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

摘要

I modelled the 14 \AA - 37 $\mu$m SED of the recurrent symbiotic nova RS Ophduring its supersoft source (SSS) phase and the following quiescent phase.During the SSS phase, the model SEDs revealed the presence of a strong stellarand nebular component of radiation in the spectrum. The former was emitted bythe burning WD at highly super-Eddington rate, while the latter represented afraction of its radiation reprocessed by the thermal nebula. During thetransition phase, both the components were decreasing and during quiescence theSED satisfied radiation produced by a large, optically thick disk (R(disk) > 10R(Sun)). The mass of the emitting material was (1.6 +/- 0.5) x 1E-4(d/1.6kpc)**(5/2) M(Sun). The helium ash, deposited on the WD surface during thewhole burning period, was around of 8 x 1E-6(d/1.6kpc)**2 M(Sun), which yieldsan average growing rate of the WD mass, dM(WD)/dt ~ 4 x 1E-7(d/1.6 kpc)**2M(Sun)/yr. The mass accreted by the WD between outbursts, m(acc) ~ 1.26 x 1E-5M(Sun), constrains the average accretion rate, dM(acc)/dt ~ 6.3 x 1E-7M(Sun)/yr. If the wind from the giant is not sufficient to feed the WD at therequired rate, the accretion can be realized from the disk-like reservoir ofmaterial 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 thegiant has to be focused to the orbital plane to sustain the high accretion rateat a few times 1E-7 M(Sun)/yr. Then the next explosion can occur even prior to2027.