Steady mass-loss from supermassive stars

Structures of Newtonian super-massive stars are calculated with the opacity for Comptor effect K₀/(1 + αT), where K₀=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 1.02×10⁶M_⊙ for a Population I star, and 1.23×10⁵M_⊙ for Population III star. Mass loss rates expected in these stars are 3.3×10^-3 and 4.0×10^-3M_⊙ yr^-1, respectively.