Gamma-rays from the pulsar wind nebulae
arXiv:astro-ph/0304049 · doi:10.1051/0004-6361:20030593
Abstract
We investigate the radiation processes inside supernova remnants which are powered by young pulsars. Using recent model for particle acceleration by the pulsar wind nebulae, we obtain the equilibrium spectra of leptons and nuclei inside the nebula as a function of time. We calculate the multiwavelength photon spectra produced by leptons and nuclei and compare them with the observations of the PWNe, i.e. the Crab Nebula, the Vela Supernova Remnant, and the nebula around PSR 1706-44. It is found that the emission from the Crab Nebula can be well fitted by the composition of the gamma-ray emission produced by leptons and nuclei. The model is further tested by successful fitting of the high energy spectrum from the Vela SNR. However, considered model does not give good fitting to the emission from PSR1706-44, for the likely parameters of this source, unless additional target for relativistic leptons is present inside the nebula, e.g. the thermal infrared emission. Based on the knowledge obtained from these fittings, we predict the gamma-ray fluxes in the TeV energy range from other PWNe, i.e. MSH15-52 (PSR 1509-58), 3C58 (PSR J0205+6449), and CTB80 (PSR 1951+32).
15 pages, 11 figures, A&A style, will be published in A&A
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Cited by in corpus (46)
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