The X-ray eclipse of the dwarf nova HT Cassiopeiae observed by the XMM-Newton satellite: spectral and timing analysis
1
XMM-Newton Science Operations Centre, ESAC, ESA, PO Box 78, 28691 Villanueva de la , Madrid, Spain e-mail: anucita@sciops.esa.int
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
Received:
2
December
2008
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