Stability of supermassive stars near the critical mass

Details Stability of supermassive stars near the critical mass Stability of supermassive stars near the critical mass

Sep 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975crasb.281..141s&link_type=abstract

Academie des Sciences (Paris), Comptes Rendus, Serie B - Sciences Physiques, vol. 281, no. 10, Sept. 8, 1975, p. 141-144. In Fr

Physics

Critical Mass, Dynamic Stability, Modal Response, Perturbation Theory, Stellar Mass, Equations Of Motion, Modes, Secular Variations, Supergiant Stars, Vibration Mode

Scientific paper

Results of a calculation of the normal modes of linear radial perturbation of supermassive stars of near-critical mass are presented. Dynamic modes were calculated in the adiabatic approximation; secular modes were calculated omitting acceleration terms in the equation of motion, which amounts to assuming hydrostatic equilibrium. Below the critical mass, two of the fundamental modes are dynamic modes which are made vibrationally unstable by the nonadiabatic terms; above the critical mass, one of these modes becomes secular. It is thus shown that the distinction between dynamic and secular modes is not absolute.

Affiliated with

Also associated with

No associations

Rating

Stability of supermassive stars near the critical mass 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 Stability of supermassive stars near the critical mass, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Stability of supermassive stars near the critical mass will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-910730