Dissipation of Magnetic Flux in Primordial Gas Clouds
Dissipation of Magnetic Flux in Primordial Gas Clouds
复制标题
原始气体云中磁通量的耗散
DOI：
10.1086/421103
复制
发表时间：
2004
期刊：
影响因子：
--
通讯作者：
H. Susa
中科院分区：
文献类型：
--
作者：
H. Maki;H. Susa
我们报告了星族III星周围吸积盘的种子磁通量的强度。吸积盘中的磁场可能在角动量输运中起重要作用，这是由于磁旋不稳定性（MRI）引起的湍流。另一方面，由于原始的恒星形成云不包含重元素或颗粒，它们在引力收缩过程中经历的热历史和磁场耗散历史与现在的恒星形成分子云非常不同。为了评估III族恒星吸积盘中的磁场强度，我们计算了原始坍缩云的热历史，并研究了磁场与原始气体的耦合。结果表明，在整个坍缩过程中，磁场与原始气体云存在强耦合，即只要初始场强满足B > 10-5(NH/103 cm-3)0.55 G，磁场就被冻结在气体中。
We report on the strength of the seed magnetic flux of the accretion disk surrounding Population III stars. Themagnetic field in accretion disks might play an important role in the transport of angular momentum because of the turbulence induced by magnetorotational instability (MRI). On the other hand, since the primordial star-forming clouds contain no heavy elements or grains, they experience a very different thermal history and magnetic-field-dissipation history in the course of their gravitational contraction from those in the present-day star-forming molecular clouds. In order to assess the magnetic field strength in the accretion disk of Population III stars, we calculate the thermal history of the primordial collapsing clouds and investigate the coupling of the magnetic field with the primordial gas. As a result, we find that the magnetic field strongly couples with the primordial gas cloud throughout the collapse, i.e., the magnetic field is frozen to the gas, as long as the initial field strength satisfies B ≲ 10-5(NH/103 cm-3)0.55 G.
影响因子：
3.2
作者：
V. Mannings;A. Boss;S. Russell
通讯作者：
V. Mannings;A. Boss;S. Russell