کد مقاله | کد نشریه | سال انتشار | مقاله انگلیسی | نسخه تمام متن |
---|---|---|---|---|
1778966 | 1523744 | 2015 | 11 صفحه PDF | دانلود رایگان |
عنوان انگلیسی مقاله ISI
Multiwavelength modeling the SED of supersoft X-ray sources III. RS Ophiuchi: The supersoft X-ray phase and beyond
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کلمات کلیدی
موضوعات مرتبط
مهندسی و علوم پایه
فیزیک و نجوم
نجوم و فیزیک نجومی
پیش نمایش صفحه اول مقاله
چکیده انگلیسی
I modeled the 14Â Ã
-37 μm 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 (Rdisk>10 Râ). 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)Ã10-4(d/1.6kpc)5/2 Mâ. The helium ash, deposited on the WD surface during the whole burning period, was around of 8Ã10-6(d/1.6kpc)2 Mâ, which yields an average growing rate of the WD mass, MÌWDâ¼4Ã10-7(d/1.6kpc)2 Mâyr-1. The mass accreted by the WD between outbursts, maccâ¼1.26Ã10-5 Mâ, constrains the average accretion rate, MÌaccâ¼6.3Ã10-7 Mâyr-1. During quiescence, the accretion rate from the model SED of â¼2.3Ã10-7 Mâyr-1 requires a super-Eddington accretion from the disk at â¼3.6Ã10-5 Mâyr-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 Ã10-7 Mâyr-1. Then the next explosion can occur even prior to 2027.
ناشر
Database: Elsevier - ScienceDirect (ساینس دایرکت)
Journal: New Astronomy - Volume 34, January 2015, Pages 123-133
Journal: New Astronomy - Volume 34, January 2015, Pages 123-133
نویسندگان
A. Skopal,