Перегляд за Автор "Glazunova, L. V."

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  • Ескіз
    Документ
    CHEMICAL EVOLUTION IN ALGOLS
    (Astroprint, 2012) Glazunova, L. V.
    ABSTRACT. We discuss the chemical abundance in Algol-type systems produced by different authors. Till this time most evolutionary changes in the chemical abundance of the components of Algols were studied by carbon depletion. We obtained the following results: 1) detections of carbon abundance in the atmosphere of donor were reported in two articles, but them don’t show dependence from the mass ratio and the mass donor, 2) the carbon abundance in the atmosphere accretor for the same system in research different authors is very different, also it isn’t dependency from the ratio of the masses and the masses of accretor. Summary: while were observed evolutionary changes in the carbon abundance for Algol’s component, but a precision was low and studied the small number of systems and can not linke to the carbon abundance and mass ratio and also the masses of the components – the parameters of the binary system evolution.
  • Ескіз
    Документ
    The chemical composition of the active stars
    (Одеський національний університет імені І. І. Мечникова, 2016) Glazunova, L. V.
    The comparison of the results of the studies of the active stars’ chemical composition obtained by different authors has been performed. It was concluded that the difference between the abundances of some elements in active and inactive stars becomes significant (> 3 ) only for the active stars with high chromospheric activity (lgR′HK > 􀀀4). This is the case primarily for the light elements, namely Li, Na and Al, as well as heavy elements with Z > 30.
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    Документ
    THE DETERMINATION OF ABSOLUTE PARAMETERS AND ABUNDANCE OF COMPONENTS BINARY SYSTEMS: THE SPECIFICITY AND PROBLEMS
    (Astroprint, 2013) Glazunova, L. V.
    ABSTRACT. Spectroscopic binaries remain a laboratory for testing the stellar atmospher and the stellar evolution theories. It’s considering problems determination of parameters of components and their errous for example two spectroscopic binaries with the mainsequence components BW Boo and OU Gem.
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    Документ
    THE NEW ABSOLUTE PARAMETERS OF OU GEM - THE STAR OF BY DRA TYPE
    (Astroprint, 2010) Mishenina, T. V.; Glazunova, L. V.; Soubiran, C.; Kovtyukh, Valery V.
    The spectra of OU Gem were obtained with the fiber-fed echelle spectrograph SOPHIE at the 1.93-m telescope of the Observatoire de Haute-Provence (France). The temperatures of components of the system were defined and are equal to 5013 ± 15 K and 4486±50 K for primary (A) and secondary(B) components, accordingly. The rotation velocity of components are measured: for primary component it is equal to 5.1±1 km/s and 6.2 ± km/s for the secondary one. The definition of radial velocities of components by LSD profile method and redetermination of spectral orbital elements were carried out. New absolute parameters of components were obtained too.
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    Документ
    THE NUMERICAL THREE-DIMENSIONAL HYDRODYNAMIC SIMULATION OF COLLIDING STELLAR WINDS IN A CLOSE BINARY SYSTEM
    (Astroprint, 2013) Nazarenko, V. V.; Glazunova, L. V.; Nazarenko, S. V.
    In the present numerical study the stellar winds from both supergiant-components of a detached close binary system (CBS) are simulated applying methods of the three-dimensional numerical hydrodynamics. The simulated winds collide in the space between the components, forming a stationary shock wave. That shock wave has geometrically intricate shape that consists of several separate filamentary structures. The temperature in the shock wave is about 105K, and the temperature in the space adjacent to the shock wave is around 104 - 1.5 104K. Away from the line-of-centres the shock wave is curved due to the effect of the Coriolis forces and greatly expands under the gas pressure at that. At a distance of about two orbital separations from the line-of-centres the shock wave expands so much that it is practically smearing out in space.
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    THE NUMERICAL THREE-DIMENSIONAL HYDRODYNAMIC SIMULATION OF THE -RAY BURSTERS AND X-RAY BURSTERS
    (Astroprint, 2013) Nazarenko, V. V.; Glazunova, L. V.; Nazarenko, S. V.
    An radiative wind accretion onto the compact object in a detached close binary system (CBS) where one of the components is a supergiant with radiation stellar wind that blows from its surface, and another component is a compact object (black hole or neutron star), is simulated applying methods of three-dimensional numerical hydrodynamics. The simulation of bursts similar to the gamma-ray bursters and X-ray bursters, i.e. isolated bursts with nearly zero in time ascending and descending branches with amplitudes from 6 - 7m to 15 - 18m, commences in the vicinity of the compact object when the precession of the donor star starts. Due to the course numerical spatial grid of 0.01 units of the orbital separation, the duration of such isolated bursts is 10-40 minutes of the orbital time. The burst simulation is as follows: when the donor stars precession starts, small grid-cell-sized regions of higher density appear in the vicinity of the compact object due to the RayleighTaylor instability. The temperature in one of those regions increases abruptly when they interact with the stellar wind from the donor star. Prior to the temperature increase, the indicated regions were radiopaque. When the temperature reaches its peak, those regions become radiolucent, and all energy contained there is momentarily illuminated, giving off a burst that appears as an isolated sharp peak. That is how the bursts similar to the gamma-ray bursts and X-ray bursts are simulated.