RADIATION MAGNETOHYDRODYNAMICS SIMULATION OF PROTO-STELLAR COLLAPSE: TWO-COMPONENT MOLECULAR OUTFLOW
RADIATION MAGNETOHYDRODYNAMICS SIMULATION OF PROTO-STELLAR COLLAPSE: TWO-COMPONENT MOLECULAR OUTFLOW
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DOI：
10.1088/2041-8205/714/1/l58
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发表时间：
2010-01
期刊：
影响因子：
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通讯作者：
K. Tomida;K. Tomisaka;Tomoaki Matsumoto;K. Ohsuga;M. Machida;K. Saigo
中科院分区：
文献类型：
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作者：
K. Tomida;K. Tomisaka;Tomoaki Matsumoto;K. Ohsuga;M. Machida;K. Saigo
我们利用自重力进行了三维嵌套网格辐射磁流体动力学（RMHD）模拟，以研究低质量恒星形成过程的早期阶段，即在第二次坍缩开始之前，从旋转分子云核心到第一个绝热核心。辐射传输是通过通量限制扩散近似、算子分裂和隐式时间积分器来实现的。在 RMHD 模拟中，第一核心的外部区域获得了更高的熵，并且其尺寸比采用正压近似的磁流体动力学模拟中的更大。由两部分组成的双极分子流出物由磁洛伦兹力通过不同的机制驱动，并且观察到流出物的冲击加热。使用 RMHD 模拟，我们可以预测和解释使用毫米/亚毫米射电干涉仪（尤其是阿塔卡马大型毫米/亚毫米阵列）观察到的恒星形成云、第一核心和流出物的特性。
We perform a three-dimensional nested-grid radiation magnetohydrodynamics (RMHD) simulation with self-gravity to study the early phase of the low-mass star formation process from a rotating molecular cloud core to a first adiabatic core just before the second collapse begins. Radiation transfer is implemented with the flux-limited diffusion approximation, operator-splitting, and implicit time integrator. In the RMHD simulation, the outer region of the first core attains a higher entropy and its size is larger than that in the magnetohydrodynamics simulations with the barotropic approximation. Bipolar molecular outflow consisting of two components is driven by magnetic Lorentz force via different mechanisms, and shock heating by the outflow is observed. Using the RMHD simulation we can predict and interpret the observed properties of star-forming clouds, first cores, and outflows with millimeter/submillimeter radio interferometers, especially the Atacama Large Millimeter/submillimeter Array.