Kinematics, close binary evolution, and ages of the O stars.
Abstract
Accurate proper motions were determined for O4-B2 stars, Wolf-Rayets, and B9-K3 supergiants. Space velocities were calculated for these stars and used to investigate the kinematics of the O stars. Observations suggest that the group H stars were produced from mass exchange in massive close binary (MCB) systems, and the high space velocities typical of these stars were caused by binary supernovae. Hence, 50% of the O stars were probably produced by mass accretion in MCS systems. A model is presented describing the evolution of a MCB system for the case of no mass loss from the system: (1) for stars exploding as supernovae, 15% of the initial stellar mass will form a collapsed remnant, (2) stars with masses at least equal to 12 solar masses will eventually explode as supernovae, and (3) the group H stars with masses greater than 45 solar masses probably have black hole binary companions.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- September 1979
- DOI:
- 10.1086/157311
- Bibcode:
- 1979ApJ...232..520S
- Keywords:
-
- Binary Stars;
- Kinematics;
- O Stars;
- Stellar Evolution;
- Stellar Mass Accretion;
- Stellar Motions;
- Black Holes (Astronomy);
- Companion Stars;
- Early Stars;
- Star Distribution;
- Stellar Models;
- Velocity Distribution;
- Astrophysics;
- Close Binaries:O Stars;
- O Stars:Evolution;
- O Stars:Kinematics;
- Proper Motions:Stars;
- Space Velocities:Stars