Rapid High-Energy Emission Variability in Relativistic Pair Plasma Reconnection

被引：1

作者：

Cerutti, B. ^{[1
]}

Werner, G. R. ^{[1
]}

Uzdensky, D. A. ^{[1
]}

Begelman, M. C. ^{[2
,3
]}

机构：

[1] Univ Colorado, Dept Phys, Ctr Integrated Plasma Studies, UCB 390, Boulder, CO 80309 USA

[2] Univ Colorado, Natl Inst Stand & Technol, JILA, UCB 440, Boulder, CO 80309 USA

[3] Univ Colorado, Dept Astrophys & Planetary Sci, UCB 391, Boulder, CO 80309 USA

来源：

HIGH ENERGY GAMMA-RAY ASTRONOMY | 2012年 / 1505卷

基金：

美国国家科学基金会;

关键词：

acceleration of particles; galaxies: active; Crab Nebula; magnetic reconnection; radiation mechanisms: non-thermal; GAMMA-RAY FLARES; CRAB-NEBULA; ACCELERATION; WIND;

D O I：

10.1063/1.4772339

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on the first study of energetic particles and radiation angular distributions generated in relativistic collisionless pair plasma reconnection, using 2.5-dimensional particle-in-cell simulations. We have discovered that the energetic particles are focused within a small solid angle, and bunched into compact regions inside magnetic islands. In addition, we find that the synchrotron radiation emitted by these particles, as seen by an external observer, is tightly beamed and variable on time scales much shorter than the light-crossing time of the system. This energy dependent "kinetic beaming" differs fundamentally from the achromatic Doppler beaming usually ascribed to relativistic jets. Our findings can account for the puzzling discoveries of bright, short flares seen in high-energy gamma rays, especially from the Crab Nebula and from blazars.

引用

页码：631 / 634

页数：4

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