Up-to-date p-p Interaction Modeling and Secondarygamma, e+/- and Neutrino Spectra in Astronomical Environment

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We have calculated spectra of stable secondary particles ({gamma}, e{sup {+-}}, {nu}{sub e}, {bar {nu}}{sub e}, {nu}{sub {mu}}{bar {nu}}{sub {mu}}) produced in high energy p-p interactions in astrophysical environment. The calculation has incorporated the up-to-date rising inelastic cross-sections, the diffraction dissociation process, and the Feynman scaling violation for the first time. We then found that the diffractive process makes secondary particle spectra harder than that of the incident proton; that the rising inelastic cross-section and the scaling violation produces significantly more secondary particles than previous calculations. Combination of the three features explain about a half of the ''GeV Excess'' in ... continued below

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Abe, T.; Kamae, T.; Karlsson, N.; Koi, T.; Mizuno, T. & /SLAC June 28, 2005.

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We have calculated spectra of stable secondary particles ({gamma}, e{sup {+-}}, {nu}{sub e}, {bar {nu}}{sub e}, {nu}{sub {mu}}{bar {nu}}{sub {mu}}) produced in high energy p-p interactions in astrophysical environment. The calculation has incorporated the up-to-date rising inelastic cross-sections, the diffraction dissociation process, and the Feynman scaling violation for the first time. We then found that the diffractive process makes secondary particle spectra harder than that of the incident proton; that the rising inelastic cross-section and the scaling violation produces significantly more secondary particles than previous calculations. Combination of the three features explain about a half of the ''GeV Excess'' in the EGRET Galactic diffuse {gamma}-ray spectrum with the local cosmic proton spectrum (power-law index around 2.7). The excess can be fully explained if the proton spectral index in the Galactic ridge is harder by 0.2 than above. As an extension of the calculation, we have parameterized the inclusive secondary particle spectra as functions of the incident proton kinetic energy: we predict {approx} 30% more e{sup +} and {nu}{sub e} than e{sup -} and {bar {nu}}{sub e} to be produced in the GeV range by p-p interactions.

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  • Prepared for 22nd Texas Symposium on Relativistic Astrophysics at Stanford University, Stanford, California, 13-17 Dec 2004

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  • Report No.: SLAC-PUB-11080
  • Grant Number: AC02-76SF00515
  • Office of Scientific & Technical Information Report Number: 881152
  • Archival Resource Key: ark:/67531/metadc885615

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  • June 28, 2005

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  • Sept. 21, 2016, 2:29 a.m.

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  • Dec. 2, 2016, 5:04 p.m.

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Abe, T.; Kamae, T.; Karlsson, N.; Koi, T.; Mizuno, T. & /SLAC. Up-to-date p-p Interaction Modeling and Secondarygamma, e+/- and Neutrino Spectra in Astronomical Environment, article, June 28, 2005; [Menlo Park, California]. (digital.library.unt.edu/ark:/67531/metadc885615/: accessed December 13, 2017), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.