List of posters below

Non-thermal images of SN 1006: from radio to gamma-rays

Supernova remnants (SNRs) are believed to be the main sources of galactic cosmic rays. Discovery of the non-thermal component in X-ray spectrum of SN 1006 in 1994 opens a new era in the investigation of SNRs. SN 1006 remains to be one of the most interesting objects for high-energy astrophysics. Electrons accelerated by the shock are the source of the non-thermal radiation in radio, X-rays (via synchrotron emission) and gamma-rays (via inverse-Compton process). Experimental images of SN 1006 are known in all these bands, including very-high energy gamma-ray range. An important task is therefore to model the distribution of the surface brightness of SNRs. We develop a method for synthesis of SNR maps due to non-thermal radiation of electrons in radio, X-rays and gamma-rays. In particular, the method takes into account the injection of particles and the behaviour of magnetic field at shock waves with different obliquities as well as the radiation losses of electrons downstream of the shock. The method is used to model images of SN 1006. Comparing the maps in different bands with observations, we can impose limitations on the number of theoretical hypotheses about electron injection and interstellar magnetic field orientation around SN 1006.

Formation of Primordial Molecules in the Early Universe

In the physical environment of the expanding Universe, molecules such us H2 and HD can be form and contribute the thermal evolution of the medium. The detailed description of the molecule formation in primordial multicomponent medium is considered. We analyze the evolution of relative number densities of free electrons, neutral and ionized atoms and molecules during Dark Ages. At decoupling epoch the amplitude of relative perturbations of electron number density is several times higher than amplitude of relative perturbations of total baryon density. The influence of this effect on evolution of perturbations of atom and molecular ionization fractions in the region of adiabatic matter density perturbations is discussed.

Reducing Abell 226 Optical Images using THELI Pipeline

In astronomy, raw images from CCD detectors are not immediately usable for scientific exploitation but are instead contaminated by several instrumental effects. Generally speaking, data reduction is the transformation of raw data into a more applicable form. Thus, this involves: • Removal of instrumental signatures, like dark current and field curvature. • Masking of unwanted signals, like cosmic rays, stellar halos and satellite tracks. • Photometric and Astrometric Calibration. • Coaddition of individual frames. in this poster [which also can be followed by a talk] we describe one of the methods available to automatically reduce large amount of data. We also present our own work with Abell 226 Optical Images.

XMM-Newton and Swift X-Ray Observations of Active Galacic Nucleus

We present the X-Ray spectrum active galactic nucleus of at NGC 4945 (z=0.0019) observed with the XMM-Newton and Swift X-Ray observatory. In X-Ray spectrum is dominated thermal emission associated with the nuclear starburst and X-Ray plume. Neverthess the signature of the AGN is present in the form of a neutral Compton reflection component and a 6.4 keV fluorescent iron Kά line. In this work were received and modeled spectrums with three cameras two independent observations of the satellite XMM-Newton galaxies NGC 4945. Also as a result of modeling were received proper values coefficient reflections, the temperature of the plasma, absorptions along ray of the vision. Processing satellite data Swift not give result, since got photon turned out to be it is not enough.

X-ray and optical emission mechanisms in AGNs and estimations of the masses of black holes.

We present one of the methods for determination of the mass of a central black hole in AGN through the spectral line width. Using this method, the mass of the central black hole in the quasar 1Е 0754 is estimated. The position of 1Е 0754 is in good agreement with the position of other NLS1 galaxies in mass-to-luminosity diagram. We present our results of cross-correlation analysis of the optical and X-ray light curves for eight Seyfert galaxies: NGC 5548, NGC 7469, NGC 3227, NGC 4051, NGC 4151, Mrk 509, Mrk 79, Akn 564. On the base of this observational data we tried to check the theoretical model, have been developed by Sergeev S.G. (Crimean astrophysical observatory, Ukraine) for X-ray activity of AGNs.

Identifications of the point sources from the AKARI Deep Field South

AKARI is a Japanese satellite dedicated to infrared astronomy. It was launched on 2006 February 21, and started observations in May of the same year. A deep survey at 65, 90, 140 and 160 $\mu$m, named AKARI Deep Field South (ADF-S), has been carried out with the FIS instrument onboard the AKARI satellite. In order to minimize the contamination from the Galactic cirrus emission, the region near the South Ecliptic Pole where the cirrus density is the lowest in the whole sky, has been selected for this survey. We have carried out a search for the counterparts of the ADF-S sources in other wavelengths (mainly optical) in the public databases (like NED). I will present the results of analysis of 1000 point sources brighter than 0.0302 Jy in the AKARI Wide-S band: their redshift distribution, the distribution od the angular deviations of counterparts with respect to the ADF-S source, the number counts of sources etc.

In 2005, Gilfanov and Arefiev studied X-ray variability of persistent LMXBs in the 10$^{-8}$ -- 10$^{-1}$ Hz frequency range and found very low frequency break, below which the power density spectra are nearly in white noise structure and at higher frequencies they approximately follow the Pν α ν$^{-1.3}$ law. In order to see whether there is a similar behavior in high mass X-ray binary spectra and if their findings for low mass X-ray binaries are also valid for high mass binaries, we analyzed time series of about 130 high mass X-ray binary sources produced by All Sky Monitor of Rossi X-ray Timing Explorer and identified break frequencies in the same frequency range for only three sources, namely OAO 1657-415, SS 433 and Vela X-1. The objective of Gilfanov & Arefiev for their study was to detect features in the power density spectra associated with the viscous time scale, which is the longest time scale, of the accretion disc, so they compared their results with the standard disc theory prediction for $f_{visc}$/$f_{orb}$. Their findings are compatible with the theory in that the break frequency correlates very well with the binary orbital frequency; however, the value of f$_{break}$/$f_{orb}$ is at least by an order of magnitude larger than the predicted. The ratios we found for OAO 1657-415 and SS 433 are also in accord with that of the low mass X-ray binaries with mass ratios greater than 0.3, q > 0.3: They all imply an aspect ratio of H/R~0.1 rather than a few times of 0.01 which is determined from the standard disc theory. Only Vela X-1 has a much larger $f_{break}$/$f_{orb}$ and that can be attributed to its wind accreting disc nature. Concluding with larger aspect ratios may be interpreted as a two phase accretion flow, i.e. additional mass flow above and below the Shakura - Sunyaev - like disc.

Photometric Study of Three New Open Clusters

We obtained BVRI CCD photometric data for three open clusters recently discovered by analyzing 2MASS catalog. Based on this data, we determined the main physical parameters: ages, distances, and color excesses of the clusters under investigation involving JHK data from the 2MASS point source catalog.

Search for Keplerian periods in light variations of T Tauri stars and Herbig Ae stars

Long-term homogeneous UBVR observations of T Tauri stars and Herbig Ae stars, collected at the Majdanak Observatory over 20 years (project ROTOR), are analysed. We found a linear relationship between the charateristic time of variability and the total bolometric luminosity of the 'star+disk' system: the larger the luminosity is, the slower the variability. The relationship is valid over a wide range of masses and luminosities from T Tauri stars to Herbig Ae stars. It turns out that the characteristric time of variability is, on average, equal to 1/4 of the Keplerian period at the radius of dust sublimation known from interferometric observations. In some of the T Tauri stars, periods of 25 to 120 days were stable during several seasons of observations. The periods correspond to Keplerian orbits with semi-major axes within 1.14 to 0.52 AU. These data are indirect evidence of the protoplanet motions within the dusty circumstellar disks at the pre-main sequence stages of stellar evolution.

Particle module of Piernik-MHD code

We present a new particle module of the Piernik-MHD code. The original multifluid grid code based on the relaxing TVD scheme has been extended by addition of dust described within the particle approximation. The dust is now described as many independent but interacting particles. The particles can interact with gas, which is still described as a fluid. In this poster we introduce the scheme used to solve equations of motion for the particles and present the first results coming from the module. The results of test problems are also compared with the results coming from fluid simulations made with the Piernik-MHD code. The comparison shows the most important differences between fluid and particle approximation used to describe dynamical evolution of dust under astrophysical conditions.

The transit monitoring is one of well-known methods for discovering and observing new extrasolar planets. Among other advantages, this way of looking for other worlds does not require complex and expensive equipment - it can be handled with a relatively small telescope and good-quality CCD camera. At the Center for Astronomy of Nicolaus Copernicus University in Torun, Poland, we collect observational data using the 60-cm Cassegrain telescope hoping that it would be possible to discover new objects in already known planetary systems using the transit timing variation (TTV) method.

Time evolution of collision probabilities for 2009 DD45, 2008 TC3, 2004 AS1

We study the evolution of collision probabilities for near-Earth objects in the case of short observational arcs and/or small numbers of observations. We focus on three objects in particular: 2009 DD45, 2008TC3, and 2004AS1. The Apollo-type asteroid 2009DD45 passed the Earth in a minimal distance of about 0.2 lunar distances on March 2, 2009. The meteoroid 2008TC3 was the first object to be observed and tracked prior to reaching the Earth. It entered the Earth's atmosphere on October 7, 2008 above northern Sudan. Finally, 2004AS1 is an asteroid that, based on single-night data, appeared to be on a collision course with the Earth in January 2004. The impact was predicted on January 15 with a likelihood of about 1:5, assuming 1.0 arcseconds for the observational noise (J. Virtanen and K. Muinonen, Icarus 184, 289-301, 2006). To assess the collision probabilities of the objects listed, we use techniques that rely on the orbital-element probability density function characterized using Markov-Chain Monte-Carlo orbital ranging. We evaluate the orbital uncertainties for the objects from the night of discovery onwards and examine the collapse of the orbital-element distributions in time, in order to confirm or discard the impact risk. In the case of the near-Earth object 2004 AS1, we compare our results to those obtained in previous studies.

Large-Scale Structure in the GOODS-North Field

We have identified a large-scale structure traced by more than 700 objects at different redshifts, within the GOODS-North field, by means of optical observations using the IAC80 telescope and the available data at Nasa Extragalactic Database (NED). All the information has been analyzed using Virtual Observatory (VO) software, and some useful tools we developed specifically for this purpose. We also present a little review of the capabilities of an relatively small telescope like the IAC80 in combination with the using of legacy data and VO tools.

Large-Scale Structure in the GOODS-North Field

We have identified a large-scale structure traced by more than 700 objects at different redshifts, within the GOODS-North field, by means of optical observations using the IAC80 telescope and the available data at Nasa Extragalactic Database (NED). All the information has been analyzed using Virtual Observatory (VO) software, and some useful tools we developed specifically for this purpose. We also present a little review of the capabilities of an relatively small telescope like the IAC80 in combination with the using of legacy data and VO tools.

Estimation of quantified parameters of orbital movements around the central body

The regularity of orbital movement of bodies in the Solar system indicating a discrete character of quantities describing orbital movement of bodies in it as well as in systems planet-satellites is described in the present report. It is found there's a relation between an orbital movement of material objects in the systems planet-satellites and a rotation of planet. It is established, that the radii of structural terrestrial shells and the orbital radii of material objects in the system called the Earth – orbital objects follow the same regular pattern. The dominating concentration of extrasolar planets in the range of orbital periods within 3-4 days is explained on the basis of established regularities. REFERENCES 1. Bolt B. 1984. Inside the Earth. Moscow, “Mir” (translation into Russian). 2. Dziewonski A.M. & Anderson D.L. 1981, Preliminary Reference Earth Model. Physics of the Earth and planetary Interiors, 25, p 297-356. 3. Kuznetsov S. N., Tverskaya L. V. 2006. The radiation belts. http://www.kosmofisika.ru/ 4. Landau L., Lifshits E. 1958. Mechanics. State’s Publishing House of Physical-and Mathematical Literature, Moscow (In Russian). 5. Singer S.F. 1958. Trapped albedo neutron theory of the radiation belt. Phys. Rev. Lett., V.1, p. 181-183. 6. Schneider J. The Extrasolar Planets Encyclopaedia. 2009, http://exoplanet.eu/ 7.Tables of physical data. Reference – book, 1976, Edited by Academician I.I. Kikoin. Atomizdat, Moscow (In Russian). 8. Ural’skaya V.S. 2003. Dynamic of planet’s satellites in the Solar system. Astron. Vestn. v.37, No. 5, p 371-399 (in Russian).

Scalar and fermion radiation from a tensional brane black hole

According to the braneworld models, our Universe is confined on a brane imbedded in a higher-dimensional manifold. It is possible for black holes to exist on a brane. Furthermore, it has been argued that in such scenarios there is a possibility of creating mini black holes in high-energy collider experiments. These objects are expected to evaporate quickly through the Hawking radiation, which can provide an interesting information of the background metric. We study the effect of a brane tension and spacetime dimensionality on massive scalar and Dirac fermion emissions from higher-dimensional tense brane black holes.

Observations of quasars optical variability

In our observatory we have started observations of quasars variability in optical band. We selected the sample of 9 quasars which are radio-loud AGNs - their radio lobes lie on the sky plane and all of them are good visible for our telescope. In connection with specification of quasars sample we expect to observe optical variability originated only from accretion disc around black hole. This kind of observations are the first step to estimation of some important quasars parameters (for example black hole masses) and can give us information about physical properties of this kind of sources.

Photometric Observations and O-C Analysis of High Amplitude Delta Scuti Stars

In my thesis I analyzed six high amplitude delta scuti stars. I searched for variabilities in the O-C diagram of the times of maxima. In the case of BE Lyn I used template curve fitting, but with the redetermined times of maxima I was unable to show the explicit changes of the light curve. The V854 Sco shown some curve shape changes, but the scatter of the measurements was too high to accurately determine the light curve variation. In the case of XX Cyg, DY Her and DY Peg the O-C diagram shown unambiguous changes of the period. The analysis of the O-C diagram in the matter of CY Aqr shown periodic phase jumps.

Photometric telescope of the Olsztyn Astronomical Observatory.

We would like to announce the new observational capabilities of the Olsztyn Observatory. We purchased in 2009 professional CCD camera, B, V and R Bessell filters and new telescope create together fotometric system allowing perform professional observations of the variable stars.

Jet like structures observed in Seccchi Cor1 data

SECCHI-COR1 is an internal occulted coronagraph on the spatial mission STEREO which was launched in october 2006. It observes the solar corona in white-light emission mostly due to Thomson scattering radiation. In 2007 and 2008, jet-like structures were observed almost daily in these images. They are supposed to be signatures of slow solar wind whose source regions are not yet known. Sometimes they can be identified on the disk with bright points observed in ultraviolet images by EIT instrument on SOHO or EUVI instrument on STEREO. We discuss their association with the bright points, statistical distribution and possible mechanisms of emission.

The slow mode oscillations of longitudinally stratified solar coronal loops

There is strong evidence of slow magnetoacoustic modes in the solar corona. This modes and their ratio are useful for extracting information about solar coronal structure. In this paper; we investigated the standing slow modes of solar corona loops with low beta plasma. We studied the influence of different scale heights on periods, their ratio and wave functions. We reduced MHD equations to a Klein-Gordon equation for possible motion of oscillations and in argument with Mc. Ewan et.al (2006). Also we plotted the wave functions for various scale heights. The departure from those of the homogeneous corona loops (when scale height is infinite) can be used as a seismological tool to estimate solar corona parameter.

Infrared Sky Surveys

In 2006 Japanese satellite AKARI (ASTRO-F) was launched. One of its objectives was to make two deep surveys at infrared wavelenghts, both centered on North Ecliptic Pole: NEP Wide Survey and NEP Deep Survey. NEP Wide Survey covers an area of about 5.8 sq. degrees, NEP Deep Survey covers an area of 0.38 sq. degrees. The data were collected by Infrared Camera (IRC) through nine filters: N2, N3, N4, S7, S9, S11, L15, L18, L24 (the numbers represent the effective wavelengths in units of micrometers). We will present first results of our analysis of these point source catalogues: magnitude distribution, colour distribution, number counts etc.

Infrared Sky Surveys

In 2006 Japanese satellite AKARI (ASTRO-F) was launched. One of its objectives was to make two deep surveys at infrared wavelenghts, both centered on North Ecliptic Pole: NEP Wide Survey and NEP Deep Survey. NEP Wide Survey covers an area of about 5.8 sq. degrees, NEP Deep Survey covers an area of 0.38 sq. degrees. The data were collected by Infrared Camera (IRC) through nine filters: N2, N3, N4, S7, S9, S11, L15, L18, L24 (the numbers represent the effective wavelengths in units of micrometers). We will present first results of our analysis of these point source catalogues: magnitude distribution, colour distribution, number counts etc.

KU Cyg - the Algol-type binary with an eccentric accretion disk

In this work we present and discuss the results from analysis of the Ha emission line observed at the primary minimum, at phases in the 0.0058 - 0.0209 range. The profile of this line, originating in the accretion disk, observed when the approaching part of the disk was partly eclipsed by the secondary, the mass losing star, was modelled. The results indicate that the double peaked emission profile can be explained as being emitted in a large, eccentric disk around the primary component. This confirms the previous suggestions, based on photometric and spectroscopic data, that the disk in KU Cyg occasionally becomes very large, eccentric, and possibly precessing.