Cosmic ray acceleration in supernova remnants and the FERMI/PAMELA data

被引：109

作者：

Ahlers, Markus ^{[1
]}

Mertsch, Philipp ^{[1
]}

Sarkar, Subir ^{[1
]}

机构：

[1] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England

来源：

PHYSICAL REVIEW D | 2009年 / 80卷 / 12期

关键词：

GAMMA-RAYS; PARTICLE-ACCELERATION; GALACTIC SOURCES; RX J1713.7-3946; TEV; DISCOVERY; EMISSION; ELECTRONS; ENERGIES; SPECTRA;

D O I：

10.1103/PhysRevD.80.123017

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We discuss recent observations of high energy cosmic ray positrons and electrons in the context of hadronic interactions in supernova remnants (SNRs), the suspected accelerators of galactic cosmic rays. Diffusive shock acceleration can harden the energy spectrum of secondary positrons relative to that of the primary protons and electrons and thus explain the rise in the positron fraction observed by PAMELA above 10 GeV. We normalize the hadronic interaction rate by holding pion decay to be responsible for the gamma rays detected by HESS from some SNRs. By simulating the spatial and temporal distribution of SNRs in the Galaxy according to their known statistics, we are able to then fit the electron (plus positron) energy spectrum measured by Fermi. It appears that IceCube has good prospects for detecting the hadronic neutrino fluxes expected from nearby SNRs.

引用

页数：14

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