Steady Mass-Loss from Supermassive Stars

Abstract

Structures of Newtonian super-massive stars are calculated with the opacity for Compton effect K ₀/(1 + αT), where k ₀ = 0.2(1 + X) and α = 2.2 × 10⁻⁹ K⁻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 x 10⁻³ and 4.0 × 10 ⁻³ M _⊙ yr⁻¹, respectively.