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V5116 Sagittarii, an Eclipsing Supersoft Postoutburst Nova?

V5116 Sagittarii, an Eclipsing Supersoft Postoutburst Nova?

Publication date: 10 March 2008

Authors: Sala, G. et al.

Journal: ApJ.
Volume: 675
Issue: 2
Page: L93-L96
Year: 2008

Copyright: AAS

V5116 Sgr (Nova Sgr 2005 No. 2), discovered on 2005 July 4, was observed with XMM-Newton in 2007 March, 20 months after the optical outburst. The X-ray spectrum shows that the nova had evolved to a pure supersoft X-ray source, with no significant emission at energies above 1 keV. The X-ray light curve shows abrupt decreases and increases of the flux by a factor ~8. It is consistent with a periodicity of 2.97 hr, the orbital period suggested by Dobrotka and coworkers, although the observation lasted just a little more than a whole period. We estimate the distance to V5116 Sgr to be 11±3 kpc. A simple blackbody model does not fit correctly the EPIC spectra, with Chi²>4. In contrast, ONe-rich white dwarf atmosphere models provide a good fit, with NH=(1.3±0.1)x1021 cm-2, T=(6.1±0.1)x105 K, and L=(3.9±0.8)x1037 (D/10 kpc)² erg s-1 (during the high-flux periods). This is consistent with residual hydrogen burning in the white dwarf envelope. The white dwarf atmosphere temperature is the same both in the low- and the high-flux periods, ruling out an intrinsic variation of the X-ray source as the origin of the flux changes. We speculate that the X-ray light curve may result from a partial coverage by an asymmetric accretion disk in a high-inclination system.

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