On cosmic ray acceleration in supernova remnants and the FERMI/PAMELA data
We discuss recent observations of high energy cosmic ray positrons and electrons in the context of hadronic interactions in supernova remnants, the suspected accelerators of galactic cosmic rays. Diffusive shock acceleration can harden the energy spectrum of secondary positrons relative to that of t...
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| Format: | Journal article |
| Language: | English |
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2009
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| _version_ | 1826294974620106752 |
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| author | Ahlers, M Mertsch, P Sarkar, S |
| author_facet | Ahlers, M Mertsch, P Sarkar, S |
| author_sort | Ahlers, M |
| collection | OXFORD |
| description | We discuss recent observations of high energy cosmic ray positrons and electrons in the context of hadronic interactions in supernova remnants, 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. |
| first_indexed | 2024-03-07T03:53:58Z |
| format | Journal article |
| id | oxford-uuid:c23a5765-d773-4d89-8c93-9a05ee961dd7 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T03:53:58Z |
| publishDate | 2009 |
| record_format | dspace |
| spelling | oxford-uuid:c23a5765-d773-4d89-8c93-9a05ee961dd72022-03-27T06:07:22ZOn cosmic ray acceleration in supernova remnants and the FERMI/PAMELA dataJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:c23a5765-d773-4d89-8c93-9a05ee961dd7EnglishSymplectic Elements at Oxford2009Ahlers, MMertsch, PSarkar, SWe discuss recent observations of high energy cosmic ray positrons and electrons in the context of hadronic interactions in supernova remnants, 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. |
| spellingShingle | Ahlers, M Mertsch, P Sarkar, S On cosmic ray acceleration in supernova remnants and the FERMI/PAMELA data |
| title | On cosmic ray acceleration in supernova remnants and the FERMI/PAMELA
data |
| title_full | On cosmic ray acceleration in supernova remnants and the FERMI/PAMELA
data |
| title_fullStr | On cosmic ray acceleration in supernova remnants and the FERMI/PAMELA
data |
| title_full_unstemmed | On cosmic ray acceleration in supernova remnants and the FERMI/PAMELA
data |
| title_short | On cosmic ray acceleration in supernova remnants and the FERMI/PAMELA
data |
| title_sort | on cosmic ray acceleration in supernova remnants and the fermi pamela data |
| work_keys_str_mv | AT ahlersm oncosmicrayaccelerationinsupernovaremnantsandthefermipameladata AT mertschp oncosmicrayaccelerationinsupernovaremnantsandthefermipameladata AT sarkars oncosmicrayaccelerationinsupernovaremnantsandthefermipameladata |