Steady mass-loss from supermassive stars

Details Steady mass-loss from supermassive stars Steady mass-loss from supermassive stars

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.119...57k&link_type=abstract

(IAU, Asian-Pacific Regional Meeting, 3rd, Kyoto, Japan, Sept. 30-Oct. 5, 1984) Astrophysics and Space Science (ISSN 0004-640X),

Statistics

Computation

3

Computational Astrophysics, Opacity, Stellar Mass Ejection, Stellar Structure, Supermassive Stars, Compton Effect, Hertzsprung-Russell Diagram, Main Sequence Stars, Mass Flow Rate, Newtonian Fluids, Stellar Evolution

Scientific paper

Structures of Newtonian supermassive stars are calculated with the opacity for Compton effect κ0/(1+αT), where κ0 = 0.2(1+X) and α = 2.2×10-9K-1. The track of the main-sequence is turned right in upper part of the HR diagram. Mass loss will occur in a main-sequence stage for a star with mass larger than a critical mass. The cause of mass loss and the expansion of the radius is continuum radiation pressure. The critical mass for mass loss is 1.02×106M_sun; for a Population I star, and 1.23×105M_sun; for Population III star. Mass loss rates expected in these stars are 3.3×10-3 and 4.0×10-3M_sun;yr-1, respectively.

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