Steady mass-loss from supermassive stars

Mariko Kato

Research output: Contribution to journalArticle

8 Citations (Scopus)

Abstract

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
Volume119
Issue number1
DOIs
Publication statusPublished - 1986 Jan
Externally publishedYes

Fingerprint

supermassive stars
critical mass
Population I stars
Population III stars
Hertzsprung-Russell diagram
stars
radiation pressure
opacity
massive stars
loss
continuums
radii
expansion
causes
diagram

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Steady mass-loss from supermassive stars. / Kato, Mariko.

In: Astrophysics and Space Science, Vol. 119, No. 1, 01.1986, p. 57-59.

Research output: Contribution to journalArticle

Kato, Mariko. / Steady mass-loss from supermassive stars. In: Astrophysics and Space Science. 1986 ; Vol. 119, No. 1. pp. 57-59.
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