Turbulent Model of Crab Nebula Radiation

被引：16

作者：

Luo, Yonggang ^{[1
]}

Lyutikov, Maxim ^{[1
]}

Temim, Tea ^{[2
]}

Comisso, Luca ^{[3
]}

机构：

[1] Purdue Univ, Dept Phys & Astron, 525 Northwestern Ave, W Lafayette, IN 47907 USA

[2] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[3] Columbia Univ, Dept Astron, 550 W 120th St, New York, NY 10027 USA

来源：

ASTROPHYSICAL JOURNAL | 2020年 / 896卷 / 02期

关键词：

Rotation powered pulsars; Stellar wind bubbles; Interstellar synchrotron emission; PULSAR-WIND NEBULAE; GAMMA-RAY FLARES; RELATIVISTIC MAGNETIC RECONNECTION; PARTICLE-ACCELERATION; X-RAY; MAGNETOHYDRODYNAMIC SIMULATIONS; SUPERNOVA-REMNANTS; COMPTON-SCATTERING; POLAR CAPS; RADIO;

D O I：

10.3847/1538-4357/ab93c0

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We construct a turbulent model of the Crab Nebula's nonthermal emission. The present model resolves a number of long-standing problems of the Kennel-Coroniti model: (i) the sigma problem, (ii) the hard spectrum of radio electrons, (iii) the high peak energy of gamma-ray flares, (iv) and the spatial evolution of the infrared (IR) emission. The Nebula contains two populations of injected particles: Component-I, accelerated at the wind termination shock via the Fermi-I mechanism; and Component-II, accelerated in reconnecting turbulence in highly magnetized (sigma >> 1) plasma in the central part of the Crab Nebula. The reconnecting turbulence in Component-II extends from radio to gamma-rays: it accelerates radio electrons with a hard spectrum, destroys the large-scale magnetic flux (and thus resolves the sigma problem), and occasionally produces gamma-ray flares (from the largest-scale reconnection events). The model reproduces the broadband spectrum of the Crab Nebula, from low-frequency synchrotron emission in radio to inverse-Compton emission at TeV energies, as well as the spatially resolved evolution of the spectral indices in the IR and optical bands.

引用

页数：13

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