X-Ray Spectroscopy and Photometry of the Accreting White Dwarf in AI Tri

Details X-Ray Spectroscopy and Photometry of the Accreting White Dwarf in AI Tri X-Ray Spectroscopy and Photometry of the Accreting White Dwarf in AI Tri

Sep 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..372..553t&link_type=abstract

15th European Workshop on White Dwarfs ASP Conference Series, Vol. 372, proceedings of the conference held 7-11 August, 2006 in

Astronomy and Astrophysics

Astronomy

Scientific paper

Based on recent X-ray observations with the XMM-Newton satellite, we present first results of our spectroscopic and photometric analysis of the accretion region on the white dwarf in the long-period magnetic cataclysmic variable AI Tri. Our XMM-Newton observation covers for the first time uninterruptedly a complete binary orbital period. The shape of the X-ray light curve is highly variable with strong flares, occurring mainly in the soft energy range over about 70% of the binary orbit. Weaker hard X-ray emission is visible nearly all the time. The ultraviolet light curve, obtained in the UVM2 filter at an effective wavelength of 231 nm, has a similar shape but higher amplitude than the optical and near UV light curves reported during high states of accretion. The X-ray spectrum is dominated by soft X-ray emission which can be described in good approximation by a mildly absorbed blackbody component with kTbb = 36.8+1.8-1.4 {eV} and NH = 3.08+0.51-0.42 \cdot 1020 {cm}-2. In addition, weak emission from a thermal plasma is present and iron Kα at 6.4 keV and iron L emission around 0.9 keV can be identified.

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