Disc instability in RS Ophiuchi: a path to Type Ia supernovae RS Oph and Type Ia SNe
Disc instability in RS Ophiuchi: a path to Type Ia supernovae RS Oph and Type Ia SNe
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RS Ophiuchi 中的盘不稳定性：通向 Ia 型超新星 RS Oph 和 Ia SNe 的路径
DOI：
10.1111/j.1365-2966.2011.19647.x
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发表时间：
2011
影响因子：
4.8
通讯作者：
Alexander R
中科院分区：
文献类型：
--
作者：
Alexander R
我们研究了周期性新星蛇夫座RS中吸积盘的稳定性。我们建立了一个一维含时的双盘系统模型，其中包括粘性加热和辐射冷却和自洽处理的双位。我们发现，在这个系统中，扩展吸积盘总是不稳定的热粘性不稳定性，并在10-20年的时间尺度上反复发生盘爆发。这是类似的复发时间尺度的RS Oph系统中观察到的爆发，但我们表明，光盘的吸积光度在爆发是不足以解释所观察到的爆发。我们探索了一系列的模型，发现在大多数情况下，在爆发的吸积率达到或超过稳定的核燃烧的白色矮星表面的临界吸积率。因此，我们认为，由盘不稳定性引发的表面核燃烧可能是观测到的爆发的原因。这使得白色矮星质量随着时间的推移而增长，我们认为RS Oph和类似系统中的圆盘不稳定性可能代表了Ia型超新星的路径。
We study the stability of disc accretion in the recurrent nova RS Ophiuchi. We construct a one-dimensional time-dependent model of the binary–disc system, which includes viscous heating and radiative cooling and a self-consistent treatment of the binary potential. We find that the extended accretion disc in this system is always unstable to the thermal–viscous instability, and undergoes repeated disc outbursts on ∼10–20 yr time-scales. This is similar to the recurrence time-scale of observed outbursts in the RS Oph system, but we show that the disc’s accretion luminosity during outburst is insufficient to explain the observed outbursts. We explore a range of models, and find that in most cases the accretion rate during outbursts reaches or exceeds the critical accretion rate for stable nuclear burning on the white dwarf surface. Consequently we suggest that a surface nuclear burning triggered by disc instability may be responsible for the observed outbursts. This allows the white dwarf mass to grow over time, and we suggest that disc instability in RS Oph and similar systems may represent a path to Type Ia supernovae.