抄録
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.
本文言語 | English |
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ページ(範囲) | 57-59 |
ページ数 | 3 |
ジャーナル | Astrophysics and Space Science |
巻 | 119 |
号 | 1 |
DOI | |
出版ステータス | Published - 1986 1 1 |
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science