Author name code: kostogryz ADS astronomy entries on 2022-09-14 author:Kostogryz, Nadiia M. ------------------------------------------------------------------------ Title: Stellar limb darkening. A new MPS-ATLAS library for Kepler, TESS, CHEOPS, and PLATO passbands Authors: Kostogryz, N. M.; Witzke, V.; Shapiro, A. I.; Solanki, S. K.; Maxted, P. F. L.; Kurucz, R. L.; Gizon, L. Bibcode: 2022arXiv220606641K Altcode: The detection of the first exoplanet paved the way into the era of transit photometry space missions with a revolutionary photometric precision that aim at discovering new exoplanetary systems around different types of stars. With this high precision, it is possible to derive very accurately the radii of exoplanets which is crucial for constraining their type and composition. However, it requires an accurate description of host stars, especially their center-to-limb variation of intensities (so called limb darkening) as it affects the planet-to-star radius ratio determination. We aim at improving the accuracy of limb darkening calculations for stars with a wide range of fundamental parameters. We used the recently developed 1D MPS-ATLAS code to compute model atmosphere structures and to synthesize stellar limb darkening on a very fine grid of stellar parameters. For the computations we utilized the most accurate information on chemical element abundances and mixing length parameters including convective overshoot. The stellar limb darkening was fitted using the two most accurate limb darkening laws: the power-2 and 4-parameters non-linear laws. We present a new extensive library of stellar model atmospheric structures, the synthesized stellar limb darkening curves, and the coefficients of parameterized limb-darkening laws on a very fine grid of stellar parameters in the Kepler, TESS, CHEOPS, and PLATO passbands. The fine grid allows overcoming the sizable errors introduced by the need to interpolate. Our computations of solar limb darkening are in a good agreement with available solar measurements at different view angles and wavelengths. Our computations of stellar limb darkening agree well with available measurements of Kepler stars. A new grid of stellar model structures, limb darkening and their fitted coefficients in different broad filters is provided in CDS. Title: Final Report for SAG 21: The Effect of Stellar Contamination on Space-based Transmission Spectroscopy Authors: Rackham, Benjamin V.; Espinoza, Néstor; Berdyugina, Svetlana V.; Korhonen, Heidi; MacDonald, Ryan J.; Montet, Benjamin T.; Morris, Brett M.; Oshagh, Mahmoudreza; Shapiro, Alexander I.; Unruh, Yvonne C.; Quintana, Elisa V.; Zellem, Robert T.; Apai, Dániel; Barclay, Thomas; Barstow, Joanna K.; Bruno, Giovanni; Carone, Ludmila; Casewell, Sarah L.; Cegla, Heather M.; Criscuoli, Serena; Fischer, Catherine; Fournier, Damien; Giampapa, Mark S.; Giles, Helen; Iyer, Aishwarya; Kopp, Greg; Kostogryz, Nadiia M.; Krivova, Natalie; Mallonn, Matthias; McGruder, Chima; Molaverdikhani, Karan; Newton, Elisabeth R.; Panja, Mayukh; Peacock, Sarah; Reardon, Kevin; Roettenbacher, Rachael M.; Scandariato, Gaetano; Solanki, Sami; Stassun, Keivan G.; Steiner, Oskar; Stevenson, Kevin B.; Tregloan-Reed, Jeremy; Valio, Adriana; Wedemeyer, Sven; Welbanks, Luis; Yu, Jie; Alam, Munazza K.; Davenport, James R. A.; Deming, Drake; Dong, Chuanfei; Ducrot, Elsa; Fisher, Chloe; Gilbert, Emily; Kostov, Veselin; López-Morales, Mercedes; Line, Mike; Močnik, Teo; Mullally, Susan; Paudel, Rishi R.; Ribas, Ignasi; Valenti, Jeff A. Bibcode: 2022arXiv220109905R Altcode: Study Analysis Group 21 (SAG21) of the Exoplanet Exploration Program Analysis Group (ExoPAG) was organized to study the effect of stellar contamination on space-based transmission spectroscopy, a method for studying exoplanetary atmospheres by measuring the wavelength-dependent radius of a planet as it transits its star. Transmission spectroscopy relies on a precise understanding of the spectrum of the star being occulted. However, stars are not homogeneous, constant light sources but have temporally evolving photospheres and chromospheres with inhomogeneities like spots, faculae, and plages. This SAG has brought together an interdisciplinary team of more than 100 scientists, with observers and theorists from the heliophysics, stellar astrophysics, planetary science, and exoplanetary atmosphere research communities, to study the current needs that can be addressed in this context to make the most of transit studies from current NASA facilities like HST and JWST. The analysis produced 14 findings, which fall into three Science Themes encompassing (1) how the Sun is used as our best laboratory to calibrate our understanding of stellar heterogeneities ("The Sun as the Stellar Benchmark"), (2) how stars other than the Sun extend our knowledge of heterogeneities ("Surface Heterogeneities of Other Stars") and (3) how to incorporate information gathered for the Sun and other stars into transit studies ("Mapping Stellar Knowledge to Transit Studies"). Title: Modelling continuum intensity perturbations caused by solar acoustic oscillations Authors: Kostogryz, N. M.; Fournier, D.; Gizon, L. Bibcode: 2021A&A...654A...1K Altcode: 2021arXiv210707220K Context. Helioseismology is the study of the Sun's interior using observations of oscillations at the surface. It suffers from systematic errors, for instance a center-to-limb error in travel-time measurements. Understanding these errors requires an adequate understanding of the nontrivial relationship between wave displacement and helioseismic observables (intensity or velocity).
Aims: The wave displacement causes perturbations in the atmospheric thermodynamical quantities which, in turn, perturb the opacity, the optical depth, the source function, and the local ray geometry, thus affecting the emergent intensity. We aim to establish the most complete relationship achieved to date between the wave displacement and the emergent intensity perturbation by solving the radiative transfer problem in the perturbed atmosphere.
Methods: We derived an expression for the emergent intensity perturbation caused by acoustic oscillations at any point on the solar disk by applying a first-order perturbation theory. As input perturbations, we considerd adiabatic modes of oscillation of different degrees in a spherically-symmetric solar model. The background and the perturbed intensities are computed by solving the radiative transfer equation considering the main sources of opacity in the continuum (absorption and scattering).
Results: We find that for all modes, the perturbations to the thermodynamical quantities are not sufficient to model the intensity perturbations: the geometrical effects due to the wave displacement must always be taken into account as they lead to a difference in amplitude and a phase shift between temperature perturbations at the surface and emergent intensity perturbations. The closer to the limb, the greater the differences. For modes with eigenfrequencies around 3 mHz, we found that the radial and horizontal components of the wave displacement are important, in particular, for high-degree modes.
Conclusions: This work presents improvements for the computation of the intensity perturbations, in particular, for high-degree modes. Here, we explain the differences in intensity computations seen in earlier works. The phase shifts and amplitude differences between the temperature and intensity perturbations increase toward the limb. This should prove helpful when interpreting some of the systematic centre-to-limb effects observed in local helioseismology. The computations are fast (3 s for 2000 positions and one frequency for one core) and can be parallelised. This work can be extended to models of the line-of-sight velocity observable. Title: MPS-ATLAS: A fast all-in-one code for synthesising stellar spectra Authors: Witzke, V.; Shapiro, A. I.; Cernetic, M.; Tagirov, R. V.; Kostogryz, N. M.; Anusha, L. S.; Unruh, Y. C.; Solanki, S. K.; Kurucz, R. L. Bibcode: 2021A&A...653A..65W Altcode: 2021arXiv210513611W Context. Stellar spectral synthesis is essential for various applications, ranging from determining stellar parameters to comprehensive stellar variability calculations. New observational resources as well as advanced stellar atmosphere modelling, taking three dimensional effects from radiative magnetohydrodynamics calculations into account, require a more efficient radiative transfer.
Aims: For accurate, fast and flexible calculations of opacity distribution functions (ODFs), stellar atmospheres, and stellar spectra, we developed an efficient code building on the well-established ATLAS9 code. The new code also paves the way for easy and fast access to different elemental compositions in stellar calculations.
Methods: For the generation of ODF tables, we further developed the well-established DFSYNTHE code by implementing additional functionality and a speed-up by employing a parallel computation scheme. In addition, the line lists used can be changed from Kurucz's recent lists. In particular, we implemented the VALD3 line list.
Results: A new code, the Merged Parallelised Simplified ATLAS, is presented. It combines the efficient generation of ODF, atmosphere modelling, and spectral synthesis in local thermodynamic equilibrium, therefore being an all-in-one code. This all-in-one code provides more numerical functionality and is substantially faster compared to other available codes. The fully portable MPS-ATLAS code is validated against previous ATLAS9 calculations, the PHOENIX code calculations, and high-quality observations. Title: Accurate Short-Characteristics Radiative Transfer in A Numerical Tool for Astrophysical RESearch (ANTARES) Authors: Kostogryz, Nadiia M.; Kupka, Friedrich; Piskunov, Nikolai; Fabbian, Damian; Krüger, Daniel; Gizon, Laurent Bibcode: 2021SoPh..296...46K Altcode: We aim to improve the accuracy of radiative energy transport in three-dimensional radiation hydrodynamical simulations in ANTARES (A Numerical Tool for Astrophysical RESearch). We implement in the ANTARES short-characteristics numerical schemes a modification of the Bézier interpolant solver. This method yields a smoother surface structure in simulations of solar convection and reduces the artifacts appearing due to the limited number of rays along which the integration is done. Reducing such artifacts leads to increased stability of the code. We show that our new implementation achieves a better agreement of the temperature structure and its gradient with a semi-empirical model derived from observations, as well as of synthetic spectral-line profiles with the observed solar spectrum. Title: On long-duration 3D simulations of stellar convection using ANTARES Authors: Kupka, F.; Fabbian, D.; Krüger, D.; Kostogryz, N.; Gizon, L. Bibcode: 2020IAUGA..30..373K Altcode: We present initial results from three-dimensional (3-D) radiation hydrodynamical simulations for the Sun and targeted Sun-like stars. We plan to extend these simulations up to several stellar days to study p-mode excitation and damping processes. The level of variation of irradiance on the time scales spanned by our 3-D simulations will be studied too. Here we show results from a first analysis of the computational data we produced so far. Title: Shine BRITE: shedding light on stellar variability through advanced models Authors: Fabbian, D.; Kupka, F.; Krüger, D.; Kostogryz, N. M.; Piskunov, N. Bibcode: 2020svos.conf..155F Altcode: 2020arXiv200201560F The correct interpretation of the large amount of complex data from next-generation (in particular, space-based) observational facilities requires a very strong theoretical underpinning. One can predict that, in the near future, the use of atmospheric models obtained with three-dimensional (3-D) radiation magneto-hydrodynamics (RMHD) codes, coupled with advanced radiative transfer treatment including non-local thermodynamic equilibrium (non-LTE) effects and polarisation, will become the norm. In particular, stellar brightness variability in cool stars (i.e., spectral types F-- M) can be caused by several different effects besides pulsation. In this review we have briefly discussed some published results, and mentioned aspects of recent progress. It then attempted to peek into what the future may hold for understanding this important aspect of the lives of stars. Title: The inner dust shell of Betelgeuse detected by polarimetric aperture-masking interferometry Authors: Haubois, X.; Norris, B.; Tuthill, P. G.; Pinte, C.; Kervella, P.; Girard, J. H.; Kostogryz, N. M.; Berdyugina, S. V.; Perrin, G.; Lacour, S.; Chiavassa, A.; Ridgway, S. T. Bibcode: 2019A&A...628A.101H Altcode: 2019arXiv190708594H Context. Theory surrounding the origin of the dust-laden winds from evolved stars remains mired in controversy. Characterizing the formation loci and the dust distribution within approximately the first stellar radius above the surface is crucial for understanding the physics that underlie the mass-loss phenomenon.
Aims: By exploiting interferometric polarimetry, we derive the fundamental parameters that govern the dust structure at the wind base of a red supergiant.
Methods: We present near-infrared aperture-masking observations of Betelgeuse in polarimetric mode obtained with the NACO/SAMPol instrument. We used both parametric models and radiative transfer simulations to predict polarimetric differential visibility data and compared them to SPHERE/ZIMPOL measurements.
Results: Using a thin dust shell model, we report the discovery of a dust halo that is located at only 0.5 R⋆ above the photosphere (i.e. an inner radius of the dust halo of 1.5 R⋆). By fitting the data under the assumption of Mie scattering, we estimate the grain size and density for various dust species. By extrapolating to the visible wavelengths using radiative transfer simulations, we compare our model with SPHERE/ZIMPOL data and find that models based on dust mixtures that are dominated by forsterite are most favored. Such a close dusty atmosphere has profound implications for the dust formation mechanisms around red supergiants.

Based on SAMPol data obtained at the ESO VLT Yepun telescope (090.D-0898(A)). Title: Modeling observables for local helioseismology. Authors: Kostogryz, Nadiia; Fournier, Damien; Gizon, Laurent Bibcode: 2019AAS...23430705K Altcode: Local helioseismology provides different techniques to study flows in the solar interior. However, all of them suffer from systematic errors, which occur because of the nontrivial relationship between wave displacement and helioseismic observables, such as intensity and Doppler velocity. In this study, we solve the radiative transfer equation in a perturbed solar atmosphere including flows caused by acoustic oscillations. The adiabatic oscillations for normal modes of low and high degree are computed using the ADIPLS code that solves an eigenvalue problem in a standard solar model assuming spherically symmetric background quantities. The wave displacement causes perturbations in atmospheric thermodynamical quantities that, in turn, perturb opacity and emergent intensity. These perturbations depend on the center to the limb distance. In addition, the oscillations modify the shape of the solar surface and thus the direction of the normal to the surface. For low-degree modes this geometrical effect is negligible, however, this effect matters for high-degree modes with a large horizontal component of wave displacement. We investigate the contribution of such perturbations on emergent intensity and velocity and estimate their impact on helioseismic observables. Title: Center-to-Limb Continuum Polarization in Solar and Stellar Atmospheres Authors: Kostogryz, N. M.; Berdyugina, S. V.; Yakobchuk, T. M.; Milić, I. Bibcode: 2019ASPC..526..139K Altcode: The center-to-limb variation of the intensity (CLVI) and of the linear polarization (CLVP) of stellar radiation arise when the scattering and absorption processes are important in the stellar atmosphere. We model the CLVI and CLVP of continuum radiation, taking into account different contributions of scattering and absorption opacity for a variety of spectral type stars with plane-parallel and spherical PHOENIX atmosphere models. We show how the polarization depends on the effective temperature and surface gravity of a star and how the considered geometry of the stellar atmosphere affects the polarization signal. For the Sun, we compare existing measurements with our theoretical predictions for different solar models (FALA, FALC, FALP, HSRA, and Phoenix). The CLVI and CLVP of stellar atmospheres are also needed to interpret the light curves of transiting exoplanets. Here we present the variation of the polarization in exoplanetary systems caused by transits and grazing transits and discuss how the considered geometry of stellar atmosphere models affect the transit curves of exoplanets. Title: Polarimetry of transiting planets: Differences between plane-parallel and spherical host star atmosphere models Authors: Kostogryz, N. M.; Yakobchuk, T. M.; Berdyugina, S. V.; Milic, I. Bibcode: 2017A&A...601A...6K Altcode: Context. To properly interpret photometric and polarimetric observations of exoplanetary transits, accurate calculations of center-to-limb variations of intensity and linear polarization of the host star are needed. These variations, in turn, depend on the choice of geometry of stellar atmosphere.
Aims: We want to understand the dependence of the flux and the polarization curves during a transit on the choice of the applied approximation for the stellar atmosphere: spherical and plane-parallel. We examine whether simpler plane-parallel models of stellar atmospheres are good enough to interpret the flux and the polarization light curves during planetary transits, or whether more complicated spherical models should be used.
Methods: Linear polarization during a transit appears because a planet eclipses a stellar disk and thus breaks left-right symmetry. We calculate the flux and the polarization variations during a transit with given center-to-limb variations of intensity and polarization.
Results: We calculate the flux and the polarization variations during transit for a sample of 405 extrasolar systems. Most of them show higher transit polarization for the spherical stellar atmosphere. Our calculations reveal a group of exoplanetary systems that demonstrates lower maximum polarization during the transits with spherical model atmospheres of host stars with effective temperatures of Teff = 4400-5400 K and surface gravity of log g = 4.45-4.65 than that obtained with plane-parallel atmospheres. Moreover, we have found two trends of the transit polarization. The first trend is a decrease in the polarization calculated with spherical model atmosphere of host stars with effective temperatures Teff = 3500-5100 K, and the second shows an increase in the polarization for host stars with Teff = 5100-7000 K. These trends can be explained by the relative variation of temperature and pressure dependences in the plane-parallel and spherical model atmospheres.
Conclusions: For most cases of known transiting systems the plane-parallel approximation of stellar model atmospheres may be safely used for calculation of the flux and the polarization curves because the difference between two models is tiny. However, there are some examples where the spherical model atmospheres are necessary to get proper results, such as the systems with grazing transits, with Earth-size planets, or for the hot host stars with effective temperatures higher than 6000 K. Title: Haze and cloud distribution in Uranus' atmosphere based on high-contrast spatially resolved polarization measurements Authors: Kostogryz, Nadiia; Berdyugina, Svetlana; Gisler, Daniel; Berkefeld, Thomas Bibcode: 2017EGUGA..1918092K Altcode: In planetary atmospheres, main sources of opacity are molecular absorption and scattering on molecules, hazes and aerosols. Hence, light reflected from a planetary atmosphere can be linearly polarized. Polarization study of inner solar system planets and exoplanets is a powerful method to characterize their atmospheres, because of a wide range of observable phase angles. For outer solar system planets, observable phase angles are very limited. For instance, Uranus can only be observed up to 3.2 degrees away from conjunctions, and its disk-integrated polarization is close to zero due to the back-scattering geometry. However, resolving the disk of Uranus and measuring the center-to-limb polarization can help constraining the vertical atmospheric structure and the nature of scattering aerosols and particles. In October 2016, we carried out polarization measurements of Uranus in narrow-band filters centered at methane bands and the adjacent continuum using the GREGOR Planet Polarimeter (GPP). The GPP is a high-precision polarimeter and is mounted at the 1.5-m GREGOR solar telescope, which is suitable for observing at night. In order to reach a high spatial resolution, the instrument uses an adaptive-optics system of the telescope. To interpret our measurements, we solve the polarized radiative transfer problem taking into account different scattering and absorption opacities. We calculate the center-to-limb variation of polarization of Uranus' disk in the continuum spectrum and in methane bands. By varying the vertical distribution of haze and cloud layers, we derive the vertical structure of the best-fit Uranus atmosphere. Title: Center-to-limb variation of intensity and polarization in continuum spectra of FGK stars for spherical atmospheres Authors: Kostogryz, N. M.; Milic, I.; Berdyugina, S. V.; Hauschildt, P. H. Bibcode: 2016A&A...586A..87K Altcode: 2015arXiv151107213K
Aims: One of the necessary parameters needed for the interpretation of the light curves of transiting exoplanets or eclipsing binary stars (as well as interferometric measurements of a star or microlensing events) is how the intensity and polarization of light changes from the center to the limb of a star. Scattering and absorption processes in the stellar atmosphere affect both the center-to-limb variation of intensity (CLVI) and polarization (CLVP). In this paper, we present a study of the CLVI and CLVP in continuum spectra, taking into consideration the different contributions of scattering and absorption opacity for a variety of spectral type stars with spherical atmospheres.
Methods: We solve the radiative transfer equation for polarized light in the presence of a continuum scattering, taking into consideration the spherical model of a stellar atmosphere. To cross-check our results, we developed two independent codes that are based on Feautrier and short characteristics methods, respectively,
Results: We calculate the center-to-limb variation of intensity (CLVI) and polarization (CLVP) in continuum for the Phoenix grid of spherical stellar model atmospheres for a range of effective temperatures (4000-7000 K), gravities (log g = 1.0-5.5), and wavelengths (4000-7000 Å), which are tabulated and available at the CDS. In addition, we present several tests of our codes and compare our calculations for the solar atmosphere with published photometric and polarimetric measurements. We also show that our two codes provide similar results in all considered cases.
Conclusions: For sub-giant and dwarf stars (log g = 3.0-4.5), the lower gravity and lower effective temperature of a star lead to higher limb polarization of the star. For giant and supergiant stars (log g = 1.0-2.5), the highest effective temperature yields the largest polarization. By decreasing the effective temperature of a star down to 4500-5500 K (depending on log g), the limb polarization decreases and reaches a local minimum. It increases again with a corresponding decrease in temperature down to 4000 K. For the most compact dwarf stars (log g = 5.0-5.5), the limb polarization degree shows a maximum for models with effective temperatures in the range 4200-4600 K (depending on log g) and decreases toward higher and lower temperatures.

The intensity and polarization profiles are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/586/A87 Title: VizieR Online Data Catalog: Center-to-limb polarization of FGK stars (Kostogryz+, 2016) Authors: Kostogryz, N. M.; Milic, I.; Berdyugina, S. V.; Hauschildt, P. H. Bibcode: 2016yCat..35860087K Altcode: Calculated center-to-limb variations of intensity (limb darkening) for different stellar parameters with spherical atmosphere model approximation. All intensities are normalized to the intensity in the center of stellar disks, therefore, in the centre of the disks (mu=1.0), I(mu)/I(1.0)=1.0. The parameters of spherical Phoenix stellar model atmospheres we considered here are the following: effective temperature is in the range of 4000K-7000K with the step of 100K and for logg=1.0-5.5 with the step of 0.5. All calculations are made for such wavelengths: 4000Å, 4500Å, 5000Å, 6000Å, 7000Å. We also present the position of the stellar limb and calculated stellar radius.

Calculated center-to-limb variations of polarization (CLVP) for different stellar parameters with spherical atmosphere model approximation. All intensities are normalized to the intensity in the center of stellar disks, therefore, in the centre of the disks (mu=1.0), I(mu)/I(1.0)=1.0. The parameters of spherical Phoenix model atmosphere we considered here are the following: effective temperature is in the range of 4000K-7000 K with the step of 100K and for logg=1.0-5.5 with the step of 0.5. All calculations are made for such wavelengths: 4000Å, 4500Å, 5000Å, 6000Å, 7000Å. We also present the position of the stellar limb.

(2 data files). Title: Investigations on physics of planetary atmospheres and small bodies of the Solar system, extrasolar planets and disk structures around the stars Authors: Vidmachenko, A. P.; Delets, O. S.; Dlugach, J. M.; Zakhozhay, O. V.; Kostogryz, N. M.; Krushevska, V. M.; Kuznyetsova, Y. G.; Morozhenko, O. V.; Nevodovskyi, P. V.; Ovsak, O. S.; Rozenbush, O. E.; Romanyuk, Ya. O.; Shavlovskiy, V. I.; Yanovitskij, E. G. Bibcode: 2015ippa.book.....V Altcode: The history and main becoming stages of Planetary system physics Department of the Main astronomical observatory of National academy of Sciences of Ukraine are considered. Fundamental subjects of department researches and science achievements of employees are presented. Fields of theoretical and experimental researches are Solar system planets and their satellites; vertical structures of planet atmospheres; radiative transfer in planet atmospheres; exoplanet systems of Milky Way; stars having disc structures; astronomical engineering. Employees of the department carry out spectral, photometrical and polarimetrical observations of Solar system planets, exoplanet systems and stars with disc structures. 1. From the history of department 2. The main directions of department research 3. Scientific instrumentation 4. Telescopes and observation stations 5. Theoretical studies 6. The results of observations of planets and small Solar system bodies and their interpretation 7. The study of exoplanets around the stars of our galaxy 8. Spectral energy distribution of fragmenting protostellar disks 9. Cooperation with the National Technical University of Ukraine (KPI) and National University of Ukraine "Lviv Polytechnic" to study the impact of stratospheric aerosol changes on weather and climate of the Earth 10. International relations. Scientific and organizational work. Scientific conferences, congresses, symposia 11. The main achievements of the department 12. Current researches 13. Anniversaries and awards Title: Polarization in Exoplanetary Systems Caused by Transits, Grazing Transits, and Starspots Authors: Kostogryz, N. M.; Yakobchuk, T. M.; Berdyugina, S. V. Bibcode: 2015ApJ...806...97K Altcode: 2015arXiv150402943K We present results of numerical simulations of flux and linear polarization variations in transiting exoplanetary systems, caused by host star disk symmetry breaking. We consider different configurations of planetary transits depending on orbital parameters. The starspot contribution to the polarized signal is also estimated. Applying the method to known systems and simulating observational conditions, a number of targets is selected where transit polarization effects could be detected. We investigate several principal benefits of the transit polarimetry, particularly for determining orbital spatial orientation and distinguishing between grazing and near-grazing planets. Simulations show that polarization parameters are also sensitive to starspots, and they can be used to determine spot positions and sizes. Title: Disentangling 2:1 resonant radial velocity orbits from eccentric ones and a case study for HD 27894 Authors: Kürster, Martin; Trifonov, Trifon; Reffert, Sabine; Kostogryz, Nadiia M.; Rodler, Florian Bibcode: 2015A&A...577A.103K Altcode: 2015arXiv150307769K Context. In radial velocity (RV) observations, a pair of extrasolar planets near a 2:1 orbital resonance can be misinterpreted as a single eccentric planet, if data are sparse and measurement precision insufficient to distinguish between these models.
Aims: Using the Exoplanet Orbit Database (EOD), we determine the fraction of alleged single-planet RV detected systems for which a 2:1 resonant pair of planets is also a viable model and address the question of how the models can be disentangled.
Methods: By simulation we quantified the mismatch arising from applying the wrong model. Model alternatives are illustrated using the supposed single-planet system HD 27894 for which we also study the dynamical stability of near-2:1 resonant solutions.
Results: Using EOD values of the data scatter around the fitted single-planet Keplerians, we find that for 74% of the 254 putative single-planet systems, a 2:1 resonant pair cannot be excluded as a viable model, since the error due to the wrong model is smaller than the scatter. For 187 EOD stars χ2-probabilities can be used to reject the Keplerian models with a confidence of 95% for 54% of the stars and with 99.9% for 39% of the stars. For HD 27894 a considerable fit improvement is obtained when adding a low-mass planet near half the orbital period of the known Jovian planet. Dynamical analysis demonstrates that this system is stable when both planets are initially placed on circular orbits. For fully Keplerian orbits a stable system is only obtained if the eccentricity of the inner planet is constrained to < 0.3.
Conclusions: A large part of the allegedly RV detected single-planet systems should be scrutinized in order to determine the fraction of systems containing near-2:1 resonant pairs of planets. Knowing the abundance of such systems will allow us to revise the eccentricity distribution for extrasolar planets and provide direct constraints for planetary system formation.

This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at http://www.exoplanets.org Title: Spectrophotometric properties of Moon's and Mars's surfaces exploration by shadow mechanism Authors: Morozhenko, Alexandr; Vidmachenko, Anatolij; Kostogryz, Nadiia Bibcode: 2015HiA....16..182M Altcode: Typically, to analyze the data of the phase dependence of brightness atmosphereless celestial bodies one use some modification of the shadow mechanism involving the coherent mechanism. There are several modification of B.Hapke [2] model divided into two groups by the number of unknown parameters: the first one with 4 parameters [3,4] and the second one with up to 10 unknown parameters [1] providing a good agreement of observations and calculations in several wavelengths. However, they are complicated by analysing of the colorindex C(α) dependence and photometric contrast of details with phase K(α) and on the disk (μ o = cos i). We have got good agreement between observed and calculated values of C(α) = U(α)-I(α), K(α), K(muo) for Moon and Mars with a minimum number of unknown parameters [4]. We used an empirical dependence of single scattering albedo (ω) and particle semi-transparency(æ): æ = (1-ω)n. Assuming that [χ (0°)/χ(5°)] = χ (5°)/χ (0°)], where χ(α) is scattering function, using the phase dependence of brightness and opposition effect in a single wavelength, we have defined ω,χ(α),g (particle packing factor), and the first term expansion of χ(α) in a series of Legendre polynomials x1. Good agreement between calculated and observed data of C(α) = U(α)-I(α) for the light and dark parts of the lunar surface and the integral disk reached at n ~ 0,25, g = 0,4 (porosity 0,91), x1 = -0,93, ω = 0,137 at λ = 359nm and 0,394 at λ = 1064nm;, for Mars with n ~ 0,25,g = 0,6 (porosity 0,84), x1 ~ 0, ω = 0,210 at λ = 359nm and ω = 0,784 at λ = 730nm.

1. Bowell E., Hapke B., Domingue D., Lumme K., et al. Applications of photometric models to asteroids, in Asteroids II. Tucson: Univ. Arizona Press. p.524-556. (1989)

2. Hapke B. A theoretical function for the lunar surface, J.Geophys.Res. 68, No.15., 4571-4586(1963).

3. Irwine W. M., The shadowing effect in diffuse reflection, J.Geophys.Res. 71,No.12, 2931-2937(1966).

4. Morozhenko A. V., Yanovitskij E.G., An optical model of the Martian surface in the visible region of spectrum, Astronomy Reports 48, No.4, 795-809(1971). Title: Center-to-limb polarization in continuum spectra of F, G, K stars Authors: Kostogryz, N. M.; Berdyugina, S. V. Bibcode: 2015A&A...575A..89K Altcode: 2014arXiv1408.5019K Context. Scattering and absorption processes in stellar atmosphere affect the center-to-limb variations of the intensity (CLVI) and the linear polarization (CLVP) of stellar radiation.
Aims: There are several theoretical and observational studies of CLVI using different stellar models, however, most studies of CLVP have concentrated on the solar atmosphere and have not considered the CLVP in cooler non-gray stellar atmospheres at all. In this paper, we present a theoretical study of the CLV of the intensity and the linear polarization in continuum spectra of different spectral type stars.
Methods: We solve the radiative transfer equations for polarized light iteratively assuming no magnetic field and considering a plane-parallel model atmospheres and various opacities.
Results: We calculate the CLVI and the CLVP for Phoenix stellar model atmospheres for the range of effective temperatures (4500 K-6900 K), gravities (log g = 3.0-5.0), and wavelengths (4000-7000 Å), which are tabulated and available at the CDS. In addition, we present several tests of our code and compare our results with measurements and calculations of CLVI and the CLVP for the Sun. The resulting CLVI are fitted with polynomials and their coefficients are presented in this paper.
Conclusions: For the stellar model atmospheres with lower gravity and effective temperature the CLVP is larger.

Full Tables 1 and 2, and coefficients of polynomials are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/575/A89 Title: VizieR Online Data Catalog: Center-to-limb polarization of FGK stars (Kostogryz+, 2015) Authors: Kostogryz, N. M.; Berdyugina, S. V. Bibcode: 2015yCat..35750089K Altcode: 2015yCat..35759089K The stellar parameters we considered here are the following: effective temperature is in the range of 4500K-6900K with the step of 100K and for logg=3.0, 3.5, 4.0, 4.5, 5.0. All calculations are made for such wavelengths: 4000Å, 4500Å, 5000Å, 6000Å, 7000Å.

table1.dat: Calculated center-to-limb variations of intensity (limb darkening) for different stellar parameters with plane-parallel atmosphere model approximation. All intensities are normalized to the intensity in the center of stellar disks, therefore, in the centre of the disks (mu=1.0), I(mu)/I(1.0)=1.0.

table2.dat: Calculated center-to-limb variations of linear polarization (Stokes parameter Q/I) for different stellar parameters with plane-parallel atmosphere model approximation. The radiation coming from the centre of the stellar disk is nonpolarized, so all values of Q/I(1.0)=0.0.

table3.dat: Calculated polynomial coefficients of center-to-limb variations of intensity (limb darkening) fits for different stellar parameters with plane-parallel atmosphere model approximation.

(3 data files). Title: Transit Polarimetry of Exoplanetary System HD 189733 Authors: Kostogryz, N. M.; Berdyugina, S. V.; Yakobchuk, T. M. Bibcode: 2015csss...18..773K Altcode: 2014arXiv1408.5023K We present and discuss a polarimetric effect caused by a planet transiting the stellar disk thus breaking the symmetry of the light distribution and resulting in linear polarization of the partially eclipsed star. Estimates of this effect for transiting planets have been made only recently. In particular, we demonstrate that the maximum polarization during transits depends strongly on the centre-to-limb variation of the linear polarization of the host star. However, observational and theoretical studies of the limb polarization have largely concentrated on the Sun. Here we solve the radiative transfer problem for polarized light and calculate the centre-to-limb polarization for one of the brightest transiting planet host HD 189733 taking into account various opacities. Using that we simulate the transit effect and estimate the variations of the flux and the linear polarization for HD 189733 during the event. As the spots on the stellar disk also break the limb polarization symmetry we simulate the flux and polarization variation due to the spots on the stellar disk. Title: On the efficiency of polarization measurements while studying aerosols in the terrestrial atmosphere Authors: Morozhenko, A. V.; Vidmachenko, A. P.; Nevodovskiy, P. V.; Kostogryz, N. M. Bibcode: 2014KPCB...30...11M Altcode: It has been shown that the orbital polarization measurements of the Earth in the spectral range λ > 300 nm do not allow the sets of the Stokes parameters satisfying the homogeneity requirement for the optical properties of the "atmosphere + surface" system to be retrieved. Due to this, the atmospheric and surface contributions cannot be correctly separated and the physical properties of the atmospheric aerosol cannot be determined. This is caused by the optical heterogeneity of the system, the different nature of aerosol above different relief features, and the poorly predictable temporal changes of the optical properties of the "atmosphere + surface" system. Observations at λ < 300 nm are more acceptable, since not only the surface but also the tropospheric layer of the atmosphere, which are both mostly subjected to the effects of horizontal inhomogeneity and temporal variations, become practically invisible due to a high absorption by the ozone layer. Because of this, from the scans along specified latitude zones, one may obtain the quasi-homogeneous dependences of the second Stokes parameter Q(α) (U(α) = 0) suitable for estimating the physical characteristics of the stratospheric aerosol and revealing their horizontal and temporal variations. Title: A spectral differential approach to characterizing low-mass companions to late-type stars Authors: Kostogryz, N. M.; Kürster, M.; Yakobchuk, T. M.; Lyubchik, Y.; Kuznetsov, M. K. Bibcode: 2013AN....334..648K Altcode: 2013arXiv1303.5254K In this paper, we develop a spectral differential technique with which the dynamical mass of low-mass companions can be found. This method aims at discovering close companions to late-type stars by removing the stellar spectrum through a subtraction of spectra obtained at different orbital phases and discovering the companion spectrum in the difference spectrum in which the companion lines appear twice (positive and negative signal). The resulting radial velocity difference of these two signals provides the true mass of the companion, if the orbital solution for the radial velocities of the primary is known. We select the CO line region in the K band for our study, because it provides a favourable star-to-companion brightness ratio for our test case GJ 1046, an M2V dwarf with a low-mass companion that most likely is a brown dwarf. Furthermore, these lines remain largely unblended in the difference spectrum so that the radial velocity amplitude of the companion can be measured directly. Only if the companion rotates rapidly and has a small radial velocity due to a high mass, does blending occur for all lines so that our approach fails. We also consider activity of the host star, and show that the companion difference flux can be expected to have larger amplitude than the residual signal from the active star so that stellar activity does not inhibit the determination of the companion mass. In addition to determining the companion mass, we restore the single companion spectrum from the difference spectrum using singular value decomposition. Title: A spectral differential characterization of low-mass companions Authors: Kostogryz, N.; Kürster, M.; Yakobchuk, T.; Lyubchik, Y.; Kuznetsov, M. Bibcode: 2013EPJWC..4713003K Altcode: We present a new approach with which the dynamical mass of low-mass companions around cool stars can be found. In order to discover companions to late-type stars the stellar spectrum is removed. For this we substract two spectra obtained at different orbital phases from each other in order to discover the companion spectrum in the difference spectrum in which the companion lines appear twice (positive and negative signal). The resulting radial velocity difference of these two signals provides the true mass of the companion. For our test case GJ1046, an M2V dwarf with a low-mass companion that most likely is a brown dwarf we select the CO line region in the K-band. We show that the dynamical mass of a faint companion to an M dwarf can be determined using our spectral differential technique. Only if the companion rotates rapidly and has a small radial velocity amplitude due to a high mass, does blending occur for all lines so that our approach fails. In addition to determining the companion mass, we restore the single companion spectrum from the difference spectrum using singular value decomposition. Title: Time variations of aerosol properties in the atmosphere of uranus Authors: Kostogryz, N. M. Bibcode: 2013SoSyR..47...24K Altcode: In the present paper, variations in the vertical structure of the cloud layer of the atmosphere of Uranus in 1981, 1993, and 1995 were analyzed from the data on the geometric albedo of Uranus in the profiles of the absorption bands of methane at λ = 543, 619, 702, 727, 842, 864, 887 nm (Neff, et al., 1984; Karkoschka, 1994; 1998). We used Morozhenko's method that allows us to identify how much the vertical structure of the atmosphere diverges from the conditions of homogeneity. This method is based on the estimation of the optical depths of the layers which form the intensity in the optically-thick vertically homogeneous gasaerosol atmosphere, i.e., the effective optical depths. It has been shown that, at the depths of formation of these absorption bands, there are two extensive cloud layers, the strength of which was maximum in 1981 and minimum in 1995. They are approximately positioned at the levels that correspond to the pressure intervals from 1.4 to 2 bar and from 3.5 to 5.8 bar. Title: Stellar activity, difference spectra, and the dynamical masses of M dwarf companions Authors: Kostogryz, N. M.; Kürster, M.; Lyubchik, Y. Bibcode: 2013MmSAI..84.1047K Altcode: We provide a differential technique that aims at discovering companions to late-type stars by removing the stellar spectrum through subtraction of spectra obtained at different orbital phases and identifying the companion spectrum in the difference spectrum. As we need to observe at different observational epochs our approach may be susceptible to changes in the stellar surface temperature distribution arising from appearing and disappearing star spots. For very active stars the temperature difference between the spots and the photosphere remains a rather unknown parameter. In our simulations we assume a single spot that can have different values of surface filling factor, spot-to-photosphere temperature ratio, and instantaneous radial velocity on the rotating star. For our test case, the M dwarf/brown dwarf binary GJ 1046, we show that the companion difference flux has a larger amplitude than the residual signal from the active star unless extreme spot filling factors and spot-to-photosphere temperature differences are assumed. Title: Simulation of polarimetric effects in planetary system HD 189733 Authors: Frantseva, K.; Kostogryz, N. M.; Yakobchuk, T. M. Bibcode: 2012AASP....2..146F Altcode: In this paper we present results of linear polarization modelling for HD 189733 in the U filter using the Monte Carlo method. Our simulations are based on the well known effect that linear polarization of a centrosymmetric unresolved star becomes non-zero during the planet transit or in the presence of spots on its surface. HD 189733 is currently the brightest (m_{V}=7.67^{m}) known star to harbour a transiting exoplanet. This fact, along with the short orbital period (2.2 d), makes it very suitable for different types of observations including polarimetry. Since we are interested in occultation effects, a very important parameter is the ratio of the planet to star radii, which is also very large (0.15). As the host star is active and spots may cover up to 1% of the planetary surface, we perform our simulations for different spot parameters such as sizes, locations on the stellar disk, and temperatures. Title: Polarimetry of Exoplanetary System CoRoT-2 Authors: Kostogryz, N. M.; Yakobchuk, T. M.; Vidmachenko, A. P. Bibcode: 2012IAUS..282..209K Altcode: We present the results of modelling the polarization resulting from the planetary transits and stellar spots in the system Corot-2 using the Monte Carlo method. The planetary transit was estimated to produce a polarization maximum at the limb of ~5 × 10-6, adopting solar center-to-limb polarization. Assuming different parameters of the spots, we evaluated the flux and polarization changes due to the stellar activity. Title: Spectropolarimetric Observations of Transiting Extrasolar Planetary System HD189733 Authors: Vidmachenko, A. P.; Ivanov, Yu. S.; Kostogryz, N. M. Bibcode: 2012LPI....43.1280V Altcode: Spectropolarimetric observations were carried out with spectropolarimeter mounted in the Cassegrain focus at the 70-cm telescope of Golosiiv (Kyiv). We observed the extrasolar planetary system HD189733 during the planet-crossing of the host star. Title: Asymmetry of reflective properties of the hemispheres of Jupiter satellite Europa Authors: Vidmachenko, Anatoliy; Morozhenko, A.; Klyanchin, A.; Shavlovskiy, V.; Ivanov, Yu.; Kostogryz, N. Bibcode: 2011AstSR...7..133V Altcode: Rotation around the central planet of Europa is synchronous. Leading hemisphere - is much brighter and less polluted by "no ice" material than the trailing one. The high albedo of the satellite may indicates that the ice on the surface is clean enough and is formed recently: 1,5-30 million years ago. Comparison of surface images of spacecrafts "Voyager" and "Galileo" with a low spatial resolution did not detect any significant changes during 20 years. But a detailed analysis of observational data with high resolution points to a number of features on the surface, which may indicate a change in the geological structures during this time. Spectral geometric albedo in the wavelength range 346-750 nm of leading and trailing hemispheres of Galilean satellites were defined using of our spectral observations in 2009 and 2010 and the observations of the other authors at different values of orbital and solar phase angles. The high geometric albedo in the red region of Io and Europa spectrum are confirmed; albedo of Io decreases sharply with decreasing of wavelength for ? < 500 nm; albedo of Ganymede and Callisto - reduced smoothly; albedo of Europa - have an intermediate gradient of reduction. Such behavior of the spectral variation of Europa surface albedo can be explained by deposition of sulfur from Io. Moreover, the sulfur absorption is more strongly on the trailing hemisphere. This indicates that the sulfur on the leading hemisphere is "processed" by meteoritic bombardment much faster and is gone to the the sub-surface regolith layer. Title: Polarimetric study of transiting extrasolar planets Authors: Kostogryz, N. M.; Yakobchuk, T. M.; Morozhenko, O. V.; Vid'Machenko, A. P. Bibcode: 2011MNRAS.415..695K Altcode: 2011MNRAS.tmp..646K We present the results of modelling the polarization produced during planetary transits in the systems HD 189733, TrES-3, Wasp-4 and Wasp-25, using the Monte Carlo method. Polarization maxima at the limb are calculated to be ∼0.022 per cent for HD 189733 with stellar polarization according to Chandrasekhar. The polarization for the system HD 189733 of ∼0.022 per cent is close to that previously published, although this was attributed to scattering of starlight, rather than produced in transit. Using three-dimensional modelling data for the linear polarization of the Sun's continuous spectrum, the limb polarization of the solar-type stars Wasp-25 was calculated to be ∼0.00018 per cent, ∼0.00024 per cent for TrES-3 and ∼0.00016 per cent for Wasp-4 in the B band. It is noted that observations of the Sun-like stars in the Ti I 4536 Å spectral line are particularly suitable for distinguishing between different contributions to the polarization. Also, the shape of the polarization curves, at the near limb transits, can be used for obtaining the inclination of the planet orbit, as a good alternative to standard transit methods. Title: Vertical cloud distribution in the Uranian atmosphere Authors: Kostogryz, N. M. Bibcode: 2011ysc..conf...77K Altcode: In this work, the vertical cloud distribution in the Uranian atmosphere is investigated. We used the method of determinination of the deviation scope of the real atmosphere from homogeneity conditions. The idea of this methods is that the diffusely reflected radiations form at different effective depths in the atmosphere, namely: the strong absorption bands form higher in the atmosphere than weak ones. The same is for separate absorption bands: their centres form in higher atmospheric layers than other points of bands or lines contours. The relative methane concentration for all points of the contours of absorption bands will be the same only for a homogeneous atmosphere and will show the systematic deviation in the center and near the edge of the absorption bands in the case of an inhomogeneous atmosphere. It was obtained that Uranus' atmosphere has two cloud layers: the first one in the region with pressure within the range 1.5-1.8 bar, and the second one in the region with the pressure 3.5-5.5 bar. We also can conclude that aerosol was more abundant in 1981 compared to 1993 and 1995 which was found in our previous work. Title: The first experience of solar eclipse observations with a miniature torsion balance Authors: Pugach, A. F.; Medvedskii, M. M.; Peretyatko, N. N.; Shavlovskii, V. I.; Karbovskii, V. L.; Nikityuk, T. V.; Lazorenko, P. F.; Zolotukhina, A. V.; Vorobyev, D. P.; Pap, V. A.; Lazorenko, G. A.; Vedenicheva, I. P.; Shatokhina, S. V.; Kostogryz, N. M. Bibcode: 2008KPCB...24..253P Altcode: No abstract at ADS Title: Study of the Reasons for the Geometric Albedo Variations of Uranus Authors: Kostogryz, N. M. Bibcode: 2007ysc..conf...44K Altcode: 2007arXiv0712.1492K The method of the optical parameter estimations of the nonisothermal giant planet atmospheres by using intensity data of Raman scattering features was used. We applied this method to the observational data of Uranus' geometric albedo spectra from 1981, 1993 and 1995 and obtained the spectral values of the optical depth, namely, τ_a/τ_R and τ_κ/τ_S (where τ_a, τ_R are aerosol and gas components, τ_S=τ_a+τ_R and τ_κ is absorption component of the effective optical depth of the intensity of diffuse - reflected irradiation forming). We showed that these ratios are different for the three years. The conclusion is that this effect can be due to the horizontal inhomogeneity of aerosol component of optical depth over the Uranus' disk. Title: Probable causes of long-period variations in the Uranian geometrical albedo Authors: Kostogryz, N. M. Bibcode: 2007KPCB...23..214K Altcode: No abstract at ADS Title: The possible reason of the optical parameters changing in the Uranus's atmosphere. Authors: Kostogryz, N. M. Bibcode: 2006IAUJD..10E..38K Altcode: In recent years there has been increasing amount of interest in the influence of Raman scattering on the spectra of planetary atmospheres. Raman scattering is the incoherent non-resonance scattering of photons by molecules. If an incident solar photon of frequency "ν_0" is scattered, it will emerge at frequency "ν_0 + δν " and "ν_0 - δν", where "δν" is the frequency of the Raman transition of the molecule. Raman scattering is a second-order effect in the overall atmospheric radiative transfer problem. It does have several important observable effects on the visible and ultraviolet spectrum of planet, which may provide new information on the composition and structure of these atmospheres. In 1997 Morozhenko demonstrated that the observed geometric albedo for wavelength corresponding to Fraunhofer lines and their "ghosts" was able to be used for estimating values of the ratios of the aerosol and gas optical thicknesses ("τ_a/τ_R") as well as the ratios of the absorbing and scattering components in the aerosol optical thicknesses ("τ_κ/τ_R"). But in this method was considered the model of isothermal atmosphere of giant planets. This method was taken as a basis. We developed a method of the optical parameters estimation of the nonisothermal giant planet atmosphere by using detailed intensity data of Raman scattering. In such a way using observational data of Uranus atmosphere the spectral mean of ratios of the optical thicknesses components: aerosol and gas components ("τ_a/τ_R"), absorbing and scattering components ("τ_κ/τ_R"), and also a single scattering albedo ω of aerosol component were obtained. Applied this calculation code to observational data in 1993 and 1995, observed by Karkoshka, we obtained different values. The average value of ratio τ_&?/τ_R is 0.96 using observation from 1993 in the spectral region of 350-450nm, and value of ratio τ_?/τ_R is 0.82 using observation from 1995 in the same spectral region. In the presence of Raman scattering, albedos are not physical properties of the planets since the albedo is quite dependent on the shape of the solar spectrum. So we obtained a "physical" albedo of Uranus, its albedo corrected for Raman scattering. Title: Raman scattering in Uranus's spectrum with regard to nonisothermal atmosphere Authors: Kostogryz, N. M. Bibcode: 2006KFNT...22..254K Altcode: A method for optical parameter estimation of the nonisothermal giant planet atmospheres is developed by using detailed intensity data on Raman scattering. Morozhenko's method was taken as a basis. Using observational data on Uranus's atmosphere, the spectral values for ratio of the components of the optical depth were obtained, namely, aerosol and gas components (τa/ τR, absorbing and scattering constituent components τκ/(τa + τR), and single scattering albedo omega of aerosol constituent ratio (where τa, τR are aerosol and gas components, and τκ is absorbing component of effective optical depth of the formation of the intensity of diffuse reflected radiation). The average value of the ratio τa/τR is 0.96 but it decreases slowly in the spectral region from 350 to 450 nm. Title: Optical parameters of the nonisothermal Uranus's and Neptune's atmospheres Authors: Kostogryz, N. Bibcode: 2006yosc.conf...61K Altcode: 2006astro.ph..7182K A method of the calculation of optical parameters of the nonisothermal giant planet atmospheres was developed using detailed intensity data of Raman scattering. We have used the model of Morozhenko (A.V. Morozhenko, 1997) as a baseline. In such a way, using observational data of Uranus and Neptune (E.Karkoschka, 1994), the spectral values of ratio of optical depth components: aerosol and gas components ?a/?R, absorbing and scattering components ??/?R, and also single scattering albedo of aerosol component corrected for Raman scattering ? were obtained (where ?a, ?R are aerosol and gas components, and ?? is absorbing components of effective optical depths of the formation of diffusely reflected irradiation). The averaged value of ratio ?a/?R is 0.96 but it slowly decreases in the spectral range of 350-450nm for Uranus and ?a/?R is 1.35 for Neptune. Title: Determination of the optical parameters of the nonisothermal Uranus atmosphere via Raman scattering. Authors: Kostogryz, N. Bibcode: 2006epsc.conf....7K Altcode: Raman scattering. N. Kostogryz Main Astronomical Observatory of NAS of Ukraine, Kyiv, Ukraine (kosn@mao.kiev.ua) Raman scattering is the incoherent non-resonance scattering of photons by molecules. If an incident solar photon of frequency ν0 is scattered, it will emerge at frequency ν0 ± ?ν, where ?ν is the frequency of the Raman transition of the molecule. It does have several important observable effects on the visible and ultraviolet spectrum of planet, which may provide new information on the composition and structure of these atmospheres. In most of the blue and UV region, the solar flux drops almost exponentially with increasing frequency. Many fewer photons will be scattered into a spectral interval than will be scattered out of it. This results in a decrease in geometric albedo of the planet in the blue and UV. A second noticeable aspect of RS results from the absorption lines present in the solar spectrum. Let us consider a spectral element in the center of Fraunhofer line and one in the adjacent continuum. In the core of the line, there are very few incident photons to be Raman scattered out, while there are still just as many photons being scattered in as for the adjacent continuum. This results in a net filling in of the line in the reflected spectrum of the planet. The geometric albedo of Uranus in 350-450nm spectral region is analyzed using a code which explicitly treats Raman scattering of solar photons by H2 . We have used the model of A.V.Morozhenko (1997) as a baseline model. The baseline model demonstrated that the observed geometric albedo for wavelength corresponding to Fraunhofer lines and their "ghosts" was able to be used for estimating values of the ratios of the aerosol and gas optical thicknesses τa/τR as well as the ratios of the absorbing and scattering components in the aerosol optical thicknesses τk/τR . But in this method the model of isothermal atmosphere of giant planets was considered. We developed a code of the optical parameters estimation of the nonisothermal giant planet atmosphere by using detailed intensity data of Raman scattering. The values of aerosol and gas ratios of optical thicknesses components were obtained τa for Uranus τR = 0.96 .We obtained that errors of determination of atmosphere parameters could be near 50% when we don't take into account it experimental temperature profile. And also we corrected single scattering albedo for Raman scattering for nonisothermal atmospheres of Uranus for spectral region 350-450 nm. Title: Some features of formation of details of raman scattering in a non-isothermal atmosphere Authors: Morozhenko, O. V.; Kostogryz, N. M. Bibcode: 2005KFNT...21..114M Altcode: The influence of non-isothermal atmosphere on the intensity of details of the Raman scattering is computed for a spectrum of Neptune. The following inferences are made: the intensity of this scattering depends on the depth of the level of its formation in an optical homogeneous non-isothermal atmosphere; neglect of real temperature profiles during the analysis of observation data leads to large errors in the parameters of the atmosphere upper levels. Title: The manifestations of Raman scattering in the non-isothermic Neptune atmosphere Authors: Kostogryz, N. Bibcode: 2005ysc..conf...73K Altcode: 2005yosc.conf...73K Raman scattering is observing in the UV spectrum of giant planets even with low (1nm) resolution. Since it condition is scattering on the hydrogen molecules that, it is obviously, the intensity of Raman scattering details are lesser when the relative hydrogen concentration is lesser and when the role of aerosol constituent of atmosphere is increaser. Undoubtedly, the appearance of Raman scattering will lead to changing the single-scattering albedo. Raman scattering in the giant planets atmosphere lead to such effect as intensity of Fraunhofer-lines in the diffuse reflected by planets atmosphere are lesser than in the Solar spectrum. This effect leads to pseudo-emission in the UV spectra of giant planet. Raman scattering in the isothermic giant planet atmospheres were considered by Morozhenko (1997). But the planetary atmospheres are gas-aerosol medium, and the optical parameters are changing with altitude. We were computed the influence of non-isothermic atmosphere to intensity of Raman Scattering details in the Neptune atmosphere. There were shown that the intensity of Raman scattering will depend on the depth of its forming level in the optical homogeneous non-isothermic atmosphere and that the mistakes will be large when we don't take into account real temperature profile in the upper levels of atmosphere. Sun spectrum in the interval of wavelengthes ?? = 320 - 400 nm with resolution 0,004 ? was taking. Standard temperature profile of Neptune atmosphere was obtained from the observation data at space vehicle. Title: Appearance of Second Harmonic in the Jupiter Spectrum Authors: Kostogryz, N. M.; Vidmachenko, A. P. Bibcode: 2004LPI....35.1034K Altcode: Such nonlinear atmospheric effect as appearance of second harmonic of the methane bands in the Jupiter spectrum was obtained. The spectral observations received by E. Karkoshka in 1993 and 1995 on the ESO from 300 to 1000 nm were used. Title: Raman scattering in the Jupiter's atmosphere and optical properties of atmospheric aerosol Authors: Kostogryz, N.; Morozhenko, A.; Vidmachenko, A. Bibcode: 2004cosp...35..275K Altcode: 2004cosp.meet..275K The basis of nonlinear atmospheric optic is considered here. When Sun radiation cross the Jupiter's atmosphere, such nonlinear optical effect as Raman scattering will be appear. For our investigations, we used the spectral observations received by E.Karkoshka in 1993 and 1995 on the ESO (European Southern Observatory) from 300 to 1000 nm. We received such nonlinear optical effects as Raman scattering of the methane bands in the Jupiter's spectrum. The vibration-rotation methane bands were considered here. The atmosphere's spectrum is formed on the different height where phisical characteristics of atmosphere are substantial different. That's why we are calculated the influence of Raman scattering effects as function of changing temperature with height in the Jupiter's atmosphere. We demonstrate that for wavelengths corresponding to Fraunhofer lines and their "ghosts", geometric albedo is observed may be used for estimating probable values of the ratios of the aerosol and gas optical thicknesses as well as the ratios of the absorbing and scattering components in the aerosol optical thickness. The ratios of the aerosol and gas optical thicknesses obtained for the Jupiter atmosphere (20±3) agree well with the estimates derived from the analysis of methane absorption bands intensity distributions over the planetary disk.