Radiative Instability in Stellar Envelopes

Details Radiative Instability in Stellar Envelopes Radiative Instability in Stellar Envelopes

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003apj...599l.103s&link_type=abstract

The Astrophysical Journal, Volume 599, Issue 2, pp. L103-L105.

Other

2

Stars: Interiors, Stars: Mass Loss, Stars: Variables: Other, Stars: Wolf-Rayet, Stars: Supergiants

Scientific paper

A general analytic criterion for radiative instability in the envelope of a nonexplosive star is derived, based on a generalization of the Eddington limit for the star's luminosity, an expression for the stationary mass-loss acceleration, and an assumed universality of the critical mean density of the envelope. The derived criterion has been formulated as the minimum rate of mass loss needed to achieve a super-Eddington state. Expressed as a simple function of luminosity and effective temperature, it is applied to luminous blue variables (LBVs), Wolf-Rayet stars, and ordinary B-type supergiants. Assuming that the brightest LBVs as well as most of the Wolf-Rayet stars are post-main-sequence objects, these objects must have radiatively unstable envelopes.

Affiliated with

Also associated with

No associations

Rating

Radiative Instability in Stellar Envelopes does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Radiative Instability in Stellar Envelopes, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Radiative Instability in Stellar Envelopes will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1652276