STELLAR WIND VELOCITY OF THE MASSIVE COMPONENT IN THE HIGH MASS X-RAY BINARY OAO 1657
Section: STARS AND THE INTERSTELLAR MEDIUM
Authors:
1.
Pulkovo Observatory
Institute of Applied Astronomy of the Russian Academy of Sciences
Institute of Applied Astronomy of the Russian Academy of Sciences
2.
Pulkovo Observatory
3.
Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo
Fesenkov Astrophysical Institute
Fesenkov Astrophysical Institute
Type:
Сonference article
Published:
27.12.2024
Subject area:
UDC 52
UDC 53
UDC 520
UDC 521
UDC 523
UDC 524
UDC 52-1
UDC 52-6
CSCSTI 41.00
CSCSTI 29.35
CSCSTI 29.31
CSCSTI 29.33
CSCSTI 29.27
CSCSTI 29.05
Russian Classification of Professions by Education 03.06.01
Russian Classification of Professions by Education 03.05.01
Russian Classification of Professions by Education 03.04.03
Russian Library and Bibliographic Classification 2
Russian Library and Bibliographic Classification 223
Russian Trade and Bibliographic Classification 614
Russian Trade and Bibliographic Classification 6135
BISAK SCI004000 Astronomy
BISAK SCI005000 Physics / Astrophysics
UDC 53
UDC 520
UDC 521
UDC 523
UDC 524
UDC 52-1
UDC 52-6
CSCSTI 41.00
CSCSTI 29.35
CSCSTI 29.31
CSCSTI 29.33
CSCSTI 29.27
CSCSTI 29.05
Russian Classification of Professions by Education 03.06.01
Russian Classification of Professions by Education 03.05.01
Russian Classification of Professions by Education 03.04.03
Russian Library and Bibliographic Classification 2
Russian Library and Bibliographic Classification 223
Russian Trade and Bibliographic Classification 614
Russian Trade and Bibliographic Classification 6135
BISAK SCI004000 Astronomy
BISAK SCI005000 Physics / Astrophysics
Language:
English
Keywords:
stars: pulsars: general, winds, outflows; X-rays: binaries; accretion; individual: OAO 1657–415
Abstract (English):
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.
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.
Keywords:
stars: pulsars: general, winds, outflows; X-rays: binaries; accretion; individual: OAO 1657–415
stars: pulsars: general, winds, outflows; X-rays: binaries; accretion; individual: OAO 1657–415
1. Delgado-Martí H., Levine A.M., Pfahl E., et al., 2001, Astrophysical Journal, 546, 1, p. 455
2. Ikhsanov N.R., Kim V.Yu., Beskrovnaya N.G., 2024, Publications of the Pulkovo Observatory, 233, p. 34
3. Saavedra E.A., Fogantini F.A., Combi J.A., et al., 2022, Astronomy & Astrophysics, 659, id. A48
