Nonradial pulsation and mass loss in early B stars
Technical Report
·
OSTI ID:5605629
It has been firmly established that nonradial pulsation (NRP) probably occurs in nearly all sharp-lined early B stars near the main sequence. A recent breakthrough occurred with the discovery of quasi emission/absorption bumps moving across the line profiles of the rapid rotators zeta Oph and alpha Vir. It was found that an intermediate-1 (1 8) NRP mode is responsible for these features in zeta Oph. Some 20 Be and Bn stars were monitored and convincing evidence for NRP in 13 of them was found. Line-profile variations suggestive of NRP in the other 7 were also discovered. A search for line-profile variables among moderate rotators has turned up NRP in epsilon and eta Lep, with v sin i's of 140 and 70 km/sec, respectively. It now seems that NRP can be present at all rotational velocities with equal frequency (near 100%) . However, at most, 20% of these stars exhibit detectable photometric variations.
- Research Organization:
- Lick Observatory, Santa Cruz, CA (USA)
- OSTI ID:
- 5605629
- Report Number(s):
- N-85-17759
- Country of Publication:
- United States
- Language:
- English
Similar Records
Connection between nonradial pulsations and stellar winds in massive stars. III. Episodic mass motions and surface phenomena
Line profile variations caused by low-frequency nonradial pulsations of rapidly rotating stars
Connection between nonradial pulsations and stellar winds in massive stars. I. Nonradial pulsation theory of massive stars
Journal Article
·
Tue Dec 31 23:00:00 EST 1985
· Publ. Astron. Soc. Pac.; (United States)
·
OSTI ID:5615165
Line profile variations caused by low-frequency nonradial pulsations of rapidly rotating stars
Journal Article
·
Wed Jan 31 23:00:00 EST 1990
· Astrophysical Journal; (USA)
·
OSTI ID:6851958
Connection between nonradial pulsations and stellar winds in massive stars. I. Nonradial pulsation theory of massive stars
Journal Article
·
Tue Dec 31 23:00:00 EST 1985
· Publ. Astron. Soc. Pac.; (United States)
·
OSTI ID:5615169