Effects of radiative transfer on the structure of self-gravitating discs, their fragmentation and the evolution of the fragments
Effects of radiative transfer on the structure of self-gravitating discs, their fragmentation and the evolution of the fragments
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DOI：
10.1093/mnras/stu2160
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发表时间：
2014-04
影响因子：
4.8
通讯作者：
Y. Tsukamoto;Sanemichi Z. Takahashi;M. Machida;S. Inutsuka
中科院分区：
文献类型：
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作者：
Y. Tsukamoto;Sanemichi Z. Takahashi;M. Machida;S. Inutsuka
我们调查结构的自引力盘，他们的碎片和演变的碎片（团块）使用解析方法和三维辐射流体力学模拟从分子核心。模拟结果表明，非局域辐射传输决定了盘的温度。我们发现具有径向辐射传输的准稳态自引力盘的解析模型能很好地描述盘的结构。由于辐射过程不是局部的，来自星际介质的辐射不能被忽略，因此局部的辐射冷却不会与低质量星星周围的大质量圆盘中的粘性加热平衡。在我们的模拟中，有一些情况下，即使磁盘满足基于磁盘冷却时间（Q1和tcool1）的碎片标准，磁盘也不会碎片化。这表明，至少该标准不是碎裂的充分条件。我们确定发生磁盘碎片的主机云核心的参数范围。此外，我们还发现，团簇中心的温度演化接近于典型的第一核，团簇的最小初始质量约为几个木星质量。
We investigate structure of self-gravitating disks, their fragmentation and evolution of the fragments (the clumps) using both analytic approach and three-dimensional radiation hydrodynamics simulations starting from molecular cores. The simulations show that non-local radiative transfer determines disk temperature. We find the disk structure is well described by an analytical model of quasi-steady self-gravitating disk with radial radiative transfer. Because the radiative process is not local and radiation from the interstellar medium cannot be ignored, the local radiative cooling would not be balanced with the viscous heating in a massive disk around a low mass star. In our simulations, there are cases in which the disk does not fragment even though it satisfies the fragmentation criterion based on disk cooling time (Q � 1 and tcool � 1). This indicates that at least the criterion is not sufficient condition for fragmentation. We determine the parameter range for the host cloud core in which disk fragmentation occurs. In addition, we show that the temperature evolution of the center of the clump is close to that of typical first cores and the minimum initial mass of clumps to be about a few Jupiter mass.