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Discovery of orbital Eccentricity and Evidence for orbital Period Increase of SS433статья
Статья опубликована в высокорейтинговом журнале
Статья опубликована в журнале из списка Web of Science и/или ScopusДата последнего поиска статьи во внешних источниках: 10 ноября 2021 г.
- Авторы: Cherepashchuk A.M., Belinski A.A., Dodin A.V., Postnov K.A.
- Журнал: Monthly Notices of the Royal Astronomical Society
- Том: 507
- Год издания: 2021
- Издательство: Oxford Journals, Oxford University Press
- Местоположение издательства: Oxford, UK, England
- Первая страница: L19
- Последняя страница: L23
- DOI: 10.1093/mnrasl/slab083
- Аннотация: The examination of long-term (1979-2020) photometric observations of SS433 enabled us to discover a non-zero orbital eccentricity of e = 0.05 ± 0.01. We have also found evidence for a secular increase in the orbital period at a rate of P˙b=(1.0±0.3)×10−7 s s−1. The binary orbital period increase rate makes it possible to improve the estimate of the binary mass ratio q = MX/MV > 0.8, where MX and MV are the masses of the relativistic object and the optical star, respectively. For an optical star mass of 10M⊙, the mass of the relativistic object (a black hole) is MX > 8M⊙. A neutron star in SS433 is reliably excluded because in that case the orbital period should decrease, in contradiction to observations. The derived value of P˙b sets a lower limit on the mass-loss rate in the Jeans mode from the binary system ≳ 7 × 10−6M⊙yr−1. The discovered orbital ellipticity of SS433 is consistent with the model of the slaved accretion disc tracing the precession of the misaligned optical star’s rotational axis.
- Добавил в систему: Додин Александр Владимирович