Energy structure of the accretion disc corona in X 1822-371

Details Energy structure of the accretion disc corona in X 1822-371 Energy structure of the accretion disc corona in X 1822-371

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.258..457h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 258, no. 3, p. 457-460.

Astronomy and Astrophysics

Astronomy

11

Accretion Disks, Binary Stars, Stellar Coronas, X Ray Stars, Exosat Satellite, Ginga Satellite, Light Curve, Spaceborne Astronomy, Stellar Orbits, Stellar Spectra

Scientific paper

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.

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