Multiwavelength modelling the SED of supersoft X-ray sources III. RS Ophiuchi: The supersoft X-ray phase and beyond

Abstract

I modelled the 14 Å- 37 $\mu$m SED of the recurrent symbiotic nova RS Oph during its supersoft source (SSS) phase and the following quiescent phase. During the SSS phase, the model SEDs revealed the presence of a strong stellar and nebular component of radiation in the spectrum. The former was emitted by the burning WD at highly super-Eddington rate, while the latter represented a fraction of its radiation reprocessed by the thermal nebula. During the transition phase, both the components were decreasing and during quiescence the SED satisfied radiation produced by a large, optically thick disk (R(disk) > 10 R(Sun)). The mass of the emitting material was (1.6 +/- 0.5) x 1E-4(d/1.6 kpc)**(5/2) M(Sun). The helium ash, deposited on the WD surface during the whole burning period, was around of 8 x 1E-6(d/1.6kpc)**2 M(Sun), which yields an average growing rate of the WD mass, dM(WD)/dt ~ 4 x 1E-7(d/1.6 kpc)**2 M(Sun)/yr. The mass accreted by the WD between outbursts, m(acc) ~ 1.26 x 1E-5 M(Sun), constrains the average accretion rate, dM(acc)/dt ~ 6.3 x 1E-7 M(Sun)/yr. If the wind from the giant is not sufficient to feed the WD at the required rate, the accretion can be realized from the disk-like reservoir of material around the WD. In this case the time between outbursts will extend, with the next explosion beyond 2027. In the opposite case, the wind from the giant has to be focused to the orbital plane to sustain the high accretion rate at a few times 1E-7 M(Sun)/yr. Then the next explosion can occur even prior to 2027.

14 pages, 6 figures, 2 tables, accepted by New Astron. on May 20, 2014; follow-up of arXiv:1402.6126

References in corpus (15)

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• Resumption of mass accretion in RS Oph
• On the effect of emission lines on the UBVR photometry
• Transient jets in the symbiotic prototype Z Andromedae
• Double radio peak and non-thermal collimated ejecta in RS Ophiuchi following the 2006 outburst
• Spitzer and ground-based infrared observations of the 2006 eruption of RS Ophiuchi

Cited by in corpus (5)

• A census of symbiotic stars in the 2MASS, WISE and Gaia surveys
• Optical Flickering of the recurrent nova RS Ophiuchi: amplitude - flux relation
• Multiwavelength modeling the SED of nova V339~Del: Stopping the wind and long-lasting super-Eddington luminosity with dust emission
• Rise and fall of silicate dust in RS Ophiuchi following the 2006 eruption
• The applicability of the wind compression model