EDP Sciences
Free access
Volume 405, Number 2, July II 2003
Page(s) 703 - 710
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20030602

A&A 405, 703-710 (2003)
DOI: 10.1051/0004-6361:20030602

XMM-Newton observations of Nova LMC 2000

J. Greiner1, M. Orio2, 3 and N. Schartel4

1  Max-Planck-Institut für extraterrestrische Physik, 85741 Garching, Germany
2  INAF - National Institute for Astrophysics, Osservatorio Astronomico di Torino, Strada Osservatorio 20, 10025 Pino Torinese, Italy
3  Department of Astronomy, 475 N. Charter Str., Madison WI 53706, USA
4  XMM-Newton Science Operations Centre, ESA, Villafranca del Castillo, PO Box 50727, 28080 Madrid, Spain

(Received 28 February 2003 / Accepted 18 April 2003 )

We report on three X-ray observations of Nova LMC 2000 with XMM-Newton at 17, 51 and 294 days after the maximum, respectively. X-ray spectral fits show a concordant decrease of the absorbing column and the X-ray luminosity. No supersoft X-ray emission is detected. The mass of the ejected shell is determined to be (less than) $7.5 \times 10^{-5}$  $M _{\odot}$. Though data are sparse, one interesting correlation becomes visible: sources with a long-duration supersoft X-ray phase have shorter orbital periods than those with short or no supersoft X-ray phase. This can be understood considering that (i) enough matter has to be accreted in order to ignite the H burning, and (ii) that H burning ceases when the mass of the remaining material (after shell ejection and burning) drops below a certain limit under which the temperature at the bottom of the envelope is too low for the shell burning to compensate the energy loss from the surface.

Key words: stars: individual: N LMC 2000 -- stars: mass-loss -- stars: novae, cataclysmic variables -- X rays: stars -- stars: binaries: close

Offprint request: J. Greiner, jcg@mpe.mpg.de

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