Steady mass-loss from supermassive stars

Mariko Kato

Research output: Contribution to journalArticlepeer-review

8 Citations (Scopus)


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.

Original languageEnglish
Pages (from-to)57-59
Number of pages3
JournalAstrophysics and Space Science
Issue number1
Publication statusPublished - 1986 Jan
Externally publishedYes

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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