LINEAR GROWTH OF THE KELVIN-HELMHOLTZ INSTABILITY WITH AN ADIABATIC COSMIC-RAY GAS

被引：6
作者：
Suzuki, Akihiro [1 ]
Takahashi, Hiroyuki R. [1 ]
Kudoh, Takahiro [2 ,3 ]
机构：
[1] Natl Astron Observ Japan, Ctr Computat Astrophys, Mitaka, Tokyo 1818588, Japan
[2] Natl Astron Observ Japan, Div Theoret Astron, Mitaka, Tokyo 1818588, Japan
[3] Grad Univ Adv Studies SOKENDAI, Sch Phys Sci, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan
来源：
ASTROPHYSICAL JOURNAL | 2014年 / 787卷 / 02期
关键词：
cosmic rays; instabilities; magnetic fields; magnetohydrodynamics (MHD); WEAKLY MAGNETIZED DISKS; LOCAL SHEAR INSTABILITY; MAGNETOHYDRODYNAMIC SIMULATIONS; MAGNETOROTATIONAL-INSTABILITY; THERMAL-INSTABILITY; PARKER INSTABILITY; ACCRETION DISKS; GALACTIC WINDS; COLD FRONTS; DRIVEN;
D O I：
10.1088/0004-637X/787/2/169
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We investigate effects of cosmic rays on the linear growth of the Kelvin-Helmholtz instability. Cosmic rays are treated as an adiabatic gas and allowed to diffuse along magnetic field lines. We calculated the dispersion relation of the instability for various sets of two free parameters, the ratio of the cosmic-ray pressure to the thermal gas pressure, and the diffusion coefficient. Including cosmic-ray effects, a shear layer is more destabilized and the growth rates can be enhanced in comparison with the ideal magnetohydrodynamical case. Whether the growth rate is effectively enhanced or not depends on the diffusion coefficient of cosmic rays. We obtain the criterion for effective enhancement by comparing the growing timescale of the instability with the diffusion timescale of cosmic rays. These results can be applied to various astrophysical phenomena where a velocity shear is present, such as outflows from star-forming galaxies, active galactic nucleus jet, channel flows resulting from the nonlinear development of the magnetorotational instability, and galactic disks.
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页数：11
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