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Preprint 16c/04


Analysis of a XMM-Newton Spectrum of the Extremely Hot White Dwarf in Nova V4743 Sgr

T. Rauch (1,2), K. Werner (2), M. Orio (3,4)

(1) Dr.-Remeis-Sternwarte, Bamberg, University of Erlangen-Nürnberg, Germany
(2) Institute for Astronomy and Astrophysics, University of Tübingen, Germany
(3) Istituto Nazionale di Astrofisica (INAF), Osservatorio Astronomico di Torino, Italy
(4) Department of Astronomy, University of Wisconsin, Madison, USA

To be published in: X-ray Diagnostics for Astrophysical Plasmas, American Institute of Physics Conference Proceedings

Abstract. Classical novae occur in close binary systems (main-sequence star + white dwarf). V4743 Sgr is a very fast nova exhibiting a X-ray spectrum which is consistent with a view on the optically thick atmosphere of an extremely hot white dwarf (WD). It exhibits strong absorption features of the C V, C VI, N VI, N VII, and O VII resonance lines indicating an effective temperature of about 610 kK.
We present preliminary results of a spectral analysis by means of line-blanketed non-LTE atmosphere models of a XMM-Newton RGS-1 spectrum of V4743 Sgr, taken about half a year after its outburst.
 
Key words: Stars: AGB and post-AGB, Stars: atmospheres, Stars: individual: V 4743 Sgr, Stars: novae, cataclysmic variables, X-rays: stars

Preprint (72 kb PDF file including figures)


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