Neutron viscosity in accretion disks
Neutron viscosity in accretion disks
复制标题
吸积盘中的中子粘度
DOI：
10.1086/169005
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发表时间：
1990
期刊：
影响因子：
--
通讯作者：
D. Kazanas
中科院分区：
文献类型：
--
作者：
N. Guessoum;D. Kazanas
中子粘滞性是致密天体周围吸积盘内部动能耗散为光度的一种可能机制。简化模型的自洽，稳态吸积流中的粘度提供中子碰撞吸积离子。离子温度是通过平衡粘性耗散对离子的加热与电子库仑碰撞对离子的冷却来确定的，从而在中子产生及其对能量耗散的影响之间提供自洽的解决方案。结果表明，中子确实可以提供必要的耗散，以维持物质的稳态吸积率约为10的-8太阳质量/年或更少，电子温度约为100 keV-1 MeV。因此，中子提出了一个有前途的方式来模拟明亮的银河系X射线源。参考文献18篇。
Neutron viscosity is investigated as a possible mechanism for the dissipation of kinetic energy into luminosity in the innermost parts of accretion disks around compact objects. Simplified models are presented of the self-consistent, steady-state accretion flows in which viscosity is provided by neutron collisions with accreting ions. Ion temperatures are determined by balancing the heating of ions by viscous dissipation to their cooling by Coulomb collisions with the electrons, providing a self-consistent solution between neutron production and their impact on energy dissipation. The results indicate that neutrons can indeed provide the necessary dissipation to sustain the steady-state accretion of matter at rates of about 10 to the -8th solar mass/yr or less, and electron temperatures of about 100 keV-1 MeV. Neutrons thus present a promising way of modeling bright Galactic X-ray sources. 18 refs.