Modeling the classical nova outburst. I - Exploring the physics of a new mechanism
Modeling the classical nova outburst. I - Exploring the physics of a new mechanism
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模拟经典的新星爆发。
DOI：
10.1086/167452
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发表时间：
1989
期刊：
影响因子：
--
通讯作者：
W. Sparks
中科院分区：
文献类型：
--
作者：
G. Kutter;W. Sparks
进行模型计算是为了描述在 1 个太阳质量或更少的白矮星上产生经典新星爆发的机制，吸积率为 4 x 10 至 -10 个太阳质量/年或更大，即与新星系统观测数据相对应的参数。计算表明，有四个因素可以引发足够强度的核失控，以每秒几百到几千公里的速度喷射出约 0.0001 个太阳质量，正如在经典新星中观察到的那样。这些是（1）吸积阶段恒星包层中角动量存储的影响； （2）在早期核失控阶段，通过角动量的向内传输，恒星外层的离心力减少； (3) 失控阶段核燃烧峰值区通过对流引起的剪切不稳定性向内移动； (4)原始CO恒星物质和富含H的物质的混合，也是通过对流引起的剪切不稳定性。 58 参考文献
Model calculations were performed to describe a mechanism that produces classical nova outbursts on white dwarfs of 1 solar mass or less and for accretion rates of 4 x 10 to the -10th solar mass/yr or greater, i.e., the parameters corresponding to observed data of nova systems. Calculations point to four factors that can induce nuclear runaways of sufficient strength to eject about 0.0001 solar mass at speeds of several hundred to a few thousand km per second, as is observed in classical novae. These are (1) the effects of storage of angular momentum in the star's envelope during the accretion phase; (2) the reduction of centrifugal forces in the star's outer layers during the early nuclear runaway phase, through the inward transport of angular momentum; (3) the inward movement of the zone of peak nuclear burning through the convectively induced shear instability during the runaway phase; and (4) the mixing of original CO stellar matter and H-rich matter, also through the convectively induced shear instability. 58 refs.