| タイトル | Stellar contributions to the hard X-ray galactic ridge |
| 本文（外部サイト） | http://hdl.handle.net/2060/19830006963 |
| 著者（英） | Marshall, F. E.; Worrall, S. M. |
| 著者所属（英） | NASA Goddard Space Flight Center |
| 発行日 | 1982-10-01 |
| 言語 | eng |
| 内容記述 | The number density of serendipitous sources in galactic plane Einstein Observatory IPC fields are compared with predictions based on the intensity of the HEAO-1 A2 unresolved hrd X-ray galactic ridge emission. It is concluded that theoretically predicted X-ray source populations of luminosity 8 x 10 to the 32nd power to 3 x 10 to the 34th power ergs s have 2 KeV to 10 KeV local surface densities of less than approximately .0008 L(32) pc/2 and are unlikely to be the dominant contributors to the hard X-ray ridge. An estimate for Be/neutron star binary systems, such as X Persei, gives a 2 keV to 10 keV local surface density of approximately 26 x 10 to the -5 power L(32) pc/2. Stellar systems of low luminosity, are more likely contributors. Both RS CVn and cataclysmic variable systems contribute 43% + or - 18% of the ridge. A more sensitive measurement of the ridge's hard X-ray spectrum should reveal Fe-line emission. We speculate that dM stars are further major contributors. |
| NASA分類 | ASTRONOMY |
| レポートNO | 83N15234
NAS 1.15:84932
NASA-TM-84932
REPT-661 |
| 権利 | No Copyright |
| URI | https://repository.exst.jaxa.jp/dspace/handle/a-is/163928 |
