Luminous supersoft X-ray emission from the recurrent nova U Scorpii

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dc.creatorKahabka, P.
dc.creatorHartmann, H. W.
dc.creatorParmar, A. N.
dc.creatorNegueruela, I.
dc.date1999-06-15
dc.date.accessioned2026-07-07T10:51:31Z
dc.date.available2026-07-07T10:51:31Z
dc.descriptionBeppoSAX detected luminous 0.2-2.0 keV supersoft X-ray emission from the recurrent nova U Sco ~19-20 days after the peak of the optical outburst in February 1999. U Sco is the first recurrent nova to be observed during a luminous supersoft X-ray phase. Non-LTE white dwarf atmosphere spectral models (together with a ~0.5 keV optically thin thermal component) were fitted to the BeppoSAX spectrum. We find that the fit is acceptable assuming enriched He and an enhanced N/C ratio. This implies that the CNO cycle was active during the outburst, in agreement with a thermonuclear runaway scenario. The best-fit temperature is ~9 10^5 K and the bolometric luminosity those predicted for steady nuclear burning on a WD close to the Chandrasekhar mass. The fact that U~Sco was detected as a supersoft X-ray source is consistent with steady nuclear burning continuing for at least one month after the outburst. This means that only a fraction of the previously accreted H and He was ejected during the outburst and that the WD can grow in mass, ultimately reaching the Chandrasekhar limit. This makes U~Sco a candidate type Ia supernova progenitor.
dc.description4 pages, accepted by A&A Letters 15 June 1999
dc.identifierhttps://arxiv.org/abs/astro-ph/9906245
dc.identifierhttp://arxiv.org/abs/astro-ph/9906245
dc.identifierAIPConf.Proc.599:682-685,1999
dc.identifierdoi:10.1063/1.1434716
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/184844
dc.subjectAstrophysics
dc.titleLuminous supersoft X-ray emission from the recurrent nova U Scorpii
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