Nucleonic gamma-ray production in pulsar wind nebulae

被引：13

作者：

Horns, D.

Aharonian, R.

Hoffmann, A. I. D.

Santangelo, A.

机构：

[1] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany

[2] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany

来源：

ASTROPHYSICS AND SPACE SCIENCE | 2007年 / 309卷 / 1-4期

关键词：

X-rays; gamma-rays; neutrinos;

D O I：

10.1007/s10509-007-9444-5

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Observations of the inner radian of the Galactic disk at very high energy (VHE) gamma-rays have revealed at least 16 new sources. Besides shell type super-nova remnants, pulsar wind nebulae (PWN) appear to be a dominant source population in the catalogue of VHE gamma-ray sources. Except for the Crab nebula, the newly discovered PWN are resolved at VHE gamma-rays to be spatially extended (5-20 pc). Currently, at least 3 middle aged (t > 10 kyrs) PWN (Vela X, G18.0-0.7, and G313.3+0.6 in the "Kookaburra" region) and I young PWN MSH 15-52 (t = 1.55 kyrs) have been identified to be VHE emitting PWN (sometimes called "TeV Plerions"). Two more candidate "TeV Plerions" have. been identified and have been reported at this conference (Carrigan, These proceedings, in preparation). In this contribution, the gamma-ray emission from Vela X is explained by a nucleonic component in the pulsar wind. The measured broad band spectral energy distribution is compared with the expected X-ray emission from primary and secondary electrons. The observed X-ray emission and TeV emission from the three middle aged PWN are compared with each other.

引用

页码：189 / 195

页数：7

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