Volume 504, Number 3, September IV 2009
|Page(s)||973 - 979|
|Section||Stellar structure and evolution|
|Published online||03 August 2009|
The X-ray eclipse of the dwarf nova HT Cassiopeiae observed by the XMM-Newton satellite: spectral and timing analysis
XMM-Newton Science Operations Centre, ESAC, ESA, PO Box 78, 28691 Villanueva de la , Madrid, Spain e-mail: email@example.com
2 Dipartimento di Fisica, Università del Salento, CP 193, 73100 Lecce, Italy
3 ESA, Research and Scientific Support Department, ESTEC, PO Box 299, 2200 AG, Noordwijk, The Netherlands
4 Integral Science Operations Centre, ESAC, ESA, PO Box 78, 28691 Villanueva de la , Madrid, Spain
5 Herschel Science Operations Centre, ESAC, ESA, PO Box 78, 28691 Villanueva de la , Madrid, Spain
6 INFN, Sezione di Lecce, via Arnesano, 73100 Lecce, Italy
Accepted: 25 June 2009
Context. A cataclysmic variable is a binary system consisting of a white dwarf that accretes material from a secondary object via the Roche-lobe mechanism. In the case of long enough observation, a detailed temporal analysis can be performed, allowing the physical properties of the binary system to be determined.
Aims. We present an XMM-Newton observation of the dwarf nova HT Cas acquired to resolve the binary system eclipses and constrain the origin of the X-rays observed. We also compare our results with previous ROSAT and ASCA data.
Methods. After the spectral analysis of the three EPIC camera signals, the observed X-ray light curve was studied with well known techniques and the eclipse contact points obtained.
Results. The X-ray spectrum can be described by thermal bremsstrahlung of temperature keV plus a black-body component (upper limit) with temperature eV. Neglecting the black-body, the bolometric absorption corrected flux is erg s-1 cm-2, which, for a distance of HT Cas of 131 pc, corresponds to a bolometric luminosity of erg s-1. In a standard accretion scenario where assuming , the amount of matter accreting onto the central white dwarf is found to be yr-1. The study of the eclipse in the EPIC light curve permits us to constrain the size and location of the X-ray emitting region, which turns out to be close to the white dwarf radius. We measure an X-ray eclipse somewhat smaller (but only at a level of ) than the corresponding optical one. If this is the case, we have possibly identified the signature of either high latitude emission or a layer of X-ray emitting material partially obscured by an accretion disk.
Key words: stars: binaries: general / stars: white dwarfs / X-rays: binaries / stars: novae, cataclysmic variables
© ESO, 2009
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