Multiwavelength modeling the SED of supersoft X-ray sources III. RS Ophiuchi: The supersoft X-ray phase and beyond (Reprinted from New Astronomy, vol 34, pg 123-133, 2015)

摘要

I modeled the 14 angstrom-37 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-Edding-ton 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 > 10R circle dot). The super-Eddington luminosity of the burning WD during the SSS phase was independently justified by the high quantity of the nebular emission. The emitting material surrounded the burning WD, and its mass was (1.6 +/- 0.5) x 10(-4)(d/1.6 kpc)(5/2) M circle dot. The helium ash, deposited on the WD surface during the whole burning period, was around of 8 x 10(-6)(d/1.6 kpc)(2) M circle dot, which yields an average growing rate of the WD mass, M-WD similar to 4 x 10(-7)(d/1.6 kpc)M-2 circle dot yr(-1). The mass accreted by the WD between outbursts, macc 1.26 x 10(-5)M circle dot, constrains the average accretion rate, M-acc 6.3 x 10(-7)M circle dot yr(-1). During quiescence, the accretion rate from the model SED of 2.3 x 10(-7)M circle dot yr(-1) requires a super-Eddington accretion from the disk at 3.6 x 10(-5)M circle dot yr(-1) during the outburst. Such a high accretion can be responsible for the super-Eddington luminosity during the whole burning phase. Simultaneous presence of jets supports this scenario. 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 x10-7M0 yr-1. Then the next explosion can occur even prior to 2027. (c) 2014 Elsevier B.V. All rights reserved.