Nonradial pulsation and mass loss in early B stars

Details Nonradial pulsation and mass loss in early B stars Nonradial pulsation and mass loss in early B stars

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985nascp2358...53p&link_type=abstract

In NASA. Goddard Space Flight Center The Origin of Nonradiative Heating/Momentum in Hot Stars p 53-56 (SEE N85-17755 08-88)

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1

B Stars, Early Stars, Electromagnetic Pulses, Stellar Mass Ejection, Variable Stars, Amplitudes, Stellar Rotation, Supergiant Stars

Scientific paper

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.

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