Ia型超新星前身星吸积和慢燃过程中的内部剪切
The Internal Shear of Type Ia Supernova Progenitors During Accretion and Simmering
摘要：
一颗白矮星（WD）在吸积过程中获得了相当大的角动量，使其朝着一个更大的质量增长。因此，当它作为Ia型超新星点燃时，预计它会快速旋转。热剖面和剪切剖面对于随后的火焰传播是重要的。我们强调的过程中，可能会影响WD剪切，在吸积以及在1000年的预爆炸煨。斜压不稳定性和/或小磁场的剪切增长提供了足够的扭矩，使WD在吸积过程中非常接近固体旋转。缺乏显著的剪切使得WD很难基本上超过典型的Alasekhar质量。一旦碳被点燃，一个对流区域从WD的中心扩散。这一阶段的发生与先驱体的情况无关，因此，了解WD内部在爆炸燃烧开始之前是如何准备的是非常有意义的。我们总结了对流区域的一些关键特性，其中包括证明在任何给定时间由对流包围的质量最敏感地取决于一个单一的参数，该参数可以表示为对流区的顶部和底部的温度或密度的比率。在低Rossby数的对流角动量的重新分配可能会导致显着的剪切在对流/非对流边界。
英文摘要：
A white dwarf (WD) gains substantial angular momentum during the accretion process that grows it toward a Chandrasekhar mass. It is therefore expected to be quickly rotating when it ignites as a Type Ia supernova. The thermal and shearing profile are important for subsequent flame propagation. We highlight processes that could affect the WD shear, during accretion as well as during the ~1000 years of pre-explosive simmering. Baroclinic instabilities and/or the shear growth of small magnetic fields provide sufficient torque to bring the WD very close to solid body rotation during accretion. The lack of significant shear makes it difficult to grow a WD substantially past the typical Chandrasekhar mass. Once carbon ignites, a convective region spreads from the WD's center. This phase occurs regardless of progenitor scenario, and therefore it is of great interest for understanding how the WD interior is prepared before the explosive burning begins. We summarize some of the key properties of the convective region, which includes demonstrating that the mass enclosed by convection at any given time depends most sensitively on a single parameter that can be expressed as either the ratio of temperatures or densities at the top and bottom of the convection zone. At low Rossby numbers the redistribution of angular momentum by convection may result in significant shearing at the convective/non-convective boundary.
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