Kafuku, S.,
Yamauchi, S.,
Yamauchi, M.,
河合 誠之,
Matsuoka, M.,
Koyama, K.,
Kifune, T..
英文:
Kafuku, S.,
Yamauchi, S.,
Yamauchi, M.,
Kawai, N.,
Matsuoka, M.,
Koyama, K.,
Kifune, T..
言語
English
掲載誌/書名
和文:
英文:
Monthly Notices of the Royal Astronomical Society
巻, 号, ページ
Vol. 268
pp. 437
出版年月
1994年5月
出版者
和文:
英文:
会議名称
和文:
英文:
開催地
和文:
英文:
アブストラクト
Ginga observations have confirmed the extended hard X-ray component around Cyg X-3 which has been detected by EXOSAT. Scanning observations of Cyg X-3 show that this component extends up to 20 from Cyg X-3 along the Galactic plane. The surface brightness observed by Ginga is consistent with that observed by the EXOSAT ME. The ratio of the count rates in the 3-6 and 6-10 keV bands shows that the extended component has either a thermal bremsstrahiung spectrum with a temperature of 612 keV or a power-law spectrum with a photon index of 2.310.3. If this is associated with Cyg X-3, the X-ray luminosity in the 2-10 keV band is estimated to be about lx 1036 erg s- . We discuss two alternative explanations for the origin of the X-ray halo: thermal emission from a hot gas or synchrotron radiation of the ultra-high-energy electrons which are expected to be produced along with ultra-high-energy y-rays. Key words: radiation mechanisms: non-thermal - binaries: close - stars: individual: Cyg X-3 - X-rays: stars.
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