A model of X Persei.
Abstract
A possible model for a close binary system X Persei is discussed. We present evidence that the primary is a post mass loss star of about 5 solar masses, and the secondary is a rapidly rotating star of about 25 solar masses, surrounded by the gaseous disk accreted in the recent phase of mass exchange. We cannot exclude the possibility that the 25 solar mass object in the center of the accretion disk is a black hole, but a possible evolutionary pattern leading to such a configuration is unnecessarily complicated. We predict light variation with an orbital period of about 584 days and with the luminosity maximum at the phase when the B 0 primary is in front. We do not discuss the source of weak X-ray emission.
- Publication:
-
Astronomy and Astrophysics
- Pub Date:
- May 1975
- Bibcode:
- 1975A&A....40..351P
- Keywords:
-
- Astronomical Models;
- Binary Stars;
- Stellar Mass;
- X Ray Sources;
- Black Holes (Astronomy);
- Light Curve;
- Stellar Evolution;
- Stellar Luminosity;
- Stellar Mass Ejection;
- Stellar Rotation;
- X Ray Stars;
- Astrophysics