Steady mass-loss from supermassive stars

Mariko Kato

doi:10.1007/BF00648812

Steady mass-loss from supermassive stars

Mariko Kato

Research output: Contribution to journal › Article › peer-review

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 language	English
Pages (from-to)	57-59
Number of pages	3
Journal	Astrophysics and Space Science
Volume	119
Issue number	1
DOIs	https://doi.org/10.1007/BF00648812
Publication status	Published - 1986 Jan
Externally published	Yes

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1007/BF00648812

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title = "Steady mass-loss from supermassive stars",

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.",

author = "Mariko Kato",

year = "1986",

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doi = "10.1007/BF00648812",

language = "English",

volume = "119",

pages = "57--59",

journal = "Astrophysics and Space Science",

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AB - 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.

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Steady mass-loss from supermassive stars

Abstract

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