RADIATIVE DAMPING AND EMISSION SIGNATURES OF STRONG SUPERLUMINAL WAVES IN PULSAR WINDS

被引：15

作者：

Mochol, Iwona ^{[1
]}

Kirk, John G. ^{[1
]}

机构：

[1] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany

来源：

ASTROPHYSICAL JOURNAL | 2013年 / 776卷 / 01期

关键词：

plasmas; pulsars: general; pulsars: individual (PSR B1259-63); radiation mechanisms: non-thermal; stars:; winds; outflows; waves; PSR B1259-63/LS 2883; GAMMA-RAY BINARIES; INVERSE COMPTON-SCATTERING; TERMINATION SHOCK; SIGMA-PROBLEM; CRAB PULSAR; PERIASTRON; DISCOVERY; SYSTEM; ACCELERATION;

D O I：

10.1088/0004-637X/776/1/40

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We analyze the damping of strong, superluminal electromagnetic waves by radiation reaction and Compton drag in the context of pulsar winds. The associated radiation signature is found by estimating the efficiency and the characteristic radiation frequencies. Applying these estimates to the gamma-ray binary containing PSR B1259-63, we show that the GeV flare observed by the Fermi Large Area Telescope can be understood as inverse-Compton emission by particles scattering photons from the companion star, if the pulsar wind termination shock acquires a precursor of superluminal waves roughly 30 days after periastron. This requirement constrains the mass-loading factor of the wind mu = L/(N) over dotmc(2), where L is the luminosity and (N) over dot is the rate of loss of electrons and positrons, to be roughly 6 x 10(4).

引用

页数：6

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