TeV Gamma-rays from the Northern Sky Pulsar Wind Nebulae

Abstract

We estimate the TeV gamma-ray fluxes expected from the population of young pulsars in terms of the self-consistent time dependent hadronic-leptonic model for the high energy processes inside the pulsar wind nebulae. This radiation model bases on the hypothesis of Arons and collaborators who postulate that leptons are accelerated inside the nebulae as a result of resonant scattering on heavy nuclei, which in turn are accelerated in the pulsar wind region or the pulsar inner magnetosphere. Our aim is to find out which nebulae on the nortehrn hemisphere are the best candidates for detection at energies above 60 GeV and 200 GeV by the next generation of low threshold Cherenkov telescopes.

13 pages, 1 figure, J.Phys. G accepted

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Cited by in corpus (13)

• TeV Gamma-Ray Sources from a Survey of the Galactic Plane with Milagro
• Measurement of the Crab Nebula spectrum over three decades in energy with the MAGIC telescopes
• Time-dependent modeling of pulsar wind nebulae: Study on the impact of the diffusion-loss approximations
• Fermi-LAT Search for Pulsar Wind Nebulae around gamma-ray Pulsars
• Detection of Extended VHE Gamma Ray Emission from G106.3+2.7 with VERITAS
• Discovery of VHE $\gamma$-ray emission from the SNR G54.1+0.3
• Discovery of TeV gamma-ray emission from the pulsar wind nebula 3C 58 by MAGIC
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• Discovery of TeV gamma-ray emission from the pulsar wind nebula 3C 58 by MAGIC
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