Accretion disk corona line emission from X0614+091

Details Accretion disk corona line emission from X0614+091 Accretion disk corona line emission from X0614+091

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...422..791c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 422, no. 2, p. 791-798

Astronomy and Astrophysics

Astronomy

17

Accretion Disks, Emission Spectra, Line Spectra, Stellar Coronas, X Ray Astronomy, X Ray Binaries, X Ray Spectra, Astronomical Spectroscopy, Heao 2, Iron, Oxygen, Spaceborne Astronomy, X Ray Spectroscopy

Scientific paper

The low-mass X-ray binary X0614+091 was observed on 3 days in 1979 with the Einstein Observatory solid state spectrometer and the monitor proportional counter. During the observation with the highest measured flux, corresponding to an X-ray luminosity of 8 x 1036 erg/s (in the 0.5-20 keV band for an assumed distance of 5 kpc), significant low-energy emission was detected, centered at 0.77 keV, possibly due to line emission for O VII-O VIII and Fe XVII-Fe XIX. The other observations, which were at fluxes lower by a factor of 2, are consistent with the presence of the emission feature. The equivalent width of the feature, 37 +/- 6 eV, is of the same order as equivalent widths previously reported for more luminous low-mass X-ray binaries using grating spectrometer data. The soft X-ray lines could be emitted by gas expected to arise in an accretion disk corona excited by the central source. But to explain the observed feature, most of the corona needs to contribute, or other sources of emission are required.

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