Nucleonic gamma-ray production in Pulsar Wind Nebulae
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Nucleonic gamma-ray production in Pulsar Wind Nebulae
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| Id. |
21796070 |
| Titulo |
Nucleonic gamma-ray production in Pulsar Wind Nebulae |
| Autor(es) |
Horns, D.
Aharonian, F.
Hoffmann, A. I. D.
Santangelo, A.
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| Localización |
http://arxiv.org/abs/astro-ph/0609386
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| Versión |
1.0 |
| Estado |
Final
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| Descripción |
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
15-5{\it2} ($t=1.55$ kyrs) have been identified to be VHE emitting PWN
(sometimes called ``TeV Plerions''). Two more candidate ``TeV Plerions'' have
been identifed and have been reported at this conference [1]. 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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| Palabras clave |
Astrophysics
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| Tipo de recurso |
Texto Narrativo
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| Tipo de Interactividad |
Expositivo
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| Nivel de Interactividad |
muy bajo
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| Audiencia |
Estudiante
Profesor
Autor
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| Estructura |
Atomic |
| Coste |
no
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| Copyright |
sí
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| Requerimientos técnicos |
Browser: Any
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| Fecha de contribución |
27-jun-2007 |
| Contacto |
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