ENERGY STRUCTURE OF THE ACCRETION DISK CORONA IN X 1822-371

被引：10

作者：

HELLIER, C ^{[1
]}

MASON, KO ^{[1
]}

WILLIAMS, OR ^{[1
]}

机构：

[1] UNIV LEICESTER, DEPT PHYS & ASTRON, LEICESTER LE1 7RH, ENGLAND

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 1992年 / 258卷 / 03期

关键词：

ACCRETION; ACCRETION DISKS; BINARIES CLOSE; STARS INDIVIDUAL X1822-371-X-RAYS STARS;

D O I：

10.1093/mnras/258.3.457

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Ginga observations of the LMXB X 1822 - 371 show that the broad orbital modulation and the eclipse are deeper at higher energies. This is explained if the X-ray emitting corona produces softer emission at greater heights from the disc plane, which suggests that either the corona is optically thick, or that the illuminating X-rays are anisotropic. Further investigation is hampered by an inadequate understanding of the X-ray spectrum of X 1822 - 371.

引用

页码：457 / 460

页数：4

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