Parameterization of γ, epm, and Neutrino Spectra Produced by p-p Interaction in Astronomical Environments

By T. Kamae, N. Karlsson, T. Mizuno, T. Abe, T. Koi. 2006

302 citations recorded by the source corpus.

We present the yield and spectra of stable secondary particles (γ, e±, νe, e, νμ, and μ) 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.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/7503167753da7fc40682f4f2d9cfa10d10012414

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Citations in the corpus

Observational Signatures of Particle Acceleration in Supernova Remnants (2012, background): “This 7 Sometimes the effect of multiplicity and cross section is combined in an inclusive cross section σ(Ep,incl) (e.g. Dermer, 1986; Kamae et al., 2006). relation between the spectral indices of the photon and electron spectrum is the same as for synchrotron radiation (Ginzburg and Syrovatskii,…”
THE SPECTRUM OF ISOTROPIC DIFFUSE GAMMA-RAY EMISSION BETWEEN 100 MeV AND 820 GeV (2014, methodology): “The γ-ray yield from the interactions of the CR with the ISG was calculated using the parametrization of Kamae et al. (2006).”
Gamma-rays from molecular clouds illuminated by cosmic rays escaping from interacting supernova remnants (2010, methodology): “Using the code provided by Kamae et al. (2006) (see also Karlsson & Kamae (2008)), we calculate the spectrum of π0-decay gamma rays.”
DEVELOPMENT OF THE MODEL OF GALACTIC INTERSTELLAR EMISSION FOR STANDARD POINT-SOURCE ANALYSIS OF FERMI LARGE AREA TELESCOPE DATA (2016, methodology): “We fit the emissivity SED of each annulus between 200MeV and 30 GeV using the γ-ray production cross-section of Kamae et al. (2006) and a CR proton flux spectrum parametrized as: bA RP P1 2, where b = v c is the proton-to-light velocity ratio, R is the proton rigidity, A is a free normalization,…”
THE SPECTRUM AND MORPHOLOGY OF THE FERMI BUBBLES (2014, methodology): “For the calculation of the spectrum of gamma rays produced in hadronic interactions, we use the cross sections described in Kamae et al. (2006) and Karlsson & Kamae (2008), which are implemented in the cparamlib package11.”
FERMI-LAT DISCOVERY OF GeV GAMMA-RAY EMISSION FROM THE YOUNG SUPERNOVA REMNANT CASSIOPEIA A (2010, methodology): “The gamma-ray spectrum is calculated following Kamae et al. (2006) with a scaling factor of 1.85 for helium and heavy nuclei (Mori 2009).”
FERMI LAT DISCOVERY OF EXTENDED GAMMA-RAY EMISSION IN THE DIRECTION OF SUPERNOVA REMNANT W51C (2009, methodology): “The gamma-ray spectrum of π 0 -decay is calculated based on Kamae et al. (2006) using a scaling factor of 1.85 for helium and heavy nuclei (Mori 2009).”
FERMI OBSERVATIONS OF CASSIOPEIA AND CEPHEUS: DIFFUSE GAMMA-RAY EMISSION IN THE OUTER GALAXY (2009, methodology): “The emissivity due to p-p interactions is evaluated using the inclusive cross sections as parametrized by Kamae et al. (2006).”
Background model systematics for the Fermi GeV excess (2014, background): “Rs that propagate in the Galaxy. Firstly, CR nuclei produce via inelastic nucleon-nucleon collisions with the interstellar gas neutral mesons (mainly ˇ0s), which subsequently decay to gamma-ray pairs [82,85,86]. This is typically, and throughout this work, referred to as the ˇ0 Galactic diuse compon”
Star-forming galaxies as the origin of diffuse high-energy backgrounds: gamma-ray and neutrino connections, and implications for starburst history (2014, background): “However the relative flux of neutrinos and gamma rays depends on the ratio of charged to neutral pions, Nπ±/Nπ0 , and the relative neutrino flux per flavor depends on the initial mix of π+ to π [71, 72].”
The 511 keV emission from positron annihilation in the Galaxy (2010, background): “New parameterizations of neutral and charged pion cross sections which provide an accurate description of the experimental data in a wide energy range from the pion production threshold up to 105 TeV are discussed in Kelner et al. (2006), Kamae et al. (2006, 2007).”
THE FIRST FERMI LAT SUPERNOVA REMNANT CATALOG (2015, methodology): “In the case of a detected SNR, the photon index, known to reproduce the spectral shape of the parent CR proton/nuclei spectrum above a photon energy of 1 GeV (see e.g. Kamae et al. 2006), is taken to be equal to ΓCR.”
Galactic electrons and positrons at the Earth: new estimate of the primary and secondary fluxes (2010, methodology): “For our default computation, we selected the protonproton cross-section parameterizations provided in Kamae et al. (2006).”