Steady mass-loss from supermassive stars

Abstract

Structures of Newtonian super-massive stars are calculated with the opacity for Comptor effectK ₀/(1 + αT), whereK ₀=0.21(1 +X and α=2.2×10⁻⁹K⁻¹. The track of the Main-Sequence is turned right in the 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 1.02×10⁶ M _⊙ for a Population I star, and 1.23×10⁵ M _⊙ for Population III star. Mass loss rates expected in these stars are 3.3×10⁻³ and 4.0×10⁻³ M _⊙ yr⁻¹, respectively.