How much boundary layer heating occurs in an accreting prenova white dwarf
How much boundary layer heating occurs in an accreting prenova white dwarf
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吸积的前新星白矮星发生了多少边界层加热
DOI：
10.1086/167453
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发表时间：
1989
期刊：
影响因子：
--
通讯作者：
M. Shara
中科院分区：
文献类型：
--
作者：
O. Regev;M. Shara
了解边界层加热对于确定前新星白色矮星的吸积包层的热结构至关重要。采用匹配渐近展开法，一致地求解了旋转白色矮星吸积盘的结构。计算了进入前新星白色矮星包层的吸积能量比例。这些结果应该被新星爆发的建模者所使用;它们将产生比迄今为止预期的显著更低的简并和更弱的爆炸。吸积盘和边界层的详细模型也可以用来计算矮新星爆发期间白色矮星的加热量。一般来说，这种模型可以作为大气模型代码的输入，以预测更现实的磁盘吸积物体的光谱。参考文献29篇。
Understanding boundary layer heating is crucial in determining the thermal structure of the accreted envelope of a prenova white dwarf. The matched asymptotic expansion method was used to solve consistently for the structure of accretion disks transferring matter onto rotating white dwarfs. The fraction of accretion energy transported into prenova white dwarf envelopes was calculated. These results should be used by modelers of nova eruptions; they will produce significantly lower degeneracies and weaker explosions than expected until now. Detailed models of accretion disks and boundary layers can also be used to calculate the amount of white dwarf heating during a dwarf nova outburst. In general, such models can serve as input to model atmosphere codes to predict more realistic spectra of disk-accreting objects. 29 refs.