An ASCA observation of the eclipsing dwarf nova HT CAS

Details An ASCA observation of the eclipsing dwarf nova HT CAS An ASCA observation of the eclipsing dwarf nova HT CAS

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.2114m&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #21.14; Bulletin of the American Astronomical Society, Vol. 26, p.1345

Astronomy and Astrophysics

Astronomy

Scientific paper

In a dwarf nova in outburst, the central white dwarf is believed to accrete material via an accretion disk which extends down to the white dwarf surface, via a boundary layer. In quiescence, accretion via the boundary layer may continue at a lower rate; in addition, a recent theory predicts the presence of a hot, extended corona which may be partially responsible for the hard (2--10 keV) X-rays observed in quiescent dwarf novae. The most direct way to distinguish between a compact boundary layer and an extended corona is the observations of hard X-ray eclipses: the former will produce a narrow, deep eclipse while the latter will result in a wide, partial one. We have selected HT Cas as our target for this experiment, because this it the brightest known hard X-ray source among eclipsing dwarf novae. Our previous attempt using the ROSAT satellite was only partially successful, as the system was found in an unusual low state and only 2 eclipses were successfully observed under favorable conditions. Here we present the preliminary results from our ASCA observation of HT Cas, obtained on 1994 Sep 6/7 UT, when the system was in normal quiescence.

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