Lomonosov Moscow State University, Faculty of Physics
Moscow, Moscow, Russian Federation
UDK 53 Физика
UDK 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
UDK 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
UDK 523 Солнечная система
UDK 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
UDK 52-1 Метод изучения
UDK 52-6 Излучение и связанные с ним процессы
GRNTI 41.00 АСТРОНОМИЯ
GRNTI 29.35 Радиофизика. Физические основы электроники
GRNTI 29.31 Оптика
GRNTI 29.33 Лазерная физика
GRNTI 29.27 Физика плазмы
GRNTI 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
OKSO 03.06.01 Физика и астрономия
OKSO 03.05.01 Астрономия
OKSO 03.04.03 Радиофизика
BBK 2 ЕСТЕСТВЕННЫЕ НАУКИ
BBK 223 Физика
TBK 614 Астрономия
TBK 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
The most reliable method for estimating the rate of mass-loss by the Wolf–Rayet stars wind is based on the assessment of secular variations in the orbital periods for close binary systems containing such stars, most often WR+OB systems. Previously, almost only photometric observations of well-studied eclipsing close WR+OB binaries were used for these purposes. This report describes the results of the work on the search for mass-loss-induced evolutionary variations in the orbital period for close WR+OB binaries and the mass-loss rates measurements for WR stars in these systems. Orbital period variations were detected in five systems studied: V444 Cyg, CQ Cep, CX Cep, WR 127 (Hen 3-1772), and WR 141 (V2183 Cyg). In addition, phase deviations between the radial velocity curves obtained at different epochs are suspected for the A pair of the GP Cep quadruple system. For eclipsing systems, estimates of the rate of change of the orbital period from the radial velocity curves are in good agreement with the corresponding estimates obtained from the light curves. A secular shortening of the orbital period has been confirmed for the CQ Cep system, which can be explained by the high degree of closeness of this system and the associated mass transfer processes. For the WR 127 and WR 141 systems, dynamic estimates of the change of the orbital period and the rate of mass loss have been obtained for the first time. Estimates of the rate of mass-loss by Wolf-Rayet stars show a power-law dependence on the mass of the star with an exponent of about 2. The effect of the finite size of stars, which turns out to be significant for estimates of the rate of mass loss to the wind in the closest systems, is discussed.
stars: Wolf–Rayet, mass-loss, winds, outflows, binaries: spectroscopic
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