Steady mass-loss from supermassive stars |
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| Authors: | Mariko Kato |
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| Institution: | (1) Department of Astronomy, Faculty of Science, University of Tokyo, Bunkyo-ku, Tokyo, Japan |
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| Abstract: | Structures of Newtonian super-massive stars are calculated with the opacity for Comptor effectK
0/(1 +  T), whereK
0=0.21(1 +X and =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 1.02×106
M
 for a Population I star, and 1.23×105
M
for Population III star. Mass loss rates expected in these stars are 3.3×10–3 and 4.0×10–3
M
yr–1, respectively.Paper presented at the IAU Third Asian-Pacific Regional Meeting, held in Kyoto, Japan, between 30 September–6 October, 1984. |
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