EXOSAT observations of H2252-035 - Pulse phase and orbital phase dependent low energy absorption and iron line emission

Details EXOSAT observations of H2252-035 - Pulse phase and orbital phase dependent low energy absorption and iron line emission EXOSAT observations of H2252-035 - Pulse phase and orbital phase dependent low energy absorption and iron line emission

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ap%26ss.130..281p&link_type=abstract

(IAU, DFG, and Bayerisches Staatsministerium für Unterricht und Kultus, Colloquium on Cataclysmic Variables, Recent Multi-Freque

Astronomy and Astrophysics

Astrophysics

11

Exosat Satellite, Light Curve, Stellar Spectra, White Dwarf Stars, X Ray Binaries, Absorption Spectra, Emission Spectra, Iron

Scientific paper

The 805 sec pulsing X-ray source H 2252-035 has been observed for 7 h on September 14/15 and on September 17, 1983 in X-rays with the low energy telescope and the medium energy detectors of EXOSAT. While below 2 keV the semiamplitude of the 805 s pulses is ≡100%, in the 2.3-7.9 keV band it is only ≡40%. X-ray dips that are more pronounced in low energies occur simultaneously with the orbital minimum of the optical light curve. The medium energy spectra during dips, with respect to the non-dip spectrum, can be explained as being just enhanced cold gas absorption of an additional absorbing column of 2×1022 cm-2. Model spectra for the 805 s minimum have to include a strong iron emission line at 6.55 keV with an equivalent width of 3 keV in addition to a reduced continuum intensity and enhanced low energy absorption.

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