Energy structure of the accretion disc corona in X 1822-371.
Abstract
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.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- October 1992
- DOI:
- 10.1093/mnras/258.3.457
- Bibcode:
- 1992MNRAS.258..457H
- Keywords:
-
- Accretion Disks;
- Binary Stars;
- Stellar Coronas;
- X Ray Stars;
- Exosat Satellite;
- Ginga Satellite;
- Light Curve;
- Spaceborne Astronomy;
- Stellar Orbits;
- Stellar Spectra;
- Astrophysics