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Parameterization of γ, e±, and neutrino spectra produced by p-p interaction in astronomical environments
KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
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2006 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 647, no 1 I, 692-708 p.Article in journal (Refereed) Published
Abstract [en]

We present the yield and spectra of stable secondary particles (γ, e±, νe, ν̄e, νμ, and v̄μ of p-p interaction in parameterized formulae to facilitate calculations involving them in astronomical environments. The formulae are derived from the up-to-date/p-p interaction model by Kamae et al. (2005), which incorporates the logarithmically rising inelastic cross section, the diffraction dissociation process, and the Feynman scaling violation. To improve fidelity to experimental data in lower energies, two baryon resonance contributions have been added: one representing Δ(1232) and the other representing multiple resonances around 1600 MeV/c-2. The parameterized formulae predict that all secondary particle spectra be harder by about 0.05 in power-law indices than that of the incident proton and their inclusive cross sections be larger than those predicted by p-p interaction models based on the Feynman scaling.

Place, publisher, year, edition, pages
2006. Vol. 647, no 1 I, 692-708 p.
Keyword [en]
Cosmic rays, Galaxies: jets, Gamma rays: theory, ISM: general, Neutrinos, Supernovae: general
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:kth:diva-155999DOI: 10.1086/505189ISI: 000239647800062ScopusID: 2-s2.0-33748441814OAI: diva2:765651

QC 20141124

Available from: 2014-11-24 Created: 2014-11-17 Last updated: 2015-10-14Bibliographically approved

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