Star Formation and the Hall Effect
Star Formation and the Hall Effect
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DOI：
10.1023/b:astr.0000045033.80068.1f
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发表时间：
2011-10
期刊：
影响因子：
--
通讯作者：
C. Braiding
中科院分区：
文献类型：
--
作者：
C. Braiding
分子云和原恒星盘中磁通冻结的破裂通常近似于低密度时的双极扩散或高密度时的电阻扩散。在这里，讨论了一个中间制度，其中的霍尔项的电导率张量是显着的，和矢量的磁场的演变，因此，正在考虑的系统的演变是显着改变。在分子云和原恒星盘的致密气体中的带电粒子丰度的计算表明，霍尔扩散是非常重要的，在一个令人惊讶的广泛的条件。
The breakdown of flux-freezing in molecular clouds and protostellar discs is usually approximated by ambipolar diffusion at low densities or by resistive diffusion at high densities. Here an intermediate regime is discussed in which the Hall term in the conductivity tensor is significant, and the vector evolution of the magnetic field, and therefore the evolution of the system under consideration is dramatically altered. Calculations of charged particle abundances in dense gas in molecular clouds and protostellar discs demonstrate that Hall diffusion is important over a surprisingly broad range of conditions.