Stellar wind velocity of the massive component in the high mass X-ray binary OAO 1657$-$415
The parameters of the wind-fed accretion process in the massive X-ray binary OAO 1657−415 are discussed. We show that the X-ray luminosity of an accreting pulsar in this system can be explained only if the velocity of the stellar wind of the massive component in the orbital plane of the binary system is in the range of 200–500 km/s.
Authors
- N. R. Ikhsanov (ORCID: https://orcid.org/0000-0002-3326-5588)
- Vitaliy Kim (ORCID: https://orcid.org/0000-0003-1202-9751)
- N. G. Beskrovnaya (ORCID: https://orcid.org/0000-0003-4454-6729)
Institutions
- Pulkovo Observatory (RU)
- Fesenkov Astrophysical Institute (KZ)
- Institute of Applied Astronomy (RU)
Publication Details
- Published
- 2024-12-27
- DOI
- https://doi.org/10.26119/vak2024.060
- Primary Topic
- Astrophysical Phenomena and Observations
- Type
- article
- Field-Weighted Citation Impact
- 0.00