STELLAR WIND VELOCITY OF THE MASSIVE COMPONENT IN THE HIGH MASS X-RAY BINARY OAO 1657$-$415
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:
52
53
520
521
523
524
52-1
52-6
41.00
29.35
29.31
29.33
29.27
29.05
03.06.01
03.05.01
03.04.03
2
223
614
6135
SCI004000
SCI005000
53
520
521
523
524
52-1
52-6
41.00
29.35
29.31
29.33
29.27
29.05
03.06.01
03.05.01
03.04.03
2
223
614
6135
SCI004000
SCI005000
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
