of the scientific instruments is depleted. Space Research Centre is involved in the HIFI experiment.

In the frame of ESA Herschel Project HIFI (Heterodyne Instrument for Far Infrared) the Space Research Centre collaborates with Max Planck Institute of Radioastronomy in Bonn, JPL in Pasadena and COM DEV in Toronto. The consortium manufactures the program-mable microwave source (Local Oscillator) working up to 2000 GHz. SRC is responsible of delivering about 100 Watts secondary power spread among of more than 120 different, floating and programmable rails. The rails supply the 30 GHz synthesizer, microwave amplifiers and bias the microwave multipliers in 14 frequency bands (chains). 80C32 microcontroller, 32KBytes of RAM, 16 Kbytes of PROM and RTX54SX32S FPGA from Actel are used in digital block. The software implemented in our unit, written in Assem-bler, controls the safety operations of the

whole Local Oscillator Subsystem and, by this, fulfills one of the most critical and difficult tasks in HIFI. In addition, more than 180 analogue channels are monitored by our system with 12 bits resolution, some of them are used internally in Local Oscillator for self checking, the others are distributed to Herschel telemetry system. The 15 kg Local Oscillator Control Unit (LCU) presents fully redundant system designed according to ESA requirements.

The flight model of LCU has been delivered to Herschel Consortium and the integration with satellite started in EADS Astrium in Friedrichshafen in 2007. During the year of 2008, the maintenance of the Flight Model of the unit was performed by SRC team. (P. Orleañski)

7

IBEX

The IBEX mission was successfully launched from the Kwajalein Atoll in the Pacific Ocean on October 19th, 2008. After some time necessary for the final stabilization of the orbit (high inclination, highly elliptic type, with the apogee of 50 Earth radii) and the commissioning phase operations, the first scientific data should be delivered to the ISOC (IBEX Science Operation Center), beginning from the middle of January, 2009.IBEX (Interstellar Boundary Explorer) is a two-year NASA Small Explorer heliospheric mission to study the interactions of the solar wind colliding with the inflowing interstellar matter. IBEX will be the first spacecraft to image and map dynamic processes taking place in the outer solar system in the region known as the heliospheric interface.

Earth and Moon visisbility in the Star Sensor FOV

(2008 Dec 01 12:00:00 - 2009 Jan 08 00:00:00)

-90

-70

-50

-30

-10

10

30

50

70

90

0 48 96 144 192 240 288 336 384 432

Number of time periods from 2008 Dec 01 12:00:00 (1 period=2h)

Ele

va

tio

n(S

/Cc

oo

rd.s

ys

tem

)[d

eg

] Moon trajectoryEarth trajectory

2008 Dec 01 12:00:00 2009 Jan 08 00:00:00

Star Sensor FOV

(-5.0 - +3.5 deg)

IBEX perigee

IBEX orbit No 9 IBEX orbit No 10

Fig.1 Earth and Moon visibility in the Star Sensor FOV (2008 Dec 01 – 2009 Jan 08)

In the frame of the cooperation between the Space Research Centre group and the IBEX project scientific team, two packages of the simulation programs were developed and delivered to ISOC center.

The first (engineering) software packet from SRC is designed to simulate the Star Sensor output signal during the IBEX mission and to predict the experiment conditions (fig. 1). The Star Sensor unit is an element of the IBEX-Lo neutral atom detector instrument

and is designed to specify with the fine accuracy the spin axis of the IBEX spacecraft. This task will be carried out with the use of a software packet which is able to determine the positions in the spacecraft coordinate system of the scanned stars obtained from the IBEX telemetry data (fig. 2). The basis for the position determination is a sub-catalog of the SAO star catalog which includes (~10000) stars with the brightness greater then 6.5 magnitude.

8

9

The second (scientific) software packet is designed to calculate the transmission function of the energetic neutral atoms (hydrogen and oxygen), i.e. to determine their energy change and survival probability within the heliospheric environ-ment between the termina-tion shock and the IBEX detectors. (M. H³ond, M. Bzowski)

Fig.2 Scanned stars position and the IBEX spin axis determining process.

International Space Station

The aim of the Obstanovka experiment on board of the International Space Station (ISS) station is to monitor and diagnose the electromagnetic radiation and property of plasma around station, simultaneously in two different localizations, to enable to study the near-Earth plasma interactions and for appli-cation purposes in space technologies. To achieve these goals the Plasma-Wave Complex (PWC) was designed and constructed by the scientific group from Bulgaria, Hungary, Poland, Russia, Sweden, UK, Ukraine. The Radio Frequency Analyzer (RFA) has been

Obstanovka

developed jointly by the Space Research Centre in Warsaw and the Swedish Institute of Space Physics (IRF) in Uppsala. New digital technology of this instrument creates an excellent possibility for monitoring the electromagnetic emissions in space and time domain. During 2008, the flight models of the electric and magnetic antennas were integra-ted. Both antennas are stowed and they will be deployed to the measurement configuration in space. (J. Juchniewicz, H. Rothkaehl, M. Morawski,

J. Grygorczuk)

ASIM

The Atmosphere-Space Interactions Moni-tor (ASIM) aboard ISS is proposed for the study of high-altitude optical emissions from the stratosphere and mesosphere related to thunderstorms. One of the two main ASIM in-struments is Miniature-X and Gamma-ray

Sensor (MXGS) designed by the University of Bergen and University of Valencia, in cooperation with Space Research Centre in Warsaw. SRC is responsible for the design and manufacture of the Power Supply Unit and an autonomous (FPGA based) Housekeeping

10

System. During 2008, the complete docu-mentation for the Science Requirements Review and the Preliminary Design Review was completed. The first model of MXGS PSU has been manufactured. The model has been tested in SRC ( in stand alone configuration) and in Bergen University (together with dete-ctor unit).

(P. Orleañski)

Rosetta

International Rosetta Mission is a Cornerstone Mission in ESA's Science Programme; its destination is the short-period comet 67P/Churyumov-Gerasimenko. Rosetta was launched on 2 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.

The Rosetta lander is provided by a European consortium under the leadership of the German Aerospace Research Institute (DLR). The 100-kilogram lander carries a payload consisting of experiments that analyse drilled samples and the surface, sound the plasma and magnetosphere environment, sound the deep interior, study dust production and sedimentation, and take images at different wavelengths and with different fields of view. Three experiments focus on physical pro-perties of the near-surface layers. MUPUS (Multi-Purpose Sensors for Surface and Sub-surface Science) is the only experiment package that penetrates the near-surface layers of the target comet and measures physical properties in situ. Using MUPUS data, we will be able to describe the uppermost 40 cm of a comet in terms of density, porosity, cohesion, thermal diffusivity and conductivity, and temperature variations. The Space Research Centre is res-ponsible for mechanical and electronic engi-neering and manufacturing of the MUPUS penetrator (including thermal sensors and densitometer), the MUPUS main electronics, and the flight software.

The Rosetta spacecraft has performed a successful close fly-by at main-belt asteroid (2867) Steins, which belongs to the rare class of E-type asteroids that had not been directly observed by an interplanetary spacecraft before. The fly-by started on 4 August 2008 with optical navigation on the asteroid itself. This technique was used for the first time in the history of ESA spacecraft operations. Rosetta had its closest approach to the asteroid on 5 September 2008, 18:58:19 UTC, when (2867) Steins was at distances of 2.14 AU from the Sun and 2.41 AU from the Earth. The spacecraft encountered it with a relative velocity of 8.62 km/s and reached a minimum distance of 800 ± 3 km.

Hans Rickman, being in charge of the OSIRIS Coma Working Group of the Rosetta science team, organized a two days WG meeting (in May 2008) at the Space Research Center, where more than 10 WG members from USA, Taiwan, Germany, Spain, Italy, France and Sweden participated. Intense and fruitful discussions were held, leading to a new list of prioritized observing projects that will serve as preliminary input to the central Rosetta planning activities.

DATA ACQUISITION

The Astrogeodynamical Observatory in Borowiec

The Observatory is involved in the following projects:- laser tracking of satellites,- positioning measurements by means of GPS technology in global geodynamic programs,- satellite synchronisation of time and development of measurement technologies.

Satellite Laser Ranging Station

The Satellite Laser Ranging station at Borowiec (7811) in the framework of the International Laser Ranging Service (ILRS) and EUROLAS Consortium performed 208 successful passes (81428 normal points) of 16 SLR satellites in 2008. The mean normal point precision of the all passes was at a level of 3 mm, accuracy 20 mm. The results of observations were sent in the near real time to EUROLAS Data Center and Crustal Dynamics Data Information System NASA. The data of the Borowiec SLR station supported scientific programs of the observed satellites and were used for orbits calculations by ESA, NASA and many other institutions and international organizations. The activity of the Borowiec SLR station was limited in 2008 by significant modernization of the hardware and software of the SLR system. The modernization of the Borowiec SLR system included the following tasks:

· instalation the microchannel PMT HAMAMATSU R5916U-64-3MCP with fotocathode gating system,

· tests of the new PMT-MCP,· adjustment of the constant fraction

discriminator TENNELEC TC-454,· formatting the triggering pulse of the

epoch registration,· tests of the two transmitting telescopes,

11

· determination of the telescope model errors,

· installation of the Event Timer A032-ET with the corresponding software,

· introduction of new procedures in the software of the main control program.

The GPS and SLR station positions and velocities in the period 1993.0-2004.0 were determined in the frame of the orbital analysis tasks in 2008. The calculations were performed for first day of each month in ITRF2005 reference frame. The results show a good agreememt of positions (several mm) and velocities (below 1 mm/year) for both satellite techniques. The significant differences (2-3 cm) were detected in the vertical component of position for several stations. The deter-mination of SLR station positions and velocities from LEO satellites Starlette, Stella and Ajisai and determination of coordinates of Champ and Larets satellites were continued. The significant disturbances on the quality of the satellite positions are from the Earth gravity field model, the atmospheric drag and the frequency of the empirical accelerations determination. The orbital RMS of the satellites was in the range from 1 cm to 6 cm depending on the satellite, the station stabilities were on the level 1-2 cm.

(S. Schillak)

12

BOR 1 station

The GNSS (GPS) and assosiated meteo data are given on the official web site: http:// orchid.cbk.poznan.pl/~bor1. The data stre-ams from BOR1 station are available by IGS-IP and EUREF-IP projects, too.

The permanent GPS station located at Borowiec and known as BOR1 has been integrated with EUREF network since 1996. BOR1 station delivers high quality and outstanding international reputation data. BOR1 makes a valuable contribution to 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: Center for Orbit Deter-mination Europe, Bern (Switzerland), GFZ – IGS Processing Centre, (Germany), JPL – IGS/FLYNN Processing Centre, Pasadena (USA), Massachutets Institute of Technology, and Scripps Institution of Oceanography (USA).

(M. Lehmann)

Time and Frequency Service

In 2008, the work at Time and Frequency Laboratory concentrated on development of time base of the Laboratory. The ensemble of clocks consists now of two hydrogen masers:- CH1-75A, developed by the Institute of Electronic Measurements “Kvarz”, at present the master clock of the Observatory source of UTC(AOS),- American Symmetricom SigmaTau, and two cesium time frequency standards HP-5071A opt. 001 also from Symmetricom. The new en-semble of clocks allows for the realization of UTC(AOS) within the range of +/- 10 ns from UTC.

International comparisons of atomic time scales are from the end of 2006 based on Two Way Satellite Time and Frequency Transfer TWSTFT ) method, which assures uncer-

tainty of the measurements in the range of 200 ps. This method allows to use fully the stability of the new H-maser. In 2007, the TWSTFT equipment was calibrated using timing GPS observations carried at the Observatory. The satellite simulator (SatSim) installed in 2008 enables control of the equipment delay changes at the picosecond level .

New receivers, the TTS-4 observing GPS, GLONASS, and Galileo satellites were developed at the end of 2008. The receivers are equipped with 116 channels and carry on observations at GPS L1, GPS L2/L2C, GPS L5, Galileo E1/E5A, GLONASS L1/L2. Applied is the ionosphere-free P3 method for clock comparisons. The receivers also supply in real time the data in RINEX format.

The laboratory was completely moder-nized: - The clocks are now working in specially air conditioned chamber with temperature sta-bility of 0.1 deg C. Stability of temperature and humidity (3%) allows utilization of full performances of the new clocks. All of them participate in TAI and TA(PL) . - All measuring and distributing time and frequency equipment was also moved to the new laboratory, also air-conditioned, impro-ving the accuracy of measurements.

Work on the Precise Timing Facility (PTF) for Galileo has passed from the design phase to realization. From March 2008 AOS team started to write final version of the software in ANSI C language. The work is carried on: - Two Way Management Software for PTF of Galileo Control Station;- GPS Common View Management software for PTF Galileo Control Station;- Galileo Common View Management soft-ware for PTF Galileo Control Station;- special algorithms developed for the esti-mation and prediction of the Galileo-GPS time offset (to be broadcasted by the Galileo satellites);- special algorithms developed for the esti-mation and prediction of the PTF1 –PTF2

13

The Geodynamic Laboratory in Ksi¹¿

The most important scientific results obtained in 2008 are following:- elaboration of five years long series of plumb line variations observed using the long water tube tiltmeter in 2003 to 2007. These series were results of measurements obtained on four ends of the tube with the help of four interference measurement units. Such mea-surements allow for applying differentiation of the signals from opposite ends of the tubes. Application of differential method causes decreasing of errors and simultaneously increasing of geodynamic signal as well as the reduction of the instrumental drift.- determination of non-tidal signal of plumb line variations in years 2003 to 2007;

time offset (differences of time scales between the two Galileo control centres, Master and Slave).The Laboratory continues:- realization and development of Polish Ato-

mic Time Scale – now about 16 atomic clocks

from Polish laboratories, Lithuania, and Latvia;- participation in the realization of UTC and TAI in cooperation with the BIPM in Sevres;- Baltic Time Project (6th Framework Prog-

ram)– development of international time stam-

ping – in cooperation with Lithuania, Estonia,

Latvia, Ireland and Italy. Application of inter-

national time stamping is tested between Poland (AOS) and Lithuania (NSI).- Realization of the Harrison Project (6th Framework Program) has been finished (Dec. 2008). Harrison aimed at application of Galileo for precise time and frequency services, as well as legal applications of Galileo Time. Most promising users are in astronomy (photon datation, interferometry), quantum cryptography, power and energy sector, synchronization in Communication Data Networks, mobile cellular network synchro-nization of base, financial and banking appli-cations, time reference for secure applications.

(J. Nawrocki)

In 2008, in the Geodynamic Laboratory of SRC in Ksi¹¿ there were led permanent observations of variations of the Earth’s gravity field, its strength and its direction. The following instruments were applied: relative gravimeter LaCoste&Romberg G-648 and tiltmeters: long water tube, and quartz horizontal pendulums. Simultaneously with measurements of parameters of gravity field there were carried out permanent measure-ments of temperature, humidity and pressure variations in surroundings of the instruments.

New TTS-4 receiver with touch-control screen

GNSS Observatory in Warsaw

14

The observatory is involved in the following projects:- EGNOS navigation system,- monitoring the quality of EGNOS

corrections in cooperation with ESA in IMAGE/PERFECT and ESA/ESTEC EXPERT projects,

- positioning measurements and defining the national reference frame with GPS techno-logy,In Warsaw there is located one of the RIMS

(Ranging and Integrity Monitoring Station) stations of the EGNOS system designed to broadcast the embedded correction signals in Europe for providing the improved perfor-mance in positioning with GPS. Besides operating RIMS station SRC cooperates with Polish and European institutions in RD activity related to EGNOS System. Most interesting activities arefollowing:

· participation in ESA IMAGE/ PER-FECT Project,

· participation in ESA/ESTEC EX-PERT Project,

· dynamic tests of the system using Mobile GNSS Laboratory,

Results from these experiments show changes of accuracy of the EGNOS corrections dependent on the temporary constellation of GPS satellites.

IMAGE is a project that was launched in 2002 by ESA GNSS-1 EGNOS Project Office (EPO) with the objective that independent Signal In Space monitoring activities are performed as EGNOS is progressively deployed and verified prior to Operational Readiness Review. Part of IMAGE project to provide continuous, near -rea l t ime information on EGNOS key performance values is called PERFECT (PERformance-website For EGNOS Continuous Tracking). It consists of a network of monitoring stations continuously tracking GPS satellites and EGNOS corrections. Every hour results are

- elimination of local effects such as tempe-rature, pressure, and humidity variations as reasons of non-tidal signals of plumb line varia-tions with the help of permanent measure-ments of temperature, pressure, and humidity variations in the underground of the Labo-ratory; - first comparison between the non-tidal signals observed with the help of quartz pendu-lums and by the long water-tube tiltmeters;-construction of hypothesis of tectonic motions as the cause of non-tidal signals of plumb line variations;- preliminary elaboration of yearly series of measurements (2007-2008) of gravity varia-tions carried out with the help of gravimeter LaCoste&Romberg G-648;- preliminary determination (in the frame of tasks of KBN Project no. 4 T12E 011 28) of Love's numbers h and k. For calculation of Love's numbers the series of gravity and plumb line variations measurements were applied (results have been presented in the final report of the Project);- preliminary elaboration of yearly series of measurements (2008) of plumb line variations measured with the help of quartz horizontal pendulums equipped with new system of electronic registration;- construction, tests, and initiation of the functional model of the interference extenso-meter (in the frame of KBN Project no. 4 T12 E 011 28 ); - realization in April 2008 of the precise leveling in the Geodynamic Laboratory in Ksiaz, including the determination of the second derivative of the gravity above the pillar for absolute gravity measurements;- realization of the third session of absolute measurements on the pillar in the under-ground chamber of the Laboratory in April 2008; the session was made with the help of absolute gravimeters FG5 belonging to the Institute of Geodesy of Warsaw University of Technology. (M. Kaczorowski)

Poland (ASG-PL), is working in Warsaw. In December 2007, the CBKA station was included in ASG–EUPOS project. The main goal of the ASG-EUPOS calibration campaign was:

· to determine 3D precise coordinates of all GNSS antennas installed on ASG-EUPOS reference stations and to connect ASG-EUPOS network and include it to the existing primary national geodetic network, defined by EUREF-POL, POLREF and EUVN points;

· to perform test measurements in order to create on Polish territory the homo-geneous geodetic network in ETRS'89 system and to verify coordinates accuracies of all ASG-EUPOS perma-nent reference stations;

· to test of ASG-EUPOS reference stations operation as well as the whole system functioning basing on selected points of the primary national GPS networks: EUREF-POL, POLREF and EUVN.

In order to realize this work, special consortium was created. All tasks concerned with the campaign were made since April 11 till May 31, 2008 but observation sessions were performed since April 23 to May 11, 2008 (114 – 131 DOY). SRC took part in field work and was responsible for analysing and processing GPS data using the Bernese GPS Software ver. 5.0 in Double Difference mode, with IERS and IGS conventions for geophysical models and parameters.

(L. Jaworski)

sent to Web Server. Space Research Centre started to participate in PERFECT project at the end of June 2005. Equipment used for this purposes consists of:

· Septentrio PolaRx2 GPS/EGNOS receiver,

· PC with RxControl software to rece-iver control and WebUpdate Software to analysis of the observation and transferring results to Web Server.

The EXPERT (Extension of PErfect Real Time) Network is a joint initiative of ESA EGNOS Project Office and ESA ESTEC to widen the horizons of the ESA PERFECT Network. This project works in a similar way as the PERFECT project, but for EGNOS monitoring the standard commercial one-frequency receivers are used. The EXPERT receiver shows also the accuracy variation of the EGNOS corrections for Warsaw station.

In addition to continuous static moni-toring, some periodic dynamic tests were performed. Mobile GNSS Laboratory is equipped with different class receivers:

· Precise geodetic, dual frequency receivers: Trimble 5700 and SPS850, Septentrio PolaRx2,

· Navigation receivers: CSI, Magellan and Garmin.

For the tests, route with minimal obstruction in horizon was selected. Results for most tests show improving of the horizontal and vertical accuracy for GPS with EGNOS corrections versus mere GPS observations.

Starting from February 2003 the GPS permanent station (CBKA), integrated with pilot project Active Geodetic Network for

15

INTERPRETATION AND MODELLING

SPACE PHYSICS

Solar physics

The analysis of spectra observed with the RESIK spectrometer in the spectral range 3.3 – 6.1 Å have been in progress. In particular the algorithm has been implemented which allows to eliminate the additional emission in chan-nels 3 and 4 of the instrument. This emission has been associated with the contribution of fluorescence coming from Al crystal supports. In correcting the spectra for this effect a semi-empirical method has been used.

A new method has been worked out allowing for the simultaneous determinations of the chemical composition of emitting plasma and its distribution with the tempe-rature (as described using the differential emis-sion measure, DEM). This method is based on the examination of the absolute fluxes observed in the line and continuum. The method has been adopted into the analysis of spectra of individual flares as well as the “quiet” (i.e. non-flaring) corona.

We have found that the chemical compo-sition of flaring plasma differs from standard photospheric as well as from the coronal values available in the literature. For the non-flaring conditions the abundances of Ar, S and Si have been determined only as the lines coming from other elements were too weak. Based on the analysis of RESIK spectra it follows that the coronal abundance of Ar is higher than presently adopted coronal value, being rather independent of the overall activity level. The Si abundance is found however lower than photospheric. Determined S abundances are becoming systematically lower with decre-asing level of overall coronal activity; S abundance is three times smaller for A9-B1 in comparison with B4-B5 activity level. As concerns DEM, the results indicate for prevalence of two-component character of plasma distributions with temperature as well for solar flares as for the quiet corona.

The performed analysis unveiled the existence of small amount of hotter (T~8 MK) plasma in the emitting volume even for the lowest (A9) analysed activity level. The maximum temperatures of the cooler (T < 5 MK) and hotter (5 MK < T < 12 MK) compo-nents, the relative amount of cooler and hotter plasma and their thermodynamic measures (characterising thermal energy content) de-pend on the level of solar activity in a regular way. Total amount of hotter plasma is three orders of magnitude smaller than the amount of cooler plasma. The other direction of analysis based on RESIK spectra was the investigation of possible presence of the non-maxwellian electron distributions in the emitting region. With this aim the spectra from the wavelength region 5.15 – 5.95 Å (channel 4) have been investigated. For a pair of selected flares it has been shown that the observed, rather high relative intensities of the satellite lines respective to parent emission lines can be explained provided the non-maxwellian electron distribution is assumed. (B. Sylwester, J. Sylwester)

16

We continued (together with R. Falewicz and P. Rudawy) the detailed analysis of the energy balance of individual solar flares using MHD numerical code. We investigated the influence of the variations of energy spectrum of non-thermal electrons on observed GOES class of flares. We have found that keeping fixed total energy delivered by non-thermal electrons and appropriately changing the spectral index and low energy cut-off of the non-thermal electrons spectra results in signi-ficant changes in the observed GOES class of the induced solar flare. This has to do with the fact that the low-energy fraction of the electrons heats the chromosphere most effectively. The results were presented on COSPAR meeting and sent for publication in Astronomy and Astrophysics.

We have also simulated the formation of a helium-like triplet CaXIX spectra during process of chromospheric evaporation in order

to compare with observations from Yohkoh satellite. The results were presented on COSPAR and 12th European Solar Physics Meeting. (M. Siarkowski)

Deuterium is a special element in the Universe. Chemically identical with hydro-gen, it was created during Big Bang and since then – as the only element – has only been destroyed by astration. By studying the abundance of deuterium with respect to hydrogen, scientists can determine the ratio of barion density to the mean density of the Universe. Up to now, investigation of deuterium in the Milky Way has been carried out by spectroscopic observations and results were unequivocal. In a paper published recently in Astronomy & Astrophysics by Tarnopolski and Bzowski, a new method of determination of the density of deuterium in the Local Cloud of interstellar gas, surro-unding the Sun, was proposed: direct in situ detection of neutral atoms of deuterium, approaching the Sun from the interstellar space. Tarnopolski and Bzowski showed that because of processes operating inside the heliosphere, in particular of the solar radiation pressure, which modifies trajectories of deuterium atoms in a different way than those of hydrogen atoms, deuterium atoms should suffer smaller losses than hydrogen, so its abundance with respect to hydrogen and bulk velocity should be increasing with a decreasing distance from the Sun and the flux of interstellar deuterium atoms should exceed the lower detectability limit of an instrument onboard the planned NASA SMEX mission IBEX. Tarnopolski and Bzowski predict that the best time during the year for IBEX to search for interstellar deuterium will be from the end of January until the end of March. (S. Tarnopolski, M. Bzowski)

17

Heliosphere

The most important results in magneto-hydrodynamic simulations of the heliosphere (published in the Geophysical Research Letters and presented at the AGU Fall Meeting in San Francisco) are:1) Estimation of the orientation and strength

of the local interstellar magnetic field inferred from Voyagers' positions.

2) Development of our 3D MHD code by a) improving boundary conditions, b) more reallistic simulation of the solar wind: taking into account inclination of the solar rotation axis to the ecliptic pole axis, and slow and fast solar wind regions.

3) Analysis of the influence of the solar wind latitudinal asymmetries and the presence of the interplanetary magnetic field on the shape of the heliosphere termination shock.

4) Comparison of simulation results obtained from our 3D MHD model without magnetic fields, and with/without con-stant flux of neutral hydrogen, with results of several multi-component hydro-dynamic heliosphere models presented by Mueller et al. (2008).

(R. Ratkiewicz, J. Grygorczuk)

The aim of our study is to examine the question of scaling properties of intermittent turbulence in the space environment. We analyze time series of velocities of the slow and fast speed streams of the solar wind measured in situ by Helios 2, Advanced Composition Explorer and Voyager 2 spacecraft in the inner and outer heliosphere during solar minimum and maximum at various distances from the Sun. To quantify scaling of solar wind turbulence, we consider the generalized Cantor set with two different scales describing nonuniform distribution of the kinetic energy flux between cascading eddies of various sizes. We investigate the multifractal characteristics (generalized dimensions and singularity spec-tra) depending on two rescaling parameters

18

and one probability measure parameter. We demonstrate that the universal shape of the multifractal spectrum resulting from the multiscale nature of the cascade is often rather asymmetric. Moreover, we observe the evolution of multifractal scaling of the solar wind in the inner and outer heliosphere. It is worth noting that for the model with two different scaling parameters a much better agreement with the solar wind data is obtained, especially for the negative index of the gene-ralized dimensions.

(W. Macek, A. Szczepaniak)

The Markov processes theory has been applied to the description of the turbulent cascade in the solar wind. Computer software has been developed for the verification of the Markovian character for experimental time series and computations of the drift and diffusion coefficients of the Fokker-Planck equation. The software has been applied for analysis of data from Ulysses and ACE spacecraft experiments. Obtained results suggest Markovian character of the turbulent cascade in the solar wind. Obtained equations can be applied for modelling the probability distributions for turbulent fluctuations. Results of the studies are important for the description of the transport processes in the turbulent cascade in the solar wind. (M. Strumik)

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 sometimes registered in the polar cusp as emissions with extremely high intensity below the electron cyclotron frequency by Interball 1. They correlate with strong fluxes of high energetic electrons often 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 emis-

Ionospheric and magnetospheric physics

sions. The observations of the waves at the frequencies close to electron cyclotron frequency done by Cluster satellites associated with strong fluxes of energetic electrons will be presented. Taking into account the plasma and magnetic field parameters in the polar cusp as well as geometry of the waves propagation, one has 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 particles flux and hea-ting the plasma.

(J. B³êcki)

The analysis of the low frequency fluctu-ations of the magnetic and electric fields prior to a strong earthquake with magnitude M ≈7.8 on May 12, 2008 in Sichuan province has been done. We analyzed the disturbances of the ionospheric electromagnetic field 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. Although the mechanism of the energy transmission from the earthquake preparation zone to the ionosphere is not determined, it can be said that the ionospheric plasma is an unstable medium and that even a small pertur-bation can lead to variations of the electro-magnetic field and plasma parameters. Some attempts of this discussion is given in the paper. 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. (J. B³êcki)

The observation of ELF and VLF signature of sprites recorded on the low altitude satellite DEMETER during thunderstorm activity has been analyzed. At an altitude of ~ 700 km,

19

waves observed on the E-field spectrograms at mid-to-low latitudes during night time are

+mainly dominated by up-going O whistlers. During the night of July 20, 2007 two sprites have been observed around 20:10:08 UTC from the observatory located on the top of the mountain Œnie¿ka in Poland (50°44' 09'' N, 15°44' 21'' E, H = 1603 m) while ELF and VLF data have been recorded by the satellite at about 1200 km from the region of thunder-storm activity. During this event, the DEMETER instruments were switched in the burst mode and it was possible to register the wave forms. It is shown that the two sprites have been triggered by two intense +CG lightning strokes (100 kA) occurring during the same millisecond but not at the same location. Despite the distance DEMETER has recorded at the same time intense and unusual ELF and VLF emissions. The whistler wave propagates from the thunderstorm regions in the Earth-ionosphere guide and enters in the ionosphere below the satellite. They last several tens of milliseconds and the amplitude of the ELF waveform is close to 1 mV/m. A particularly intense proton whistler is also associated with these emissions. After the occurrence of the sprites, the non-detection by the lightning networks of a whistler observed by DEME-TER reveals the persistence of an in-cloud dis-charge activity.

(J. B³êcki)

These parameters are used to study the morphology of scintillation. Slight increase of the scintillation activity is observed in spring and early summer. As far as diurnal variations are concerned, two maxima are observed, around 9 and 21 UT, which correspond to the magnetic noon and midnight, respectively. Besides statistical parameters, GISTM provides the raw amplitude and phase sampled at a 50 Hz rate. The spaced receiver analysis of raw data is used to estimate the diffraction pattern, drift, and anisotropy. Preliminary results indicate a strong variability of the drift velocity and its dependence on the irregularities scale size. All presented results refer to a low solar activity conditions.

(A. Wernik)

Since September 2007 amplitude and phase scintillations of GPS signals are recorded at the Polish Polar Station at Hornsund, Spitsbergen (77 N, 15.55 E, invariant latitude 73.4). The location of the Station enable us to study the scintillations in the auroral zone as well as in the dayside cusp and, partly, the polar cap region. Three antenna and GISTM (GPS Ionospheric and TEC Monitor) receivers have been installed in the apexes of a triangle with two sides, approximately 100 m long, oriented along magnetic north-south and east-west. GISTM outputs every minute the scintillation index S4, phase standard deviation, and TEC.

Several algorithms for disperssion analysis of the ionospheric experiment MISTECS have been elaborated:1. Highpass filtering adapted to desired

boundary condition;2. Drift estimation methods based on Radon

transform of cross-spcectrum phase histo-grams;

3. Identification of drift in the time domain for nonstationary signals.

(M. Grzesiak)

A new interpolation method called Adap-tive Normalised Convolution was imple-mented to ionospheric data. I wrote programs and numerical codes based on the ANC method. Many program testing, debugging and fault detections was performed. The code was applied to generate maps of the new magnetic

index h and the ionospheric parameters foE and h'E. The main goal was to find the spatial correlation between high values of the

magnetic index h and the changes in the E layer of the ionosphere in time of very low magnetic index Kp.

(B. Dziak-Jankowska)

Wave polarization is a key feature in under-standing the auroral kilometric radiation (AKR). There is a general view that the AKR

20

AKR pulsations at frequencies 1 to 4 Hz, typical for Pc1 geomagnetic pulsations, were observed from four Cluster spacecraft (years 2001-2005). Fourteen of them occurred in a recovery phase of a strong magnetic storm. Event of 22 June 2003 was studied in more details. Positive frequency drifts of the AKR pulses are interpreted as a result of the earthward motion of AKR sources along auroral magnetic field lines. The determined source velocities match velocities characte-ristic for propagation of shear Alfven waves within the auroral cavity. Proposed scenario identifies inertial Alfven waves converted either from electromagnetic ion cyclotron waves generated in the equatorial magneto-sphere, or from electromagnetic ion cyclotron waves generated in the auroral cavity, as the primary cause of the AKR pulsations. Parallel electric field produced by earthward propa-gating Alfven wave can periodically modify the 'shell' electron distribution, believed to be the free energy source of the AKR pulse emission through the electron-cyclotron maser instability. Results were published in Geophysical Research Letters (2008).

(J. Hanasz, R. Schreiber)

polarization is fully circular with dominating right-hand extraordinary mode and some admixture of the left-hand ordinary mode. Most of up-to-date determinations of the wave modes of the AKR have been based on measurements of the circular component of the wave polarization, leaving the linear polarization parameters unknown. We have been studying (together with dr. M. Panchenko and prof. H. Rucker from Graz) the question whether AKR is partly linearly polarized. In space observations the polarimeter is usually not directed to the AKR source. However, having determined the polarization parameters in each of the three perpendicular planes, one is able to determine the polarization ellipse in the 3-D space. Results of statistical estimations of the AKR polarization parameters in the wave plane are presented. Data were provided by the Interball-2/Polrad triaxial polarimeter. It is the first time the dynamic spectra of all four Stokes parameters of the AKR are displayed in the wave plane. The AKR polarization is mostly circular with an estimated mean value of the semiaxes ratio of 0.99 ± 0.10 rms error, with a small or none contribution of the linear component at a level of 0.07 ± 0.09 rms error, and a small or none unpolarized component at a level of 0.10 ± 0.08. The uncertainties of these estimations are too large to definitely conclude on presence or absence of some small contributions of the linear and unpolarized components in the AKR. However, in the limits of the above uncertainties these estimations do not contradict expectations that the linear polarization is absent in the AKR. Some small contribution of the unpolarized component can be explained by a relatively high level of noise and board interefences. These results were published in Radio Science (2008).

(J. Hanasz)

We have been studying cases of auroral kilometric radiation (AKR) modulation by Pc1 geomagnetic pulsations. Fifteen events of

I worked with Dr. Panchenko and Prof. Hanasz on the determination of AKR sources positions using Interball-2 (POLRAD experi-ment) radiopolarimeter data. Preliminary search for dayside sources proved to be rather inconclusive (they are not numerous and are difficult to localize). On the other hand checking of the AKR directivity pattern based on about 20 different dynamic spectra confirmed for most cases presence of AKR beams collimated along the auroral oval according to recent findings of Mutel et al., 2008. Our approach is based on data analysis on much longer time scales (of the order of 10 minutes) as compared with AKR microbursts tens of milliseconds long analyzed by Mutel et al. We introduced more detailed AKR visibility maps – that means for every AKR source we can determine both the azimuthal and elevation sizes of the AKR beams in ques-

tion. Dr. Panchenko introduced substantial improvements in his code for AKR sources positions determination – with a new version we will repeat our search for dayside AKR sources as well as improve existing position measurements and add the new ones. Preliminary results were presented in August at the URSI General Assembly 2008 in Chicago.

(R. Schreiber)

PHYSICAL AND GEODESIC STUDIES OF PLANETS AND

EARTH

Planetology

The orbital motion of Comet 81P/Wild 2 is investigated using a two-source model of outgassing. In the process of orbit impro-vement the nucleus orientation and the location of two active regions are found from numerical fitting of the non-gravitational acceleration model to positional observations of the comet. The derived spin axis orientation (I – about 60o, phi – about 155o) as well as the location of two active regions, the northern (beta: 84o) and the southern one (beta: -42o), agree with determinations based on different observations by other authors. The non-gravitational perturbations were also used to constrain the sizes of the two active areas as well as the mass and bulk density (about 400 kg/m3) of the comet nucleus. Orbital linkages of two and three successive apparitions of 81P/Wild 2 indicate an evolution of the change in the orbital period, possible time variations of the spin axis of the comet and an increase of the source areas during the last five revo-lutions. Two different approaches to the lag angle of the outgassing behind the subsolar meridian are considered, assuming this angle to be either constant or varying with heliocentric distance. The modeled two-source water production curve is compared with the activity data represented by the observed water production curve and the brightness curve. (S. Szutowicz, M. Królikowska, H. Rickman)

A paper about Monte Carlo simulations of the Oort Cloud dynamics over the age of the Solar System focussing on the injection mechanism into observable orbits was revised and published in Celest. Mech. & Dyn. Astron. This showed that the Galactic tide and the passing stars act in synergy to a previously unsuspected degree so that the injection rate with the full model is much larger than in any model that limits attention to just one of the two perturbers. I gave seminars about these results at CBK, CAMK, and Uppsala Observatory. In a further study, submitted for publication, we simulate comet injection by single stellar encounters of different types in order to elucidate the differences between the ways diferent stars act on the Cloud. This paper highlights the large difference in perturbing efficiency between high- and low-mass stars, arguing that the former are much more important than one is led to believe by their low encounter frequency, and the long-term effects of each stellar passage arising from the synergy with the tide.

(H. Rickman)

21

The Monte Carlo method of the nominal orbit clonning was applied to the case of 2007 WD5, the asteroid from the Apollo group. Calculations based on 33 observations from the time interval of 2007 11 08 – 2008 01 02 showed that the asteroid will pass near planet Mars at the minimum distance of 10.9 ± 2.9 R , what implies that probability that 2007 Mars

WD5 strike the planet decreased to the value of 0.03% from the value of about 3-4% previously announced by NASA. The additional observa-tions taken on January 3-9 reduce further the asteroid's impact chances, effectively to nil: the asteroid will pass near planet Mars at the minimum distance of 8.4 ± 1.1 R (Mars Mars

radius). (M. Królikowska, G. Sitarski)

We study the dynamical evolution of Asteroid 2002 AA . This object moves in the 29

co-orbital region of the Earth and is the first known asteroid which experiences recurrent

22

In our modeling the results of laboratory measurements were used. The Martian data given by VIRTIS-Rosetta spectrometer were also analysed and simulated. This work will be also continued in the nearest future.

We started also a new numerical simu-lations: 1) emission of CO line in the microwave range (HIFI project in Herschel Mission), 2) influence of biological aerosols on atmospheric spectra in various geometry of ground FTIR measurements. A possible detection of biological aerosols on Mars and Venus have been taken in considerations.

(M. B³êcka)

horseshoe–sitions between the HS and QS states are uni-que among other known Earth co-orbital asteroids and in the QS state 2002 AA remains 29

very close to Earth (within 0.2 AU for several decades. Based on results obtained analytically by Brasser et al. (2004) we developed a simple analytical method to describe and analyze the motion of 2002 AA . We distinguish a few 29

moments in time crucial for understanding its dynamics. Near 2400 and 2500 this object will be close to going through the maxima of the averaged disturbing function and it will either change its co-orbital regime by transition from the HS into QS state, or leave the librating mode. These approaches generate instability in the motion of 2002 AA . By means of 66 29

observations covering a two-year interval, we extend the analysis of the long term evolution of this object presented by Connors et al. (2002) and Brasser et al. (2004). Our analysis is based on a sample of 100 cloned orbits. We show that the motion of 2002 AA is 29

predictable in the time interval [- 2600,7100] and outside of this interval the past and future orbital history can be studied using statistical methods.

(P. Wajer)

quasi-satellite transitions. The tran-

The works connected with the spectro-metric measurements of OMEGA (Mars-Express mission) and VIRTIS (Venus Express and Rosetta missions) in the VIS-IR spectral range were continued. The transmittance and total radiance spectra from the soil and atmospheres in the spectral region 0.2-6.0 microns were calculated. We have simulated the dayside spectra of Venus and then we started to search for molecular oxygen in the dayside Venusian atmosphere. The results of our modeling were compared with recent VIRTIS Venus data. The role of dust and aerosols in the radiative transfer equation were carefully analysed. The presence of dust in Venusian clouds were taken in consideration. Influence of emittance of Valles Marineris region on Mars on spectra has been calculated.

Earth rotation studies

My research work was focused on the following two subjects. The first concerned perturbations in Earth rotation due to influence of the external fluid layers, the atmosphere, the oceans and the land hydro-logy. Together with J. Nastula and B. Ko³aczek, we performed detailed excitation balance of the seasonal components of polar motion. The aim was to estimate the role played by time variations taking place in land water reservoirs, represented by the hydro-logical angular momentum (HAM). We used the estimates of HAM from the hydrological models and those derived from the measure-ments done by the Gravity Recovery and Climate Experiment (GRACE). Results have been described in the paper (Brzezinski et al., 2009, J. Geodyn.). The second subject concerned the possibility of modeling and observation the perturbations in Earth rotation having very short periods, daily and subdaily. We performed detailed analysis of the recent high resolution determinations of polar motion based on the measurements of the ring laser in Wettzell, Germany, and the possibility of their use for interpolation of the standard determinations from space geodesy, which have typical sampling interval between 1 and 3 days. Results have been reported in two

The atmospheric, ocean and hydrologic excitation functions as well as their sums were used to compute the x, y pole coordinates model data using numerical integration of differential equation of polar motion. Other x, y pole coordinates model data were obtained by summing different frequency components determined by the discrete wavelet transform band pass filter. The IERS pole coordinates data and the pole coordinates model data were then predicted by the combination of the least-squares model extrapolation and autore-gressive prediction. Comparison of the prediction errors computed at different starting prediction epochs for the IERS pole coordinates data and the pole coordinates model data, has enabled examination of influence of the irregular oscillations in the fluid excitation functions on the prediction errors of pole coordinates data. It was shown that the increase of pole coordinate data prediction errors are caused mostly by irregular short period oscillations excited by joint atmospheric and ocean excitation functions. This joint atmosphere and ocean angular momentum excitation of the pole coordinates data cause increase of their prediction errors up to 100 days in the future similarly as in the case of prediction errors of the pole coordinates model data created as the sum of Chandler, annual and shorter period frequency components. The prediction errors of the pole coordinates model data computed from hydrologic angular momentum exci-tation functions are negligible. (W. Kosek, W. Popiñski, A. Rzeszótko,

T. Niedzielski).

In order to predict the Universal Time UT1-UTC and the length of day the combination of least squares model extrapo-lation and univariate or multivariate autore-gressive methods were applied. In the case of multi-variate autoregressive method the axial component of atmospheric angular momen-tum was used. Analysis showed that predi-ction errors of combination of the least-squares model and multivariate autoregressive methods are smaller than prediction errors of the least-squares model extrapolation and its squares model extrapolation and its combi-nation with univariate autoregressive method especially at the time of El Niño and La Niña events. The combination of the least-squares extrapolation and univariate autoregression method was also applied to predict sea level variations based on TOPEX/Poseidon and Jason-1 altimetric measurements. The global and local sea level variations were considered. Prediction of local sea level variations in the east-equatorial Pacific showed that the prediction errors of the combination of least-squares model extrapolation and autore-gressive method are smaller than the predi-ction errors of the deterministic method. Several known probability distributions were fitted to the length of day and the x, y pole coordinates data. The x, y pole coordinates data and their residuals can be modeled using the normal distribution. The probability distribution of the length of day data and their residuals differ from a normal probability law and the Johnson SB and SU distributions provide the best overall fit to empirical distribution of these data and their residuals.

(T. Niedzielski, W. Kosek)

works (Brzezinski, 2009, Proc. Journees 2008) and (Mendes et al.., 2009, Pure Appl.Geophys., in press).

(A. Brzeziñski)

23

The Earth Orientation Parameters predi-ctions submitted since October 2005, by different participants of the Earth Orientation Parameters Prediction Comparison Campaign who were using various algorithms, were evaluated by the same statistical analysis. It was shown that combined predictions are better than most individual predictions, predictions of UT1 - UTC have to be based on the atmo-spheric angular momentum forecast data and the best techniques to predict polar motion variations are combinations of least squares extrapolation and autoregressive prediction.

(M. Kalarus, W. Kosek).

Together with physicists from the Institute of Physics of the Polish Academy of Sciences (R.R. Ga³¹zka) and Italian Institute of Space Physics (R. Peron) the idea is presented of the measurement of the speed of the gravity signal in space. According to the general relativity theory it should be the same as the velocity of light, however it was never confirmed experimentally. In the presented work it is proposed to use the gradient of the Earth gravitational acceleration, which is locally observable parameter of the gravity field and the rotation of the Earth as the time measure. As technical tools the gradiometers and GPS and Galileo satellites are proposed. Realization of such an experiment will require significant improvement of the accuracy of the gradient measurement but is in the range of realistic possibilities.

(J.B. Zieliñski)

Earth gravitational field

24

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.

ISES

The International Space Environment Service, is an international organisation co-ordinating 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 ISES' Regional Warning Center (RWC) (http:// www.cbk.waw.pl/rwc). Space Research Cen-tre exchanged data with other Warning Cen-ters: in Boulder, USA; Tokyo, Japan; Sydney, Australia; Brussels, Belgium; Moscow, Russia; and Prague, Czech Republic. A large portion of data is received directly from various national and international observatories, such as observatorio de l'Ebre. Data on terrestrial magnetic field activity are supplied by the Central Geophysical Observatory PAS in Belsk, Poland. Solar radio flux at 10 freq-uencies is supplied by Observatory of Cracow. Both are available on the home page in near-real time. The new ionosonde has been recently installed in SRC Warsaw. Data are available in real time. SRC publishes a special daily bulletin URSIGRAM Warsaw on the basis of the continuous flow of data from Poland and abroad, and it broadcasts it within the ISES.

The impact of various space weather phenomena is studied. Methods and algo-rithms linked directly to the radiocom-munication prediction and forecast domain are developed and continuously improved. The RWC/IDCE (The Ionospheric Despatch Centre in Europe) web service (http:// www.cbk.waw.pl/rwc/idce) provides on line access to data base of the critical frequency of F2 ionospheric layer forecast for all available

25

sites. Daily plots for 30 stations from all over the world are presented along with their digital version. 24-hours ahead forecast for every station is supplied. 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 communication HF radio signal intensity. The work is carried out using software packages HELGEO and Ray-Route 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 organizes 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. New, fifth - generation version of the system Ray-Route has been prepared. The major change required by the users has been implemented.

(I. Stanis³awska)

Space Research Centre is involved in the Global Monitoring for Environment and Security (GMES) thematic projects.

GMES

In December 2008 the PEARL project has been accomplished. The objective of the project was to develop a port monitoring system that employs satellite and in situ data. The project under Atos Origin coordination has provided platform which is scalable and

capable of ingesting future data products and models, together with the effective integration of space and in-situ data and models. This provides the port environmental manager with a user friendly tool for accessing and inter-preting all relevant environmental infor-mation (data and models).

The establishment of the PEARL platform requirements has been based on the analysis and translation into platform technical requirements (broaching software and com-munications issues) of the port environmental requirements and the sensors selection (space and in-situ) identified within the project. The PEARL platform was validated in three European ports: Port of Barcelona, Port of Southampton, Port of Tallinn. The validation of the Pearl project aims at testing the platform in practice, highlight its capabilities and work further on adapting it according to the received feedback, in future projects not under the scope of PEARL project, so that it can take its final form as a practical tool responding to the needs of general and operational port envi-ronmental management. Based on the market analysis SRC has prepared exploitation plan of the PEARL platform. The market analysis considered the current market trends, market characteristics, existing services and products. The main outcome from the analysis is that the system design should include a global, as well as regional components which provide ocean analysis and forecasts in real-time and near real-time through assimilation of in situ and satellite data. The platform should provide an integrated service of ocean monitoring and forecasting to intermediate users and policy makers in support of safe and efficient offshore activities, environmental management, securi-ty, and sustainable use of marine resources. SRC also has prepared business plan for platform implementation. The aspects that has been taken under consideration are: business organization options, business models, marketing strategy, financial and risk manage-ment plan. Simultaneously SRC was responsi-

ble for dissemination activities. The PEARL project was promoted during the conferences and workshops dedicated to marine thematic area and GMES thematic area. The promo-tional materials were prepared: brochures, posters, publications. The PEARL web was maintained http://www.pearl-project.eu/.

26

In 2008 Space Research Center has enriched Land Border Monitoring service (one of Land and Infrastructure Surveillance work packages within LIMES project) in updated infor-mation and data. Land Border Monitoring services are dedicated to Border Guards and FRONTEX Agency, so all the activities are prepared for their needs.

Collected data allows to create services based on: (1) land use and land cover mapping; (2) change detection; (3) semi-automated chan-ge analysis using object-oriented methods. Hence, Land Border Monitoring is divided into three services: 1. update and enrichment of cartographic data

using VHR satellite data, 2. cross-border accessibility maps, 3. change detection.

In September 2008 demonstration of proposed service took place in Space Research Centre of the Polish Academy of Science in Warsaw. The purpose of this event was to present work results and collect feedback from end-users. Services were prepared for certain test area of Polish-Ukraine green border.

First service case refers to update and enrichment of cartographic data using VHR satellite data. This case shows that land cover and border-specific objects like border control points can be changed by raster or vector layers with updated information on infrastructure, buildings, roads, tracks, waters, etc. The actualization of data gives better view on guarded area and improves work of guards from neighborhood countries.

Second service case presents cross-border accessibility maps. Interactive raster layer in

Geoland2 intends to constitute a major step forward in the implementation of the GMES Land Monitoring Core Service (LMCS). The three components (Local, Continental and Global) of the LMCS are addressed. The goal of geoland2 is (1) to prepare, validate and demonstrate pre-operational service chains and products that will underpin the LMCS, and (2) to propose and demonstrate a concrete functional organization of the LMCS.

The architecture of geoland2 is made of two different layers, the Core Mapping Services (CMS) and the Core Information Services (CIS). The CMS produce 'basic' land cover, land cover change, and land state products which are of broad generic use and can be directly used for deriving more elaborated products. The CMS products cover a wide variety of thematic content, spatial scales from local to global, and update frequency, from 1 day to several years.

27

GIS system and specific algorithm, which calculate faster interception route, is a great tracking help for border guards.

Third service case is detection of changes, based on segmentation of TerraSAR-X ima-gery. Activities in this service extract diffe-rences between data, collected not in the same time. Surveillance operators are informed about occurrences or displacements of groups of people, vehicles, newly build roads or even deployed camps in border areas.

MR continental coverage of seasonal and annual vegetation parameters to produce land cover change and agricultural land use. The time frequency of the product update is on the order of 3 - 12 months.

In 2008 SRC participated in numbers of meetings related to creation service portfolio and users requirements. As a SATChMo coordinator, SRC organized KO meeting and technical meeting with partners. During the second one, Methodology of AFS Europe scheme (definition of classes, classification scheme), Methodology of Classification and change detection were discussed. Works focused also on choosing areas of image acquisitions and estimating future (2013-2019) SATChMo service budget. (K. Bieliñska, £. Paluchowski, M. Stelmaszczuk)

Space Research Centre of the Polish Academy of Science plays important role in geoland2. SRC is responsible for coordination of Seasonal & Annual Change Monitoring (SATChMo).

SATChMo operates at continental scale over Europe and Su-Saharan Africa. It delivers: (1) a VHR/HR Area Frame Sampling over permanent samples representative for all European and African environmental/ ecological conditions for annual statistics of land cover & land cover change; (2) a complete

The objectives of TANGO (Telecom-munications Advanced Networks for GMES Operations) is three-year European Com-mission (EC) program to develop, integrate, demonstrate and promote new satellite telecom services dedicated to GMES (Global Moni-toring for Environment & Security) require-ments. TANGO - the first project under EC FP6 focused on the use of satellite telecom is addressed to key environment and security applications including risk and crisis manage-ment and humanitarian aid. The project is led by EADS Astrium, and gathers 24 research and industrial partners including GMES service providers, GMES data providers and end-users

users representatives as well as Satellite Com-munication's leading expertise in the area. TANGO consortium aims at providing operational telecommunication solutions to the GMES services needs, and at preparing the definition of satellite telecom infrastructures to expand the future GMES services.The Space Research Centre as a partner of TANGO consortium is involved in definition of SATCOM infrastructure for risk and crisis management demands of GMES services related to natural and man-made disasters situations. Another line of activity of SRC is the elaboration and selection of methodology of cost benefit analysis for SATCOM/GMES solutions. The GMES scenarios suggested by SRC need on-field operations. In the rescue operational practice, the Situation Centre is organized in the disaster area to provide local operation coordination and to supply units in the field with wide range of geospatial products. On the other side, the permanent operating National Crisis Management Centre supports rescue operations through gathering information and analyzing it, providing recommendations and using the experts' knowledge. In Poland, the permanent Crisis Management Centre is affiliated to the Minis-

and petrol pipelines as well as the railway system infrastructure related damages. SATCOM application to GMES services in the context of cost benefit analysis has been evaluated in the frame of three dimension metrics:

• Time: Can the GMES services be provided faster?

• Quality: Can GMES service be provided better?

• Cost: Can GMES services be provided cheaper?

The current process of different GMES services has been segmented and SATCOM application areas were addressed to Data collection, Data Providers and Customer Services, End User and in-Field Communication, System Capa-bilities, Technical Architecture and System Coast.Finally, TANGO functional requirements and business process and architecture (type of services and data transportation models) have been adjusted by TANGO team at the Joint Research Centre to Work Package documents. Results of work were regularly reported at Partners Meetings.

(Z. K³os)

try of Interior Affairs and Administration, while the Situation Centre is deployed at Local Administration infrastructure and is com-manded by the Voyevoda of the Region. Providers of the regular geospatial, mete-orology, hydro, radiation, chemical or seismic infor-mation and products supply the system by data stream. The Crisis Management Sys-tem takes care of prevention and security and it dis-seminates the information about the major regional electrical power failures, gas

28

PUBLICATIONS

* Total number of publications in 2008: 290 (including 54 in the journals from JCR list)* Papers in refereed international science journals, books, and proceedings: 70* Articles, referee reports, monographs, reviews in international and national publications: 33* Papers delivered at international science conferences and meetings: 187 (including 13 invited talks)* Papers in press or submitted for publication in 2008: 21

Papers in refereed international

science journals and proceedings:

Boudjada MY, Schwingenschuh K, Biernat HK, Berthelier JJ, B£ÊCKI J, Parrot M, Stachel M, Aydogar O, Stangl G, Weingrill E, Similar behaviors of natural ELF/VLF ionospheric emissions and transmitter signals over seismic Adriatic regions. Natural Hazards Earth System Science, Vol. 8, 1229-1236, 2008.

Bradley PA, STANIS£AWSKA I, JU-CHNIKOWSKI G, Options for mapping foF2. Advances in Space Research, doi: 10.1016/j.asr.2008.09.028, 2008.

BRZEZIÑSKI A, On the influence of diur-nal atmospheric tides on Earth rotation.

29

Proc. Journées 2007, Systèmes de référence spatio-temporels, pp. 180-183, 2008.

BZOWSKI M, Survival probability and energy modification of hydrogen energetic neutral atoms on their way from the termination shock to Earth orbit. Astrono-my & Astrophysics, Vol. 488, pp. 1057-1068, 2008.

BZOWSKI M, Moebius E, TARNOPOL-SKI S, Izmodenov V, Gloeckler G, Density of neutral interstellar hydrogen at the termination shock from Ulysses pickup ion bservations. Astronomy & Astrophysics, Vol. 491, pp. 7-19, 2008.

BZOWSKI M, Moebius E, TARNOPOL-SKI S, Izmodenov V, Gloeckler G, Neutral H Density At the Termination Shock:

35

29

67

45

47

43

48

54

94

101

87

92

91

76

86

75

73

70

47

35

49

96

0 20 40 60 80 100 120

1998

1999

2000

2001

2002

2003

2004

2005

2006

2007

2008

Published in the JCR journals total

30

Consolidation of Recent Results. Space Science Reviews, doi: 10.1007/s11214-008-9479-0, 2008.

Carrasco N, Hebrard E, BANASZKIE-WICZ M, Dobrijevic M, Pernot P, Influence of neutral transport on ion chemi-stry uncertainties in Titan ionosphere. Icarus, Vol. 192, pp. 519-526, 2007.

Collura A, Barbera M, Varisco S, Calderone G, Reale F, GBUREK S, KOWALIÑSKI M, SYLWESTER J, SIARKOWSKI M., BAKA£A J, PODGÓRSKI P, TRZE-BIÑSKI W, P£OCIENIAK S, KOR-DYLEWSKI Z, Calibration of the SphinX experiment at the XACT facility in Palermo. Proc. SPIE, Vol. 7011, 70112U, 2008.

CZECHOWSKI A, Hilchenbach M, Hsieh KC, GRZÊDZIELSKI S, Kota J, Imaging the heliosheath using HSTOF energetic neutral atoms and Voyager 1 ion data.

Astronomy & Astrophysics, Vol. 487, pp. 329-335, 2008.

De Franceschi G, Alfonsi L, Altadill D, Bencze P, Bourdillon A, Buresova D, Cande LjR, de la Morena B, Economou L, Herraiz M, Kauristie K, Lastovicka J, Pau S, Rodriguez G, Stamper R, STANI-S£AWSKA I, The contribution to IHY from the COST296 Action MIERS: Mitigation of Ionospheric Effects on Radio Systems. Earth Moon and Planets, doi: 10.1007/s11038-008-9275-6, 2008.

Dyrud L, Krane B, Oppenheim M, Pecseli HL, Trulsen J, WERNIK AW, Structure functions and intermittency in ionospheric plasma turbulence. Nonlinear Processes in Geophysics, Vol. 15, pp. 847-862, 2008.

Dzifcakova E, Kulinova A, Chifor C, Mason HE, Del Zanna G, SYLWESTER J, SYLWESTER B, Nonthermal and thermal diagnostics of a solar flare observed with

RESIK and RHESSI. Astronomy & Astrophysics, Vol. 488, pp. 311-321, 2008.

GULYAEVA TL, Linkage of the iono-spheric peak electoron density and height deduced from the topside sounding data. Advances in Space Research, doi: 10.1016/ j.asr.2008.08.015, 2008.

GULYAEVA TL, Bradley PA, STANI-S£AWSKA I, JUCHNIKOWSKI G, To-wards a new reference model of hmF2 for IRI. Advances in Space Research, Vol. 42, pp. 666-672, 2008.

GULYAEVA TL, Gallagher DL, Compa-rison of two IRI electron-density plasma-sphere extensions with GPS-TEC observa-tions. Advances in Space Research, Vol. 39, pp. 744-749, 2007.

GULYAEVA TL, STANIS£AWSKA I. Derivation of a planetary ionospheric storm index. Annales Geophysicae, Vol. 26, pp. 2645-2648, 2008.

GULYAEVA TL, STANIS£WSKA I, TO-MASIK M, Ionospheric weather: cloning missed foF2 observations for derivation of variability index. Annales Geophysicae, Vol. 26, pp. 315-321, 2008.

HANASZ J, SCHREIBER R, Pickett J, de Feraudy H, Pulsations of auroral kilometric radiation at Pc1 frequencies. Geophysical Research Letters, Vol. 35, art. no. L15819, doi:10.1029/2008GL034609, 2008.

Hathi B, Ball AJ, BANASZKIEWICZ M, Daniell PM, Garry JRC, Hagermann A, Leese MR, Lorenz RD, Rosenberg PD, Towner MC, Zarnecki JC, In situ thermal conductivity measurements of Titan's lower atmosphere. Icarus, Vol. 197, pp. 579-584, 2008.

Izhovkina NI, Prutensky IS, Pulinets SA, Erokhin NS, Mikhailovskaya LA, K£OS Z, ROTHKAEHL H, Electromagnetic waves and electrostatic oscillations in an inhomo-geneous plasma structure at the geoma-gnetic equator. Geomagnetism and Aerono-my, Vol. 48, pp. 631-641, 2008.

31

JAWORSKI L, ŒWI¥TEK A, ZDUNEK R, ZIELIÑSKI JB, Data processing of the ASG-EUPOS network test campaign, Reports on Geodesy, No 2(85), pp. 113-124, 2008.

KACZOROWSKI M, Non tidal plumb line variations observed with help of the long water-tube and horizontal pendulums tiltmeters in Geodynamic Laboratory of PAS in Ksiaz. Reports on Geodesy, No. 2(85), pp. 79-86, 2008.

KALARUS M, KOSEK W, Schuh H, Current results of the Earth Orientation Parameters Prediction Comparison Cam-paign. Proc. Journées 2007, Systèmes de Réfé-rence Spatio-Temporels, pp. 159-162, 2008.

Kierulf HP, Plag HP, Bingley RM, Teferle N, Demir C, Cingoz A, Yildiz H, Garate J, Davila JM, Silva CG, ZDUNEK R, JAWO-RSKI L, Martinez-Benjamin JJ, Orus R, Aragon A, Comparison of GPS analysis strategies for high-accuracy vertical land motion. Physics and Chemistry of the Earth, Vol. 33, pp. 194-204, 2008.

Kirchner G, KUCHARSKI D, Cristea E, Gravity Probe-B: New Methods to deter-mine Spin Parameters From kHz SLR Data. IEEE Transactions on Geoscience and Remote Sensing, Vol. 47, pp. 370-375, 2009.

Komle NI, Hutter ES, Kargl G, Ju HH, Gao Y, GRYGORCZUK J, Development of Thermal Sensors and Drilling Systems for Application on Lunar Lander Missions. Earth Moon and Planets, Vol. 103, pp. 119-141, 2008.

KORBACZ A, BRZEZIÑSKI A, Thomas M, Geophysical excitation of LOD/UT1 estimated from the output of the models ERA-40 and OMCT. Proc. Journées 2007, Systèmes de référence spatio-temporels, pp. 188-191, 2008.

KOSEK W, KALARUS M, NIEDZIELSKI T, Forecasting of the Earth orientation parameters – comparison of different tech-niques. Proc. Journées 2007, Systemes de Réfé-rence Spatio-Temporels, pp. 155-158, 2008.

Kossacki KJ, SZUTOWICZ S, Comet 9P/Tempel 1: Sublimation beneath the dust cover. Icarus, Vol. 195, pp. 705-724, 2008.

KUCHARSKI D, Kirchner G, Cristea E, ETALON spin period determination from kHz SLR data. Advances in Space Research, Vol. 42, pp. 1424-1428, 2008.

Kueppers M, Keller HU, Kührt E, A'Hearn MF, Altwegg K, Bertrand R. Busemann H, Capria MT, Colangeli L, Davidsson B, Ehrenfreund P, Knollenberg J, Mottola S, Rathke A, Weiss P, Zolensky M, Akim E, Basilevskij A, Galimov E, Gerasimov M, Korablev O, Lomakin I, Marov M, Martynov MB, Nazarov M, Zakharov A, Zelenyi L, Aronica A, Ball AJ, Barbieri C, Bar-Nun A, Benkhoff J, Biele J, Biver N, Blum J, Bockelee-Morvan D, Botta O, Bredehöft J-H, Capaccioni F, Charnley S, Cloutis E, Cottin H, Cremonese G, Cro-visier J, Crowther S, Epifani EM, Esposito F, Ferrari AC, Ferri F, Fulle M, Gilmour J, Goesmann F, Gortsas N, Grady M, Green SF, Groussin O, Grün E, Gutiérrez PJ, Hartogh P, Henkel T, Hilchenbach M, Tra-Mi Ho, Horneck G, Hviid SF, Ip W, Jäckel A, Jessberger E, Kallenbach R, Kargl G, Kömle NI, Korth A, Kossacki K, Krause C, Krüger H, Li Z-Y, Licandro J, Lopez-Moreno JJ, Lowry SC, Lyon I, Magni G, Mall U, Mann I, Markiewicz W, Martins Z, Maurette M, Meierhenrich U, Mennella V, Ng TC, Nittler L, Palumbo P, Pätzold M, Prialnik D, Rengel M, Rickman H, Rodriguez J, Roll R, Rost D, Rotundi A, Sandford S, Schoenbaechler M, Sierks H, Srama R, Stroud R, SZUTOWICZ S, Tornow C, Ulamec S, Wallis M, Waniak W,

32

Weissman P, Wieler R, Wurz P, Yung KL, Zarnecki JZ, Triple F - A Comet Nucleus Sample Return Mission. Experimental Astronomy, doi: 10.1007/s10686-008-9115-8, 2008.

LELIWA-KOPYSTYÑSKI J, Burchell MJ, Lowen D, Impact cratering and break up of the small bodies of the Solar System. Icarus, Vol. 195, pp. 817-826, 2008.

MACEK WM, SZCZEPANIAK A, Generalized two-scale weighted Cantor set model for solar wind turbulence. Geophy-sical Research Letters, Vol. 35, art. no. L0 2108, doi:10.1029/2007GL032263, 2008.

MACEK WM, WAWRZASZEK A, Evo-lution of asymmetric multifractal scaling of solar wind turbulence in the outer helio-sphere. Journal of Geophysical Research. doi: 10.1029/2008JA013795, 2008.

Nakagawa H, BZOWSKI M, Yamazaki A, Fukunishi H, Watanabe S, Takahashi Y, Tagu Taguchi M, Yoshikawa I, Shiomi K, Nakamura M, UV optical measurements of the Nozomi spacecraft interpreted with a two-component LIC-flow model. Astrono-

my & Astrophysics, Vol. 491, pp. 29-41, 2008.

NASTULA J, KO£ACZEK B, Salstein DA, Comparison of hydrological and GRACE – based excitation functions of po-lar motion in the seasonal spectral band. Proc. Journées 2007, Systemes de Référence Spatio-Temporels, pp. 220-222, 2008.

NIEDZIELSKI T, KOSEK W, Forecasting sea level anomalies from TOPEX/Poseidon and Jason-1 satellite altimetry. Journal of Geodesy, doi: 10.1007/s00190-008-0254-5, 2008.

NIEDZIELSKI T, KOSEK W, Forecasting irregular variations of UT1-UTC and LOD data caused by ENSO. Proc. Journées 2007, Systemes de Référence Spatio-Temporels, pp. 222-223, 2008.

Panchenko M, HANASZ J, Rucker HO, Estimation of linear wave polarization of the auroral kilometric radiation. Radio Science, Vol. 43, art. no. RS1006, doi: 10.1029/2006RS003606, 2008.

Pryor W, Gangopadhyay P, Sandel B, For-rester T, Quemerais E, Moebius E, Esposito L, Stewart I, McClintock W, Jouchoux A, Colwell J, Izmodenov V, Malama Y, Tobiska K, Shemansky D, Ajello J, Hansen C, BZOWSKI M, Radiation transport of heliospheric Lyman-alpha from combined

Cassini and Voyager data sets. Astronomy & Astrophysics Vol. 491, pp. 21-28, 2008.

RATKIEWICZ R, GRYGORCZUK J, Orientation of the Local Interstellar Magnetic Field Inferred from Voyagers Positions. Geophysical Research Letters, Vol. 35, art. no. L23105, doi: 10.1029/23008 Gl036117, 2008.

RATKIEWICZ R, Ben-Jaffel L, GRY-GORCZUK J, What Do We Know about the Orientation of the Local Interstellar Magnetic Field? ASP Conference Series, Vol. 385, pp. 189-194, 2008.

RICKMAN H, Fouchard M, Froeschle C, Valsecchi GB, Injection of Oort Cloud comets: the fundamental role of stellar

perturbations. Celestial Mechanics & Dynamical Astronomy, Vol. 102, pp. 111-132, 2008.

ROTHKAEHL H, Krankowski A, STA-NIS£AWSKA I, B£ÊCKI J, Parrot M, Berthelier JJ, Lebreton JP, Wave and plasma measurements and GPS diagnostics of the main ionospheric trough as a hybrid met-hod used for Space Weather purposes. An-nales Geophysicae, Vol. 26, pp. 295-304, 2008.

ROTHKAEHL H, Trotignon J-G, Dec-reau P, B£ÊCKI J, Pitout F, Reme H, HF wave activity in the low and middle-

33

altitude polar cusp. Advances in Space Re-search, doi:10.1016/j.asr.2008.07.018, 2008.

Rzeszótko A, KOSEK W, Popiñski W, The influence of variable amplitudes and phases of the most energetic oscillations in the EOP on their prediction errors, Proc. Journées 2007, Systèmes de Référence Spatio-Temporels, pp. 224-225, 2008.

Saad AS, BANASZKIEWICZ M., SITAR-SKI G, A new algorithm of the recurrent power series method for the nongra-vitational motion of comets. Applied Mathe-matics and Computation, Vol. 197, pp. 874-879, 2008.

Savin S, Amata E, Zelenyi L, Budaev V, Consolini G, Treumann R, Lucek E, Safrankova J, Nemecek Z, Khotyaintsev Y, Andre M, Buechner J, Alleyne H, Song P, B£ÊCKI J, Rauch JL, Romanov S, Klimov S, Skalsky A, High energy jets in the Earth's magnetosheath: Implications for plasma dynamics and anomalous transport. JETP Letters, Vol. 87, pp. 593-599, 2008.

SIARKOWSKI M, Falewicz R, KÊPA A, Rudawy P, Diagnostic of the temperature and differential emission measure (DEM) based on Hinode/XRT data. Annales Geophysicae, Vol. 26, pp. 2999-3005, 2008.

S£OMIÑSKA E, B£ÊCKI J, Parrot M, S£OMIÑSKI J, Satellite study of VLF ground-based transmitter signals during seismic activity in Honshu Island. Physics and Chemistry of the Earth, doi: 10.1016/ j.pce.2008.06.016, 2008.

Smith A, Crawford IA, Gowen RA, Ball AJ, Barber SJ, Church P, Coates AJ, Gao Y, Griffiths AD, Hagermann A, Joy KH, Phipps A, Pike WT, Scott R, Sheridan S, Sweeting M, Talboys D, Tong V, Wells N, Biele J, Chela-Flores J, D¥BROWSKI B, Flannagan J, Grande M, GRYGORCZUK J, Kargl G, Khavroshkin OB, Klingelhoefer G, Knapmeyer M, MARCZEWSKI W,

McKenna-Lawlor S, Richter L, Rothery DA, SEWERYN K, Ulamec S, WA-WRZASZEK R, Wieczorek M,Wright IP, Sims M, LunarEX – a proposal to cosmic vi-sion. Experimental Astronomy, doi: 10. 1007/s10686-008-9109-6, 2008.

STANIS£AWSKA I, Belehaki A, Space weather observational activities and data management in Europe. Acta Geophysica, Vol. 57, pp. 236-244, 2009.

STASIEWICZ K, Ekeberg J, Dispersive MHD waves and alfvenons in charge non-neutral plasmas. Nonlinear Processes in Geophysics, Vol. 15, pp. 681-693, 2008.

STASIEWICZ K, Ekeberg J, Electric potentials and energy fluxes available for particle acceleration by alfvenons in the solar corona. Astrophysical Journal Letters, Vol. 680, pp. L153-L156, 2008.

STRUMIK M, MACEK WM, Statistical analysis of transfer of fluctuations in solar wind turbulence. Nonlinear Processes in Geophysics, Vol. 607-613, 2008.

STRUMIK M, MACEK WM, Testing for Markovian character and modeling of intermittency in solar wind turbulence. Physical Review E, Vol. 78, art. no. 026414, doi: 10.1103/PhysRevE.78.026414, 2008.

SYLWESTER B, SYLWESTER J, Phillips KJH, X-ray studies of flaring plasma. Jour-nal of Astrophysics and Astronomy, Vol. 29, pp. 147-150, 2008.

SYLWESTER J, Kuzin S, Kotov YD, Farnik F, Reale F, SphinX: A fast solar pho-tometer in X-rays. Journal of Astrophysics and Astronomy, Vol. 29, pp. 339-343, 2008.

SYLWESTER J, SYLWESTER B, Phillips KJH, Resik observations of helium-like argon X-ray line emission in solar flares. Astrophysical Journal Letters, Vol. 681, pp. L117-L120, 2008.

Articles, referee reports, monographs,

reviews in international and national publications:

34

SZCZEPANIAK A, MACEK WM, Asymmetric multifractal model for solar wind intermittent turbulence. Nonlinear Processes in Geophysics, Vol. 15, pp. 615-620, 2008.

SZUTOWICZ S, KRÓLIKOWSKA M, RICKMAN H, Non-gravitational motion of the Jupiter-family comet 81P/Wild 2, II. The active regions on the surface. Astro-

nomy & Astrophysics, Vol. 490, pp. 393-402, 2008.

ŒWI¥TEK A, Ionospheric trough in GPS signal. Acta Geophysica, Vol. 56, pp. 1162-1178, 2008.

TARNOPOLSKI S, BZOWSKI M, Detec-tability of neutral interstellar deuterium by a forthcoming SMEX mission IBEX. Astro-

nomy & Astrophysics, Vol. 483, pp. L35-L38, 2008.

TARNOPOLSKI S, BZOWSKI M, Neu-tral interstellar hydrogen in the inner helio-sphere under the influence of wavelength-dependent solar radiation pressure. Astrono-

my & Astrophysics, Vol. 493, pp. 207-216, 2009.

Treumann RA, K£OS Z, Parrot M, Physics of electric discharges in atmospheric gases: An informal introduction. Space Science Reviews, Vol. 137, pp. 133-148, 2008.

WAJER P, 2002 AA29: Earth's recurrent quasi-satellite? Icarus, doi: 10.1016/ j.icarus. 2008.10.018, 2008.

WERNIK AW, Pozoga M, GRZESIAK M, ROKICKI A, MORAWSKI M, Monitoring ionospheric scintillations and TEC at the Polish Polar Station on Spitsbergen: Instru-mentation and preliminary results. Acta Geophysica, Vol. 56, pp. 1129-1146, 2008.

ZIELIÑSKI JB, Ga³¹zka RR, Peron R, On possible determination of the speed of the gravity signal in space with help of gradio-

Belehaki A, Cander L, Zolesi B, Bremer J, Juren C, STANIS£AWSKA I, Dialetis D, Hatzopulos M, DIAS system: Specification and forecasting of the ionospheric

thconditions over Europe, Proc. IES2008, 12 International Ionospheric Effects Symposium, 441-442, 2008.

Belehaki A, STANISLAWSKA I, Lilensten J, Modeling space weather effects in the ionosphere: a review, Space Sci. Rev, in press, 2008.

B£ÊCKA MI, GURGUREWICZ J, Helbert J, Maturilli A, Modelling the in-fluence of the emittance of weathered basal-tic materials on radiance spectra – related to observations of Valles Marineris region on Mars. EPSC Abstracts, Vol. 3, EPSC2008-A-0462, 2008.

B£ÊCKA MI, Piccioni G, Drossart P, Exa-mination of the structure of the clouds on Venus by comparison the simulated and me-asured radiance from the atmosphere. Ab-stracts 37th COSPAR Scientific Assembly, 2008.

Clark G, O'Neill M, Moebius E, Kucharek H, Granoff M, Widholm M, BZOWSKI M, H£OND M, Expected Performance of the IBEX Star Sensor for Accurate Pointing of IBEX-Lo Sensor. Eos Trans. AGU, Vol. 89 (53), Abstract SH21B-1606, 2008.

GABRYSZEWSKI R, Telefon do lamusa. PC FORMAT, No. 4, 2008.

GABRYSZEWSKI R, Wybór operatora. VoIP, NEXT, No. 2, 2008.

metry. Artifical Satellites, Vol. 42, pp. 129-140, 2008.

35

GABRYSZEWSKI R, Tajniki konfiguracji. VoIP, NEXT, No. 12, 2008.

GURGUREWICZ J, Mineralogy of Noctis Labyrinthus (Valles Marineris, Mars) – results from imaging and Fourier spectro-meters. Mineralogia – Special Papers, 32, 74, 2008.

GURGUREWICZ J, Maturilli A, Helbert J, Infrared spectrometric data of basaltic Martian analogues from Mongolian ter-ranes and the Baikal Rift Zone. EPSC Abstracts, Vol. 3, EPSC2008-A-00412, 2008.

Hippler R, Wolfgram M, Glover A, Jansen F, Kokowsky M, Schmieder B, Poedts S, STANIS£AWSKA I, Stelmach J, Kudela K, Reis R, Nakamura R, Denne W, Gausa M. Beck P, Tulunay Y, Rayabov B, Space Weather and Europe – an education tool with the Sun (SWEETS), COST 724 Final Report, COST Office, 417-422, 2008.

Jockers K, SZUTOWICZ S, HCN and CN in Comet 2P/Encke, a three-dimensional view on Comet Encke's outgassing. EPSC Abstracts, Vol. 3, EPSC2008-A-00492.

KALARUS M, KOSEK W, Schuh H, Cur-rent results of the Earth Orientation Para-meters Prediction Comparison Campaign. Proc. Journées 2007, Systèmes de Référence Spatio-Temporels, pp. 159-162, 2008.

K£OS Z, STANIS£AWSKA I, Michno-wski S, Globalny elektryczny obwód atmo-sfery i pogoda kosmiczna. In: PTG-60 lat dzia³alnoœci, IMGW, 2009.

Krypiak-Gregorczyk A, Krankowski A, ROTHKAEHL H, Parrot M, Berthelier J-J, Lebreton J-P, A hybrid method for dia-gnostics of the mid-latitude ionospheric trough using GPS and DEMETER obser-vations. Geophysical Research Abstracts, Vol. 10, EGU2008-A-06402, 2008.

Lilensten J, Candidi M, Belehaki A, STANIS£AWSKA I, Heyndericks D, Gille P, Amata E, Messerotti M, Jansen F,

Tulunay Y, Synthesis of Working group 4 activities, COST 724 Final Report, COST Office, 359-366, 2008.

Lilensten J, Zolesi B, Belehaki A, STA-NIS£AWSKA I, Perrone L, Collaboration among COST actions. Ionosphere and space weather, COST 724 Final Report, COST Office, 427-433, 2008.

Lundstedt H, Windtoft P, STANIS£A-WSKA I, Belehaki A, European space weather forecasting service, COST 724 Final Report, COST Office, 373-384, 2008.

£ukowski MI, Usowicz B, MARCZEWSKI W, Ground tests and ENVISAT images interpretation for SMOS validation. EU-ROSOIL 2008 Book of Abstracts, p. 252, 2008.

Pezzopane M, Scotto C, STANIS£AWSKA I, JUCHNIKOWSKI G, Autoscala applied at the Ionospheric Station of Warsaw, INAG-69 Ionosonde Network Advisory Group, Working Group 1 of URSI Commission G, Bulletin on the Web, 2008.

Romantsova T, Panchenko M, Mogilevsky M, HANASZ J, SCHREIBER R, Rucker H, Birukov V, Localization of AKR source using observation from two satellites. Geophysical Research Abstracts, Vol. 10, EGU2008-A-06525, 2008.

ROTHKAEHL H, Krankowski A, Koper-ski P, Kulak A, Parrot M, Berthelier J-J, Lebreton J-P, Response of main ionospheric trough for distance plasma disturbances, Geophysical Research Abstracts, Vol. 10, EGU2008-A-06402, 2008.

ROTHKAEHL H, Kudela K, Bucik R, Grigoryan O, The response of ionospheric plasma to the physical processes in the radiation belt regions. COST 724 final report, pp. 209-219, 2008.

ROTHKAEHL H, Thide B, Bergman JE, Natural spacecraft-Moon, challenge for monitoring Sun, solar wind and the dif-

ferent region of magnetosphere. Geophysical Research Abstracts, Vol. 10, EGU2008-A-06402, 2008.

Seoane L, NASTULA J, Bizouard C, Gam-bis D, Hydrological effects on polar motion compared to GRACE observations. Proce-edings of the Annual Meeting of the French Society of Astronomy and Astrophysics, p. 145, 2008.

SCHILLAK S, Upgrading of the Borowiec SLR station in 2006/2007. Proc. ILRS Fall 2007 Workshop, 2008.

SCHILLAK S, The comparison of the reference frames ITRF2000 and ITRF2005 in the determination SLR station positions and velocities, Geophysical Research Ab-stracts, Vol.10, EGU2008-A-03520, 2008.

SCHILLAK S, LEHMANN M, The com-parison of the station coordinates between SLR and GPS in the period 1999.0-2004.0. Abstracts 37th COSPAR Scientific Assembly, PSD1-0021-08, 2008.

SCHREIBER R, Search for dayside AKR sources. EPSC Abstracts, Vol. 3, EPSC2008-A-00505, 2008.

SCHREIBER R, Ciekawe strony interne-towe. Urania Postepy Astronomii, Nos. 1-6, 2008.

SCHREIBER R, Google Earth-Sky. Urania Postepy Astronomii, No. 2, p. 75, 2008.

SCHREIBER R, Tajemnice ob³oków srebrzystych. Urania Postepy Astronomii, No. 6, p. 255, 2008.

STANIS£AWSKA I, Belehaki A, The state of the art in space weather observational activities and data management in Europe, COST 724 Final Report, COST Office, 423-430, 2008.

STANIS£AWSKA I, KIRAGA A, ROTH-KAEHL H, ŒWI¥TEK A, Plasma influence on propagation parameters on VHF and

thUHF frequencies, Proc. IES2008, 12 International Ionospheric Effects Symposium, 126-127, 2008.

STANIS£AWSKA I, Lastovicka J, Bour-dillon A, Zolesi B, European monitoring and modeling activity in MIERS, Proc.

thIES2008, 12 International Ionospheric Effects Symposium, 144-148, 2008.

STANIS£AWSKA I, Lastovicka J, Bour-dillon A, Zolesi B, Models and observations of the ionosphere in the frame of European Action COST 296, Radio Sci, submitted, 2008.

Treumann RA, K£OS Z, Parrot M, Physics of Electric Discharges in Atmospheric Gases. Space Science Series of ISSI, Vol. 30, Springer, 2008.

Usowicz B, MARCZEWSKI W, Lipiec J, Usowicz JB, Soko³owska Z, D¹bkowska-Naskrêt H, Hajnos M, £ukowski MI. Soil moisture spatial distribution at the SMOS Cal/Val Campaign POLESIE (AO-3275) in Poland, Geophysical Research Abstracts, Vol. 10, EGU2008-A-07145, 2008.

Usowicz B, MARCZEWSKI W, Lipiec J, Usowicz JB, Soko³owska Z, D¹bkowska-Naskrêt H, Hajnos M., £ukowski MI, Spa-tial variability of soil texture and wetness: effects on thermal conductivity. EURO-SOIL 2008 Book of Abstracts, p. 253, 2008.

Usowicz B, MARCZEWSKI W, Usowicz JB. The thermal conductivity of the porous soil media, Geophysical Research Abstracts, Vol. 10, EGU2008-A-07166, 2008.

WAJER P, Long-Term Evolution of the Earth's Co-Orbital Asteroids. LPI Contri-butions, 1405:8122, 2008.

36

37

ZIO£KOWSKI K, L¹dowanie na Tytanie. Delta, No. 1(404), pp. 8-9, 2008.

ZIO£KOWSKI K, Misja Hayabusa, czyli kosmiczne perypetie japoñskiego soko³a. Urania Postepy Astronomii, No. 1(733), pp. 12-17, 2008.

ZIO£KOWSKI K, Five Biographies. In: Sylwetki Astronomów Polskich XX w., ed. A. Woszczyk, p. 28, 2008.

B£ÊCKI J, Parrot M, WRONOWSKI R, ELF and VLF signatures of sprites registered onboard the low altitude satellite DEMETER. Geophysical Research Letters.

BRZEZIÑSKI A, Recent advances in observation and modeling of Earth rota-tion: an overview. Reports on Geodesy.

BRZEZIÑSKI A, Recent advances in the-oretical modeling and observation of Earth rotation at daily and subdaily periods. Proc. Journées 2008, Systèmes de référence spatio-temporels.

BRZEZIÑSKI A, Ma C, Dehant V, Defra-igne P, Dickey JO, Cheng-Li Huang, Sou-chay J, Vondrak J, Charlot P, Richter B, Schuh H, Commission 19 "Rotation of the Earth" triennial report 2006-2009, Reports on Astronomy 2006-2009. Transactions IAU, ed. K. A. van der Hucht, Vol. XXVIIA.

BRZEZIÑSKI A, NASTULA J, KO£A-CZEK B, Seasonal excitation of Earth rota-tion estimated from recent geophysical models and observations, Journal of Geodynamics.

Papers in press or submitted for

publication:

Davidsson BJR, Guti'errez PJ, RICKMAN H, Physical Properties of Morphological Units on Comet 9P/Tempel 1 Derived from Near-IR Deep Impact Spectra. Icarus.

Fouchard M, RICKMAN H, Froeschlé CH, Valsecchi GB, Preliminary study on stellar perturbations of the Oort comet cloud. Publ. Astron. Obs. Belgrade.

KOSEK W, Rzeszótko A, Popiñski W, Contribution of wide-band oscillations excited by the fluid excitation functions to the prediction errors of the pole coordinates data. Proc. Journées 2008, Systèmes de référence spatio-temporels.

KOSEK W, Popiñski W, Rzeszótko A, An influence of wide-band oscillations in pole coordinates caused by atmospheric, ocean and hydrology excitation functions on their prediction errors. Reports on Geodesy.

LEJBA P, SCHILLAK S, Determination of the SLR station coordinates and velocities on the basis of laser observations of low satellites, Proc. 16th International Workshop on Laser Ranging.

MACEK WM, Chaos and Multifractals in the Solar Wind, Advances in Space Research.

MACEK WM, WAWRZASZEK A, Hada T, Multiscale Multifractal Intermittent Tur-bulence in Space Plasmas. J. Plasma Fusion Res. Series.

MARCZEWSKI W, Usowicz B, D¥BRO-WSKI B, WAWRZASZEK R, Sendek E, On the use of the fourier number to inter-pret thermal measurements with a quasi-linear heat source. Proc. of the 2nd Workshop on Penetrometry in the Solar System.

38

Mendes Cerveira PJ, Boehm J, Schuh H, Kluegel T, Velikoseltsev A, Schreiber KU, BRZEZIÑSKI A, Earth Rotation observed by Very Long Baseline Interferometry and Ring Laser. Pure Appl. Geophys.

NIEDZIELSKI T, KOSEK W, Regional sea level prediction and its relation to El Nino Southern Oscillation. Proc. Journées 2008, Systèmes de référence spatio-temporels.

RICKMAN H, Cometary Dynamics. Lec-ture Notes in Physics.

ROTHKAEHL H, Trotignon J-G, Decre-au P, B£ÊCKI J, Pitout F, Reme H, HF wave activity in the low and middle-altitude polar cusp. Advances in Space Research.

Rzeszótko A, KOSEK W, Popiñski W, Comparison of time-frequency characte-ristics between geodetic and geophysical excitation functions of polar motion. Proc. Journées 2008, Systèmes de référence spatio-temporels.

SCHILLAK S, BARTOSZAK J, MICHA-£EK P, The upgrading of the Borowiec SLR station. Proc. 16th International Workshop on Laser Ranging.

SCHILLAK S, LEHMANN M, The com-parison of the station coordinates between SLR and GPS, Proc. 16th International Workshop on Laser Ranging.

Sen AK, NIEDZIELSKI T, KOSEK W, Is length of day time series normally distributed? Proc. Journées 2008, Systèmes de référence spatio-temporels.

Invited papers delivered at the international science conferences and

meetings:

B£ÊCKI J, Savin S, Project STRUCTURA – observation of superdiffusion by compa-ring Cluster, Interball and Geotail data. Dni Nauki Polskiej, Moscow (Russia), 1-7 Octo-ber, 2008.

BRZEZIÑSKI A, Diurnal and subdiurnal signals in polar motion and UT1: theo-retical developments and observational ef-forts. European Geosciences Union Gene-ral Assembly 2008, Vienna (Austria), 13–18 April, 2008.

BRZEZIÑSKI A, Recent advances in theoretical modeling and observation of Earth rotation at daily and subdaily periods. Journées 2008 “Systèmes de référence spatio-temporels”, and X. Lohrmann-Kolloquium "Astrometry, Geodynamics and Astronomical Reference Systems", Dresden (Germany), 22-24 September, 2008.

BRZEZIÑSKI A, Recent advances in obser-vation and modeling of Earth rotation: an overview, International Seminar "Studies of the Earth Crust Deformation in Central Europe", Warsaw, 29-30 September, 2008.

BZOWSKI M, Ionization rates, radiation pressure, and ENA survival probabilites, invited talk presented at IBEX Science Team Working Meeting, Boston MA, 19-20 June, 2008.

39

BZOWSKI M, Influence of the Sun on the interplanetary hydrogen/helium atoms. Solar wind data as inputs for the models, invited talk presented at a meeting of the International Space Science Institute Wor-king Group "Cross-calibration of past FUV experiments", Bern, Switzerland, 24-26 November 2008.

CZECHOWSKI A, Distant heliosphere: Theories and observations, Symposium “Solar Activity, Heliosphere and Solar-Terrestrial Relations”, St. Petersburg 13 - 17 October 2008.

H£OND M, BZOWSKI M, O'Neil M., Moebius E, Star Sensor (IBEX-Lo) Signal Simulation and Spin Axis Determination Software. IBEX Science Working Team Meeting, Boston (USA), 19-20 June, 2008.

K£OS Z, Atmospheric electrity: Current status of knowledge, Symposium “Solar Activity, Heliosphere and Solar-Terrestrial Relations”, St. Petersburg 13 - 17 October 2008.

ROTHKAEHL H, Earth's electromagnetic environment – a challenge for space rese-arch and technological applications. 7th LOIS Workshop, Växjö (Sweden), 16-18, June 2008.

ROTHKAEHL H, Project DIAGNO-STYKA, Dni Nauki Polskiej, Moscow (Russia), 1-7 October, 2008.

Savin S, Budaev V, Amata E, Zelenyi L, Treumann R, Consolini G, Yordanova E, Khotyaintsev Y, B£ÊCKI J, Rauch J-L, Observation of superdiffusion by compa-ring Cluster, Interball and Geotail data. 37-th COSPAR Scientific Assembly, Montreal (Canada), 13-20 July, 2008.

SCHREIBER R, Search for dayside AKR sources. European Planetary Sciences Con-gress 2008, Muenster (Germany), 21-27 September, 2008.

STANIS£AWSKA I, KIRAGA A, ROTH-KAEHL H, ŒWI¥TEK A, Plasma influen-ce on propagation parameters on VHF and UHF frequencies. 12th International Iono-spheric Effects Symposium, Alexandria (USA), 13-15 May, 2008.

STANIS£AWSKA I, Lastovicka J, Bour-dillon A, Zolesi B, European ionospheric monitoring and modelling activity in MIERS. 12th International Ionospheric Effects Symposium, Alexandria (USA), 13-15 May, 2008.

STANIS£AWSKA I, “Space weather - an international affair”, Symposium “Solar Activity, Heliosphere and Solar-Terrestrial Relations”, St. Petersburg 13 - 17 October 2008.

SYLWESTER J, Ongoing and future solar X-ray experimenting at the Solar Physics Division of Polish Space Research Centre. RAS National Astronomy Meeting, Bur-lington House, London (UK), 9 May, 2008.

SYLWESTER J, The Sun in X-rays, Sympo-sium “Solar Activity, Heliosphere and Solar-Terrestrial Relations”, St. Petersburg 13 - 17 October 2008.

WERNIK AW, Scintillation measurements as a means for diagnosis of ionospheric plasma irregularities. Workshop on Iono-spheric Scintillation: Scientific Aspects, Space Weather Applications and Services, Nottingham (UK), 20-22 February, 2008.

GENERAL INFORMATION

Staff

At the end of 2008 the Space Research Centre employed 116 persons of whom 8 professors, 17 habilitated doctors and 19 PhD research associates.

M. KRÓLIKOWSKA-SO£TAN and H. ROTHKAEHL were awarded with habilitated doctor degree in Physics by the Scientific Council of the Space Research Centre. A. KÊPA was awarded with PhD degree.

J. SYLWESTER was elected as an Honorary Fellow of the Royal Astronomical Society. M. BANASZKIEWICZ and J. SYLWESTER were awarded with the Keldysh Medal and J. JUCHNIEWICZ was awarded with the Tsiolkovsky Medal by the Cosmonautics Federation of Russia.

Finances

The major source of financing of the Space Research Centre comes from the state budget (ca. 75%). The SRC budget in 2007 was 10012 thousands PLN. The budget structure was following: basic allocation – 57.1%, national grants – 23.3% , EU grants – 6%, contracts (national and international) – 8.1%, other sources – 5.5%.

Grants and Contracts

In the Space Research Centre 41 grants (31 from the Ministry of Science, and 10 SPUBs – Special Research Projects to support international cooperation) and 47 contracts (24 national and 23 foreign) were carried out in 2008.

International cooperation

In 2008 the Space Research Centre was involved in cooperative projects and grants with 34 organizations from 15 countries, and 2 new agreements on international cooperation were signed.

thIn 2008 the Space Research Centre organized 5 international meetings (e.g. 16 International Workshop on Laser Ranging in Poznañ, 13-17 October, in which 144 scientists from 20 countries participated and more than 120 papers were presented, and two workshops in Wroc³aw on Coronas-Photon and STIX-SphinX, 31 August – 2 September and 9 – 12 December, attended by altogether 60 researchers who presented about 60 talks).

During the report year the SRC scientists participated in many international conferences, e.g. 37-th COSPAR Scientific Assembly, Montreal, Canada; International Astronautical Congress, Glasgow, UK; XXIX URSI General Assembly, Chicago, USA; American Geophysical Union 2008 Fall Meeting, San Francisco, USA; European Geosciences Union General Assembly 2008, Vienna, Austria; European Planetary Science Congress 2008, Münster, Germany; Journées 2008 “Systèmes de référence spatio-temporels” and X. Lohrmann-Kolloquium "Astrometry, Geodynamics and Astronomical Reference Systems", Dresden, Germany; Earth Tides Symposium 2008 "New Challenges in Earth's Dynamics", Jena, Germany.

40

Educational and promotional activity

The number of students registered in the Doctoral Studies carried out in the Space Research Centre in 2008 was 15, and 6 persons (B. D¥BROWSKI, J. GURGUREWICZ, D. KUCHARSKI, T. NIEDZIELSKI, K. SEWERYN, S. TARNOPOLSKI) were awarded with PhD degree.

SRC cooperates with universities and higher schools in student training (e.g. academic lectures by 3 SRC scientists in 2008) and makes its laboratories available for their practice and graduation works (e.g. 7 students worked on their graduation thesis in 2008).

The Space Research Centre participated in the 12th Science Picnic in Warsaw (June 2008) and in the XII Science Festival in Warsaw (September 2008), and in similar events in Wroc³aw, Poznañ, Toruñ, Wa³brzych. The SRC scientists participated also in Fifth European Space Weather Week (November 2008) in Brussels. The SRC co-organized Polish Science Days in Moscow (October 2008) and together with the Space Research Institute RAS prepared an exhibition illustrating 30 year long cooperation in space between Polish and Russian institutes.

Some of the SRC staff members were reviewers or consultants in many scientific popular magazines, and organizers of scientific competitions addressed to young people. The SRC scientists delivered a lot of public lectures and participated in many TV and radio programmes.

SRC published the first Polish edition of the book “Science of Space Environment” by Tadanori Ondoh and Katsuhide Marubashi (eds.) being the first handbook in Polish language for students in the fields related to space exploitation.

41

CONTENTS

03 .......... SUMMARY 200805 .......... SPACE PROJECTS11 .......... DATA ACQUISITION16 .......... INTERPRETATION AND MODELLING25 .......... APPLICATIONS29 .......... PUBLICATIONS40 .......... GENERAL INFORMATION

Edited by:KRZYSZTOF ZIO£KOWSKI

Technical editor:EDYTA LISIECKA

Publikacjê wykonano na papierze bezchlorowym POLARIS 100 gr.Ok³adkê wykonano na papierze kredowanym Magnomatt 200 gr.

Sk³ad: Edyta LisieckaDruk i oprawa: CBK PAN

00-716 Warszawa, ul. Bartycka 18a

Cover: The SRC contribution to the SIR-2 instrumentfor the Chandrayaan-1 lunar mission.