Gamma-Rays Produced in Cosmic-Ray Interactions and the TeV-band Spectrum of RX J1713.7-3946

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dc.creatorHuang, C. -Y.
dc.creatorPark, S. -E.
dc.creatorPohl, M.
dc.creatorDaniels, C. D.
dc.date2007-06-04
dc.date.accessioned2026-07-07T10:36:02Z
dc.date.available2026-07-07T10:36:02Z
dc.descriptionWe employ the Monte Carlo particle collision code DPMJET3.04 to determine the multiplicity spectra of various secondary particles (in addition to $π^0$'s) with $γ$'s as the final decay state, that are produced in cosmic-ray ($p$'s and $α$'s) interactions with the interstellar medium. We derive an easy-to-use $γ$-ray production matrix for cosmic rays with energies up to about 10 PeV. This $γ$-ray production matrix is applied to the GeV excess in diffuse Galactic $γ$-rays observed by EGRET, and we conclude the non-$π^0$ decay components are insufficient to explain the GeV excess, although they have contributed a different spectrum from the $π^0$-decay component. We also test the hypothesis that the TeV-band $γ$-ray emission of the shell-type SNR RX J1713.7-3946 observed with HESS is caused by hadronic cosmic rays which are accelerated by a cosmic-ray modified shock. By the $χ^2$ statistics, we find a continuously softening spectrum is strongly preferred, in contrast to expectations. A hardening spectrum has about 1% probability to explain the HESS data, but then only if a hard cutoff at 50-100 TeV is imposed on the particle spectrum.
dc.description3 pages; 4 figures; Contribution to the First GLAST Symposium, Standord, 2007
dc.identifierhttps://arxiv.org/abs/0706.0509
dc.identifierhttp://arxiv.org/abs/0706.0509
dc.identifierAIPConf.Proc.921:169-171,2007
dc.identifierdoi:10.1063/1.2757294
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/179921
dc.subjectAstrophysics
dc.titleGamma-Rays Produced in Cosmic-Ray Interactions and the TeV-band Spectrum of RX J1713.7-3946
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