Relativistic Asymmetric Magnetic Reconnection

被引：11

作者：

Mbarek, Rostom ^{[1
,2
,3
]}

Haggerty, Colby ^{[1
,4
]}

Sironi, Lorenzo ^{[5
,6
]}

Shay, Michael ^{[7
]}

Caprioli, Damiano ^{[1
,3
]}

机构：

[1] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA

[2] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[3] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA

[4] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA

[5] Columbia Univ, Dept Astron, New York, NY 10027 USA

[6] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA

[7] Univ Delaware, Bartol Res Inst, Dept Phys & Astron, Newark, DE 19716 USA

来源：

PHYSICAL REVIEW LETTERS | 2022年 / 128卷 / 14期

关键词：

EARTHS MAGNETOPAUSE DEPENDENCE; INFLOW ALFVEN SPEED; PARTICLE-ACCELERATION; ELECTRON; SIMULATIONS; TURBULENCE; DYNAMICS; SPECTRA; SHOCKS; MODEL;

D O I：

10.1103/PhysRevLett.128.145101

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

We derive basic scaling equations for relativistic magnetic reconnection in the general case of asymmetric inflow conditions and obtain predictions for the outflow Lorentz factor and the reconnection rate. Kinetic particle-in-cell simulations show that the outflow speeds as well as the nonthermal spectral index are constrained by the inflowing plasma with the weaker magnetic energy per particle, in agreement with the scaling predictions. These results are significant for understanding nonthermal emission from reconnection in magnetically dominated astrophysical systems, many of which may be asymmetric in nature. The results provide a quantitative approach for including asymmetry on reconnection in the relativistic regime.

引用

页数：6

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