Nucleonic gamma-ray production in pulsar wind nebulae |
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| Authors: | D Horns F Aharonian A I D Hoffmann A Santangelo |
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| Institution: | (1) Institute for Astronomy and Astrophysics, Karl-Eberhards University Tübingen, Sand 1, 72076 Tübingen, Germany;(2) Max-Planck-Institut f. Kernphysik Heidelberg, P.O. Box 10 39 80, 69117 Heidelberg, Germany |
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| Abstract: | 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 1 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. |
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| Keywords: | X-rays Gamma-rays Neutrinos |
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