Kitamoto, S.,
Hirano, A.,
Kawashima, K.,
Miyamoto, S.,
Nagase, F.,
White, N. E.,
Smale, A. P.,
Soong, Y.,
Matsuoka, M.,
河合 誠之,
Yoshida, A..
英文:
Kitamoto, S.,
Hirano, A.,
Kawashima, K.,
Miyamoto, S.,
Nagase, F.,
White, N. E.,
Smale, A. P.,
Soong, Y.,
Matsuoka, M.,
Kawai, N.,
Yoshida, A..
言語
English
掲載誌/書名
和文:
英文:
Publications of the Astronomical Society of Japan
巻, 号, ページ
Vol. 47
pp. 233-238
出版年月
1995年4月
出版者
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英文:
会議名称
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英文:
開催地
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英文:
アブストラクト
We describe the orbital period change of the X-ray binary Cygnus X-3, and present three new times of X-ray minima, obtained using the Ginga and ASCA satellites. Before 1990, the long-term ephemeris of Cyg X-3 required the introduction of a second time derivative, ddot {P}, of order -(1.27 +/- 0.19) times 10(-10) yr(-1) . This value indicates that the first time derivative, dot {P}, changes from a positive to a negative value around 1986. However, the new ASCA data points presented here do not confirm this large ddot {P} variation and indicate a significantly smaller ddot {P} of -(8.13 +/- 1.15) times 10(-11) yr(-1) and a global period change of dot {P}/P = (1.17 +/- 0.44) times 10(-6) yr(-1) . The derived dot {P} can be explained by a large mass-loss rate of 0.58 times 10(-6) M_T yr(-1) , where M_T is the total mass of the Cyg X-3 system. This value is consistent with the expected mass-loss rate of the Wolf-Rayet star of about 10(-6) MO yr(-1) . The existence of a red-noise type fluctuation is also described.
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