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Chemical Abundances of Early Type Stars

Published online by Cambridge University Press:  25 May 2016

S. Tanaka ,
S. Kitamoto ,
T. Suzuki ,
K. Torii ,
M.F. Corcoran  and
W. Waldron
S. Tanaka
Affiliation:
Osaka University, Department of Earth and Space Science, Osaka University 1-1, Machikaneyama-cho, Toyonaka, Osaka, 560, Japan
S. Kitamoto
Affiliation:
Osaka University, Department of Earth and Space Science, Osaka University 1-1, Machikaneyama-cho, Toyonaka, Osaka, 560, Japan
T. Suzuki
Affiliation:
Osaka University, Department of Earth and Space Science, Osaka University 1-1, Machikaneyama-cho, Toyonaka, Osaka, 560, Japan
K. Torii
Affiliation:
Osaka University, Department of Earth and Space Science, Osaka University 1-1, Machikaneyama-cho, Toyonaka, Osaka, 560, Japan
M.F. Corcoran
Affiliation:
Laboratory for High Energy Astrophysics, NASA/GSFC, Greenbelt, MD20771, USA
W. Waldron
Affiliation:
Applied Research Corp., 8201 Corporate Dr., Landover MD 20785, USA

Extract

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X-rays from early-type stars are emitted by the corona or the stellar wind. The materials in the surface layer of early-type stars are not contaminated by nuclear reactions in the stellar inside. Therefore, abundance study of the early-type stars provides us an information of the abundances of the original gas. However, the X-ray observations indicate low-metallicity, which is about 0.3 times of cosmic abundances. This fact raises the problem on the cosmic abundances.

Type
Session 1: Plasma and Fresh Nucleosynthesis Phenomena
Information
Symposium - International Astronomical Union , Volume 188: The Hot Universe , 1998 , pp. 224 - 225
Copyright
Copyright © Kluwer 1998