Modelling spectral evolution of pulsar wind nebulae inside supernova remnants

被引：183

作者：

Bucciantini, N. ^{[1
,2
,3
]}

Arons, J. ^{[2
,3
,4
]}

Amato, E. ^{[5
]}

机构：

[1] AlbaNova Univ Ctr, NORDITA, SE-10691 Stockholm, Sweden

[2] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[3] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA

[4] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[5] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2011年 / 410卷 / 01期

基金：

美国国家科学基金会;

关键词：

radiation mechanisms: non-thermal; pulsars: general; stars: winds; outflows; ISM: supernova remnants; GAMMA-RAY EMISSION; RELATIVISTIC MHD SIMULATIONS; AREA TELESCOPE OBSERVATIONS; MAGNETOSONIC SHOCK-WAVES; FORMED DENSE SHELL; X-RAY; CRAB-NEBULA; MAGNETIC-FIELD; PSR B1509-58; ULTRARELATIVISTIC ELECTRONS;

D O I：

10.1111/j.1365-2966.2010.17449.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a new model for the spectral evolution of pulsar wind nebulae (PWNe) inside supernova remnants (SNRs). The model couples the long-term dynamics of these systems, as derived in the 1D approximation, with a one-zone description (all quantities are assumed uniform in the nebula) of the spectral evolution of the emitting plasma. Our goal is to provide a simplified theoretical description that can be used as a tool to put constraints on unknown properties of PWN-SNR systems: a piece of work that is preliminary to any more accurate and sophisticated modelling. In this paper, we apply the newly developed model to a few objects of different ages and luminosities. We find that an injection spectrum in the form of a broken power law gives a satisfactory description of the emission for all the systems we consider. More surprisingly, we also find that the intrinsic spectral break turns out to be at a similar energy for all sources, in spite of the differences mentioned above. We discuss the implications of our findings on the workings of pulsar magnetospheres, pair multiplicity and on the particle acceleration mechanism(s) that might be at work at the pulsar wind termination shock.

引用

页码：381 / 398

页数：18

共 133 条

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