List of lectures below

Low-mass eclipsing binaries in the ASAS database

K and M type stars, despite beeing the most numerous in the Galaxy, are surprisingly poorly known. Our knowledge of the physics of their interiors, especially the phenomenon of convection, or the molecular opacity, is based on weak assumptions and estimations. We do not fully understand the influence of activity and rotation on K and M type stars' evolution. Recently we improved our evolutionary models, but to test them, we need to precisely derive such a fundamental parameters like mass, radius or temperature. Perfect objects for this purpose are detached eclipsing binaries (DEBs). Unfortunatelly, we don't know many of late type DEBs, and half of them have their parameters calculated with poor accuracy. In my lecture I will present results of my small survey of the eclipsing binaries in the {\it All Sky Automated Survey} database. I will show some new discoveries of late type systems, as well as models and derived parameters of few interesting objects.

Observation of 3c454.3 with the Fermi-LAT Telescope

The Gamma ray Large Area Space Telescope (GLAST) has been successfully launched on 11 June 2008 and then renamed in Fermi Gamma Ray Space Telescope after starting its scientific mission on 11 August, 2008. Large Area Telescope (LAT) and GLAST Burst Monitor (GBM) are the two instruments on board on the Fermi satellite. Fermi-LAT is a pair-conversion gamma-ray telescope sensitive to photon energies from about 20 MeV to above 300 GeV. It is a new-generation detector which provides an unprecedented sensitivity in the gamma-ray and which explores the energy range of MeV-GeV band, including a part of the electromagnetic spectrum still not covered by any other instrument. Two of the main subjects of observational cosmology that can be studied by the LAT are the luminosity functions of AGNs and the diffuse backgrounds. Evaluating the luminosity function of AGNs is a major task now, because only a few AGNs were detected also at higher energies. Things are rapidly changing now after Fermi's launch: Just 43 days after launch, the LAT dispatched its first ATel on 3c454.3, an AGN (24/7/2008: ATel #1628). This presentation aims precisely at modelling AGN spectra in the LAT energy range: on the one hand, it exploits LAT data to build a phenomenological model of medium-high redshift AGNs. These AGNs present, at LAT energies, a bent spectrum as a result of the absorption by means of the EBL, in such a way that understanding the model may shed light both on AGNs and on the EBL itself. On the other hand, it will also pave the road to the future calibration of TeV experiments, that can only be accomplished by comparing the data around 100 GeV, an energy within reach both by LAT and by Cherenkov experiments.

Giant Radio Galaxies as probes of radio sources and the IGM evolution.

Galaxies with active galactic nuclei are usually powerful synchrotron emitters. A small fraction of radio galaxies with linear sizes of more than 1 Mpc represent the biggest single objects in the universe. Giant radio galaxies (GRGs) are extremely important for better understanding the last stages of evolution of RGs and their host galaxies, constraining the analytical models of their time evolution. In addition, by observing them we may acquire important information about the composition of the intergalactic medium on scales comparable to those of cluster of galaxies or larger. Unfortunately, steep radio spectra and low surface-brightness of such sources make them difficult to observe. Here, a new sample of large sized, high-redshifted radio galaxies has been presented and used to constrain the dynamical model of jet propagation through two media environment surrounding the host galaxy (AGN).

Microwave spectroscopy as a tool for studying the properties of active cometary nuclei

I will start with presenting a new model of spectral-line profiles as observed in comets at microwaves. The model is a self-consistent fully time-dependent construction, accounting for several properties of the cometary nucleus. These include the rotation period, spin-axis orientation, and activity pattern of the surface. In the second part I will demonstrate how these properties manifest themselves in the spectra of comet 8P/Tuttle. I will also present results of retrieving them using the model presented earlier.

Generation of TeV gamma-ray radiation in the SNRs. The case IC 443.

Supernova remnants (SNRs) are believed to be the sites of Galactic cosmic ray (CR) acceleration. The strong shocks in SNRs can accelerate electrons, protons and nuclei. Some shell-type SNRs have been detected at TeV energies, as expected if they indeed are the sources of CRs. Besides inverse Compton process, TeV gamma-rays can originate from the decay of neutral pions produced in nonelastic collisions between the accelerated protons (nuclei) and swept up by the SNR shock ISM particles. In the present work we examine a model of interaction of the ultrarelativistic particles accelerated in the SNR IC 443 with molecular clouds, situated inside or outside SNR. We evaluate the SNR and cloud parameters from comparison of predicted and observed fluxes of TeV gamma-ray radiation.

Calculation and Visualisation of Coronal Magnetic Field during 2006 and 2008 Total Solar Eclipses

Coronal magnetic field was calculated by a potential field extrapolation using a Potential Source Surface (PSS) model. Wilcox Solar Observatory photospheric magnetic field data for Carrington rotations 2040-2042 and 2072-2073 were used. Coronal magnetic field charts at the source-surface distance were plotted. We used the radial and classical approaches to calculate spherical harmonic coefficients and magnetic field lines in the Sun’s corona. Observed structure of the solar corona and calculated coronal magnetic field were compared and analyzed.

Divulgation of scientific knowledge: The Lara State Astronomy Association Experience

Latin American and Caribbean countries need to improve their emerging scientific development. One of the objectives of the Lara State Astronomy Association, located in Venezuela, is to develop extension activities toward the community, constituting a center of information and popularization of the Astronomy, through of the promote of the study of Astronomy, basic sciences among students of Lara State Elementary Education. Events like Space Baptism and Astronomy in the classroom encourage children interest in Astronomy, and from this point develop a scientific mentality that allows them to aquire conciusness of the characteristics and conditions about their place in the universe, with a vision of the problematic issues regarding earth climate and the necessary conciousness that should be assumed. Also, these activities put into practice cognoscitive values, originality and creativity as well as solidarity and cooperation.

Chemistry of impact events in the Solar system

The main principles of the quenching theory as a powerful tool for study of the chemical processes in the impact-produced hot clouds and fireballs are considered. Specific cases of impact events include collision between the comet Shoemaker-Levy 9 and Jupiter and collisions between comets and the Moon as a potential source of lunar polar volatiles. Micrometeoroid bombardment as a source of metal atoms (especially, Na, K, Ca, and Mg) in the exospheres of the Moon, Mercury, and Europa is discussed. The properties of impact-generated exospheres of atmosphereless bodies are estimated.

Two-field model of dark energy with canonical and non-canonical kinetic terms

The phantom divide crossing is not allowed for single fields with the simplest Lagrangians, however it is possible for the 2-field models of dark energy including both quintessence and phantom. We focus on the model given by Lagrangian with a canonical kinetic term and a Dirac-Born-Infeld one: $L=-\frac{1}{2}\phi_{;i}\phi^{;i}-U(\phi,\xi)\sqrt{1-\xi_{;i}\xi^{;i}}$. For such case the potentials $U(\phi,\xi)$ are reconstructed using the modern observational data. The existing ambiguities and necessary additional assumptions are dicussed.

The investigation of HII region optical spectra of the BCD galaxy IC4662

The investigation of HII region optical spectra of the BCD galaxy IC4662 is presented in this paper. Spectral data were obtained at ESO VLT. This spectra includes such bright emission lines as H beta 4861, OIII 4363, 4959, 5007 etc. During the research were derived O and N chemical abundances and obtained the number of WR-stars in the most bright areas of HII region. Also we studied kinematics of ionized gas of HII region of the galaxy.

General Magnetic Field of the Sun as a Star

The amplitude of General Magnetic Field of the Sun as a Star (GMFSS) shows changes with 11-years cycle of activity. In maximum of solar activity the value of GMFSS is maximal, in minimum of activity is minimal. The values of magnetic periods of solar axial rotation vary from cycle to cycle of sunspot activity. Resulting magnetic field of GMFSS is non equal to zero during four solar activity cycles of observations (two solar magnetic cycles). The ratio between positive and negative magnetic fluxes is approximately equal to 1, i.e. GMFSS is a real large-scale magnetic field.

AMATEUR ASTRONOMER’S ROLE IN THE DEVELOPMENT OF THE ASTRONOMICAL SCIENCE.

Since ancient times man has always gaze up at the sky to understand and seek answers to questions most troubling that remain so far. Where do we come from?, why are we here? and where to go?. In seeking answers to these, men devoted to the study of the sky as Galileo, Copernicus and Kepler. Also developed techniques, theories and extend knowledge of human society around the universe. In full observance of the International Year of Astronomy amateur astronomers spend their days and nights collecting data to better understand the operation of Cosmos. Amateur astronomy has greatly technified and has made major scientific contributions and discoveries of various bodies that help increase awareness of space. The thin line between amateur and professional is fading out even more, that allows the astronomical science to be one of the few that can bring both amateur and professional work together as one to increase human knowledge and the popularization of science in the most remote areas of our planet.

Hands-On Universe (HOU)

Hands-On Universe is a global educational program with an important objective to bring astronomy to the classroom. I had the honour to create an exercise about the detection of exoplanets with the method of transit, during an internship at the Observatory of Paris in January 2009. My aim during the talk is to introduce the organisation, as well as it's different objectives. Moreover, I will explain the work I did and how this program helps us all introduce astronomy to young children at school. Teachers are trained to use a specific software (SalsaJ) and thanks to HOU, every step is clearly explained to them, to enable them to easily sacrifice time to teach their students about astronomy. Hands-On Universe insists on the importance of science at school and uses real obserations and data acquired from robotic telescopes to motivate the pupils to learn the path of a researcher.

The outbursts properties of AM CVn stars

I will briefly summarize the observational properties of ultra-compact binaries called AM CVn stars, and analize their outbursts originating from thermal-viscous instability in helium accretion disc. I'll present our preliminary results in applying the model of Dwarf Novae outbursts to helium discs.

Polarimetry of Iapetus Near Opposition

We present results of polarimetric observations of Iapetus at phase angles ranging from 2; 4± to 4; 6±. The observations were carried out using 125-cm telescope equipped with the UBVRI double image chopping photoelectric polarimeter on the Crimean Astrophysical Observatory (Ukraine) on January 14 - April 9, 2008. Observed longitudes range from 54± to 146± and correspond to the dark leading side of the satellite. The phase-angle dependence of polarization and longitude dependence polarization of Iapetus were obtained using the results of our observations and all the data availible. Our results are in good agreement with previous observations and supplement them.

V473 Lyra: Spectroscopic determinations of effective temperatures and absolute stellar magnitudes in various phases.

In this report I would like to present a new spectroscopic research of the unique Cepheid V473 Lyra in 32 pulsation phases. It is based on high-resolution, high signal-to-noise echelle spectra which were obtained with ELODIE at 1.93m telescope of OHP (1994-1995 observational series). The extremely high precision of the effective temperature determination (10-30 K) is achieved by using the line-depth ratio method (Kovtyukh, 2007). Also the absolute magnitudes are achieved by using a new method based on line-intensity ratios (suggested by Kovtyukh and Chekhonadskikh, 2008). Presumably, the accuracy of luminosity determination is estimated as 0.2-0.3 mag. Pulsation modes are still discussed.

Aerodynamical properties of fragments of a meteor body in the terrestrial atmosphere

We certainly know that the part of meteoric bodies collapses in the atmosphere. How the swarm of fragments will evolve it depends on many factors: height and velocity at the moment of destruction, the sizes of splinters and properties of a material of a body. Interaction of the shock waves formed in front of the fragments may lead to both increase and decrease of the total cross section [1]. The solution of this problem should be based on aerodynamic properties of systems of bodies in a supersonic flow. The present work is devoted to research of a mutual influence of bodies in a supersonic flow. Aerodynamic properties of configurations of two spherical fragments of different radii are considered and systematized. By means of numerical calculations a pressure distribution is found in a flow around fragments at their various positions relative to each other. Dependences of coefficients of lateral force and drag force on an angle between a center line and incoming flow for various distances between bodies are constructed. The basic aerodynamic properties of group of bodies in a supersonic flow are emphasized. The collimation effect is shown on a certain range of angles, smaller fragments are involved in the wake of the leading one. In case of fragments of the different size the collimation effect shown for smaller bodies on a wider range of angles. Resistance of the body in the wake is considerably smaller then resistance of the leading one except for positions where the shock wave of first body falls on the frontal surface of the backward one. External fragments separate primary from the central part of a swarm [3]. These properties allow to designate the most probable configurations of fragments in the atmosphere depending on destruction conditions. For example, if a meteoric body collapses on a few (from two to five-six) almost identical parts, most likely they disperse in a transverse direction and will move further independently. When meteoroid collapses on many splinters having one largest fragment, it becomes a leading one and smaller fragments are involved in its trace, the needle model is realized. If several largest (almost the same size) splinters appear all swarm can be divided into trains with greatest fragments at the head [4]. In a case when meteoroid is of a fragile material it collapses on great number of small splinters. They will move most likely as a cloud with consecutive separation of external fragments which will be involved in a trace of this cloud. Surely, dynamics of fragments in atmosphere can be more complicated. However the described configurations are basic ones in a process of evolution of a fragments swarm. This work was supported by the Russian Foundation for Basic Research, project no. 07-01-00009. List of references Artem’eva N.A., Shuvalov V.V. Interaction of shock waves during the passage of a disrupted meteoroid through the atmosphere // Shock Waves 1996. V 5. P. 359–367. Laurence S.J., Deiterdingand R., Hornung H.G. Proximal bodies in hypersonic flow // J. Fluid Mechanics 2007. V.590. P. 209–237 Zhdan I.A., Stulov V.P., Stulov P.V. 3D configurations of broken body fragments in a supersonic flow // Dokl. Phys.2005. V 50, № 10, P. 514–518. Artem’eva N.A, Shuvalov V.V. Motion of a fragmented meteoroid through the planetary atmosphere // J. Geophys. Res. 2001. V. 106. № E2. P. 3297–3309

Identification of X-ray and gamma sources in the optical bad

High energy astronomy, although quite a young area, is one of the esseintial parts of astronomy studying variety of exotic objects all the way to cosmological distances. Despite rapid advances in this field the detectors of high energy photons still have poor accuracy compared to optical ones which makes it difficult to identify objects in more spectral bands and therefore prevents us to carry out broadband spectroscopy -- the most powerful tool we have to study these objects. In my lecture I would like to present several methods how to identify high-energy sources in the optical data (thus data obtained by common telescope and CCD).

Project Solaris: Circumbinary Exoplanets

The area of research in extrasolar planets appears to engender a great deal of interest nowadays and numerous observations continue to be conducted in this field. It seems that it is only a question of time before the new circumbinary planets are discovered. Timing and eclipses have been well known for years, but when combined with massive photometry and recent improvement in the robotic telescopes, new possibilities arise. Project Solaris is the network of fully autonomous photometric telescopes located in the south hemisphere which are going to constantly monitor hundreds of eclipsing binaries potentially harboring extrasolar planets. We utilize all the scientific and equipment progress made till now. In my presentation the current state of Project Solaris as well as the potential of the eclipses timing are elaborated on.

Spectral synthesis of astronomical images.

Spectral synthesis in other words is preparing colorful images of deep space objects. The realistic projection is as well accentuated as the aesthetic appearance. These images are really powerfull tool when it comes to popularization of astronomy and communication with public. The main part of process of making these is work with raw images which are taken as monochromatic ones by CCD detector. In the lecture, I would like to present basics of making full colored image, which includes some technical details about image takingg, proces of the synthesis and finaly coloring final image without being unrealistic. Usefull software as well as new technics and handy advice will be discused.

MIDI/VLTI-Infrared Interferometry of the young, massive star Allen's Source

Allen's Source is a young star with a mass of 9.5 solar masses, therefore belonging to the intermediate to high-mass stars. Our knowledge about the formation of high-mass stars is still very limited. With a distance of 760 pc Allen's Source provides the unique possibility to investigate its circumstellar environment on scales of few AU. With MIDI, the mid-infrared instrument of ESO's Very Large Telescope Interferometer (VLTI), spectral dispersed Michelson interferograms of Allen's Source were taken at wavelengths between 8 and 13 micron. For the interpretation of the data the radiative transfer code DUSTY was employed to extract physical parameters of a possible circumstellar envelope. Furthermore, a temperature-gradient model for a possible disk around the object was tested.

Analysis and classification of variable stars in the "Pi of theSky" Project

One of the goal of the "Pi of the Sky" project is to observe and analyze variable stars. Based on data collected during 2006 and 2007 observing seasons, we have analyzed over 10 mln stars and preliminary results show detection of 635 variable stars. This lecture presents the analysis of the photometric data and classification of variable stars found in this data set. We have determined period using the AoV algorithm (Szwarzenberg- Czerny, 1989) and checked period in the range from 0.01 to 50 days. After visual investigation of the shape of the light curve we have classified the type of the variability. The results will be presented in the second edition of the variable stars catalogue.

Science with small telescopes - exoplanets

The search for extrasolar planets has become one of the most attractive problems in modern astrophysics. The biggest observatories in the world are involved in this task as well as little amateur instruments. There is also a huge variety of astronomical methods used for their investigation. Here I will talk about the projects for searching for exoplanets by transit method and our observations of the planet WASP-2b. We observed a transit on 3/4 August 2008 with a 354 mm Schmidt-Cassegrain Celestron telescope and CCD SBIG STL 11000M camera. By precise photometry made using MaximDL software we obtained the light curve of the star system. Decrease of brightness by 0.02m is detected. Analyzing our data we estimate the radius of the planet and inclination of its orbit. Our results are in good correlation with the published information in literature. Finally, I discuss the possible error sources.

Photometrical investigation of the shell galaxy NGC 474

The shell galaxies are a subclass of the peculiar galaxies. In the majority of the cases these galaxies are elliptical or lenticular. They are surrounded by arcs or shells of matter, which origin is still debated. Numerical simulations confirm two models for shell formation. According to the first they are a result of merging of two galaxies, which mass is low (elliptical or lenticular). The second model states, that shells form without merging but because of close tidal interaction between two galaxies. In each case one of the two scenarios is realized. In this paper I present the results of my photometrical exploration of galaxy NGC 474. It is based on CCD images, taken in standard broad-band filters. Firstly, I have examined the surface brightness of NGC 474 as a function of the distance from the center, in each filter. The obtained profiles are typical for a lenticular galaxy. Then I plotted the analogical diagrams for the color indices. According to my measurements, they are consistent with those of its shells. This implies, that their origin is not due to merging between two galaxies, but they are gravitationally liberated matter from the satellite galaxy NGC 470.

Partially Screened Gap - general approach and observational consequences

Observations of thermal X-ray emission from radio pulsars implicate that in most cases surface hot-spot is much smaller than polar cap defined under the assumption that magnetic field of pulsars is dipolar. Most plausible explanation is that surface magnetic field above the polar cap is non-dipolar and much stronger. Assuming that the magnetic flux of the open field lines is conserved, we can determine magnetic field at the surface - for the observed pulsars it is of the order of $10^{14}$G. We discuss the Partially Screened Gap (PSG) model which implies that the temperature of the polar cap surface is almost equal to the so called critical temperature. For these conditions sub-Goldreich-Julian thermionic flow of iron ions or electrons coexists resulting in partial screening of the polar gap. We present the observed values of black body temperature and bolometric surface of X-ray emission for a number of pulsars. The results of our analysis show that the PSG model is suitable to explain both cases: when bolometric surface is smaller or larger then conventional polar cap. For the second case both the structure and curvature of the field lines is such that allows the pair creation in the closed field line region thus heating the surface outside actual polar cap.

The hidden transition from AGB to post-AGB stars as observed by AKARI

When intermediate mass stars experience their final nuclear burning stage, they have reached the asymptotic giant branch (AGB) in the Hertzsprung-Russell diagram (HRD). Here they lose a major part of its mass and exhibit much higher luminosities than their main-sequence progenitors. It is the mass-loss process, which leads to the formation of stellar winds causing the total obscuration of the central star in the optical wavelength range. For an astronomically short while, the star is observable only in the infrared, since a circumstellar envelope consisting of the recently ejected matter absorbs all the optical radiation emerging from the star and reemits it in the infrared. When the star has lost its entire stellar envelope, the mass-loss process stops and the star reappears in the optical. It has now reached the post-AGB stage and is about to create one of the most fascinating phenomena of the sky, a planetary nebula. Circumstellar envelopes of post-AGB stars exhibit a variety of axis- or point-symmetrical structures, while the mass outflow on the AGB proceeds in a radial symmetric way. To investigate what is happening in the short time of obscuration between the AGB and the post-AGB stage, AKARI/IRC observations of 13 IRAS-selected candidate stars for the "hidden" transition stage were analyzed. Results of this analysis, including implications on shell chemistry and the final phase of AGB evolution, will be presented.

H.E.S.S. observations of PKS 2155-304

H.E.S.S. is a system of Imaging Atmospheric Cherenkov Telescopes that investigates cosmic gamma rays in the 100 GeV to 100 TeV energy range. This experiment allows to detect Very High Energy photons coming from many different objects. One of them are blazars, a subclass of active and radio loud galaxies, which jet axis is oriented toward an observer. This objects are well known for their brightness variability in whole EM spectrum. I present results of detailed analysis of gamma ray flux variability for one of the blazars, PKS 2155-304. Observational data in years 2004-2008 are obtained by the H.E.S.S. experiment. To verify the short and long term variability the observational data are binned in different timescales. Obtained light curves show variations of the signal in the case of all studied time scales. On the light curves I reproduce a flare from year 2006 (Aharonian et al. 2007) and I find that probably in year 2007 might happened a following flare, however the lack of observations does not allow to state it straightforward. Using optical observations obtained by ATOM telescope a correlation with the gamma ray flux is tested. Detailed study of the gamma ray flux with respect to an optical brightness does not reveal any dependence.

The Radiative Transfer Problem

To understand the physics behind an astronomical observation, we have to compute synthetic spectra and compare them with the observed ones. This requires a theory, which describes the physics of the stellar or planetary atmosphere the light originates from. The theory of radiative transport is crucial for this problem, because it describes how radiation is transported from the inner regions to the outer layers of an atmosphere. Therefore, the radiative transfer equation has to be solved. This a demanding task, because of the loss of radiative energy into space, assumptions of a thermodynamic equilibrium are not valid. The non-local nature of interaction processes between the radiation and the matter in an atmosphere causes the basic physical quantities of the theory to be connected mostly non-linear. We present the basic theory behind a model atmosphere and the radiative transfer problem as well as a numerical solution scheme.

Prompt optical observations of GRB 080319B with "Pi of the Sky" detector

"Pi of the Sky" experiment has been designed for continuous observations of large parts of the sky, in search for short-timescale astrophysical phenomena, in particular for prompt optical counterparts of Gamma Ray Bursts (GRBs). Other scientific goals include searching for novae and supernovae stars and monitoring of blasars and AGNs activity. The prototype aparatus is working since July 2004 in the Las Campanas Observatory, the full is now under construction and is expected to become operational next year. I will present the "Pi of the Sky" full system as well as a prototype. On 19th of March 2008 the "Pi of the Sky" prototype observed the prompt optical emission from long-duration gamma ray burst GRB080319B. Later measurements proved that the burst occurred at the redshift z=0.937. However, the optical flash was so strong that for about 40 seconds it could have even been seen with a naked eye, without any instruments. For this reason the GRB 080319B burst is became famous as the "naked-eye burst". Observations of the prompt emission of this burst challenged the existing models of GRB emission and demonstrated the usefulness of wide-field detectors. I plan to present our measurements, to show how the fast detection of the GRB080319B was possible and discuss why it was so crucial for the models of the GRB emission mechanism.

Stars in dusty galaxies.

Far-infrared galaxy surveys provide us with a powerful tool to investigate the evolution of the star-formation history in the Universe, since they measure thermal emission from dust heated by the UV light from stars. One of such deep surveys has been carried out recently by the FIS instrument onboard the AKARI satellite, at wavelengths: 65, 90, 140 and 160 micrometers. The region around the Southern Ecliptiptic Pole, selected for this survey, is unique because the cirrus density there is the lowest in the whole sky. It is named AKARI Deep Field South (ADF-S). In the ADF-S, almost 2200 sources were successfully detected down to ~20 mJy at 90 micrometers. A search for counterparts in other wavelengths, carried out in public databases (NED, SIMBAD) for 500 ADF-S sources brighter than 48.2 mJy at 90 micrometers resulted in identification of 330 counterparts, among them 314 known galaxies. In order to understand the relation between the far-infrared emission from dust and UV emission from young stars in these objects, we have carried out a search for the UV images of the identified galaxies in the GALEX public database and measured their fluxes in near and far UV. I plan to present the identification and measurement process, as well as the conclusions obtained from the common analysis of the IR and UV data for these galaxies. Results provide us with better understanding of relations between newly born stars and dust surrounding them in star forming galaxies.

Cosmological Implications of the SDSS and 2dF Redshift–Population Histograms

Empirical observation of galaxy population density in redshift space is inconsistent with expectations based on the canonical cosmological model. The magnitude of this inconsistency implies a significant error in the canonical model’s theoretical redshift-distance relationship. A new model has been derived that rests on first principles and which is consistent with observed galaxy population density in redshift space. Additionally, the observed Type Ia supernovae redshift-luminosity curve does not require interpretation as accelerating cosmic expansion. Moreover, the revised redshift–distance relationship of the proposed new model implies that the entire mass of early-type galaxies associated with observed Einstein rings is composed of normal matter; no “dark matter” need be assumed to exist in these systems.

Taylor and MEGNO -- proof of concept

Studying dynamics of extrasolar planets became a big challenge for nowadays astronomers. Several theoretical and numerical methods has been developed and applied. However, due to limited CPU time and huge space of unknown orbital parameter space of a planet, we need our methods to be both fast and accurate, which in practice means, that we have to achieve a compromise between speed and accuracy of the simulation. This is especially important in case of searching Earth-like bodies, which are currently unseen by direct observations. With numerical tools we can predict possible locations of such planets by studying dynamics of discovered bodies in the system, similar to discovering Neptune in 19th century. In our work we present a proof of concept of combining well-known Taylor Series Method and MEGNO fast stability indicator (Cincotta, Simó, 2000). We used Taylor package (Jorba \& Zou, 2004) as main numerical engine and compare it with ODEX (Gragg-Bulirsh-Stoer extrapolation method; Hairer \& Wanner 1995). We did our simulations for Solar System planets, $\nu And$ and $\gamma Cephei$ system, testing both the default step size and order control method, provided by the Taylor Package, and the Lagrange reminder method (Gozdziewski \& Maciejewski, 1995). In our work we used Poincare variables in full 3D dynamical model. We proofed that the Taylor Series Method can be competetive with classical methods, especially when used in problems where huge accuracy is desired (i.e. computing ephemerides). We created dynamical maps of $\gamma Cephei$ and confirmed direct 3D computations by Haghighipour (2006), showing, that it is possible for an Earth-like body to exist in this binary star system. For our purpose an interface for Taylor package has been developed. Simulations were done on Hydra Cluster machines (TCfA, NCU) and we achieved the accuracy at 12 significant numbers level for standard double precision of GCC4 compiler. This work was supported by Ministry of Science and Education grant No. 1P03D-021-29.

Iodine Cell as a tool for finding exoplanets

The radial velocity method is the most successful way of finding exoplantes. To detect Doppler shift of a host star high precision spectroscopy is needed. Iodine absorption cell is widely adopted approach to obtain precise measurements. I will present the technical aspects of iodine cells' construction, results of data collected using this technique, its contribution to finding extrasolar planets and basics of polish project of exoplanets in multiple stellar systems detection using this method.