Dissipation of Magnetic Flux in Primordial Star Formation: From Run-away Phase to Mass-Accretion Phase
Dissipation of Magnetic Flux in Primordial Star Formation: From Run-away Phase to Mass-Accretion Phase
复制标题
原始恒星形成过程中的磁通量耗散：从逃逸阶段到质量吸积阶段
DOI：
10.1093/pasj/59.4.787
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发表时间：
2007
影响因子：
2.3
通讯作者：
H. Susa
中科院分区：
文献类型：
--
作者：
H. Susa
我们研究了原始恒星形成云在整个塌缩过程中磁通量的耗散，包括失控塌缩阶段和吸积阶段。我们求解塌缩气体中的能量方程和非平衡化学反应，以获得塌缩过程中电离部分的径向分布。结果，我们发现电离分数足够高，足以使磁场在整个云的演化过程中与气体耦合。这一结果表明，在 Langer、Puget 和 Aghanim (2003, Phys. Rev. D67, 43505) 提出的宇宙种子磁通量存在的情况下，原恒星的射流形成以及吸积盘中磁旋转不稳定性的激活是可能的。
We investigat et he dissipation of magnetic flux in primordial star-forming clouds throughout their collapse, including the run-away collapse phase as well as the accretion phase. We solve the energy equation and the non-equilibrium chemical reactions in th ec ollapsing gas, in order to obtain the radial distribution of the ionized fraction during the collapse. As a result, we find that the ionized fraction is high enough for the magnetic field to couple with the gas throughout evolution of the cloud. This result suggests that the jet formation from protostars as well as the activation of magneto–rotational instability in the accretion disk are enabled in the presence of the cosmological seed magnetic flux proposed by Langer, Puget, and Aghanim (2003, Phys. Rev. D67, 43505).