EVOLUTION OF BLISTER-TYPE H ii REGIONS IN A MAGNETIZED MEDIUM
EVOLUTION OF BLISTER-TYPE H ii REGIONS IN A MAGNETIZED MEDIUM
复制标题
磁化介质中泡罩型 H ii 区域的演变
DOI：
10.1088/0004-637x/745/2/158
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发表时间：
2011
期刊：
影响因子：
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通讯作者：
M. Krumholz
中科院分区：
文献类型：
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作者：
Leo Gendelev;M. Krumholz
我们使用三维 Athena 电离辐射磁流体动力学代码来模拟磁化气体云边缘由恒星驱动的泡罩型 H ii 区域。我们将这些与恒星嵌入云深处的球形 H ii 区域的模拟以及这两种类型的非磁化模拟进行比较，以比较它们驱动湍流和影响恒星形成的能力。我们发现磁化泡状 H ii 区域可以非常有效地将能量注入云中。这部分是一种磁效应：H ii区域添加到云中的磁能与动能相当或更大，磁场还可以帮助准直喷射的气体，增加其能量产量。由于这些效应，膨胀到磁场垂直于其边缘的云中的泡罩 H ii 区域注入的能量是由相同光度恒星驱动的非磁化泡罩 H ii 区域的两倍，多 5 Myr。由于逃逸气体提供的反冲力，泡罩 H ii 区域在注入动能方面也比球形 H ii 区域更有效，但不如一些解析近似预测的那么多。
We use the three-dimensional Athena ionizing radiation-magnetohydrodynamics code to simulate blister-type H ii regions driven by stars on the edge of magnetized gas clouds. We compare these to simulations of spherical H ii regions where the star is embedded deep within a cloud, and to non-magnetized simulations of both types, in order to compare their ability to drive turbulence and influence star formation. We find that magnetized blister H ii regions can be very efficient at injecting energy into clouds. This is partly a magnetic effect: the magnetic energy added to a cloud by an H ii region is comparable to or larger than the kinetic energy, and magnetic fields can also help collimate the ejected gas, increasing its energy yield. As a result of these effects, a blister H ii region expanding into a cloud with a magnetic field perpendicular to its edge injects twice as much energy by 5 Myr as a non-magnetized blister H ii region driven by a star of the same luminosity. Blister H ii regions are also more efficient at injecting kinetic energy than spherical H ii regions, due to the recoil provided by escaping gas, but not as much as predicted by some analytic approximations.