Testing astrophysical models for the PAMELA positron excess with cosmic ray nuclei.
The excess in the positron fraction measured by PAMELA has been interpreted as due to annihilation or decay of dark matter in the Galaxy. More prosaically it has been ascribed to direct production of positrons by nearby pulsars or due to pion production during diffusive shock acceleration of hadroni...
| Main Authors: | , |
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| Format: | Journal article |
| Language: | English |
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2009
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| _version_ | 1826267031513595904 |
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| author | Mertsch, P Sarkar, S |
| author_facet | Mertsch, P Sarkar, S |
| author_sort | Mertsch, P |
| collection | OXFORD |
| description | The excess in the positron fraction measured by PAMELA has been interpreted as due to annihilation or decay of dark matter in the Galaxy. More prosaically it has been ascribed to direct production of positrons by nearby pulsars or due to pion production during diffusive shock acceleration of hadronic cosmic rays in nearby sources. We point out that measurements of secondary cosmic ray nuclei can discriminate between these possibilities. New data on the titanium-to-iron ratio support the hadronic source model above and enable a prediction for the boron-to-carbon ratio at energies above 100 GeV. |
| first_indexed | 2024-03-06T20:47:58Z |
| format | Journal article |
| id | oxford-uuid:3691f8b6-b42d-4f48-b8b2-01b9aa774c81 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T20:47:58Z |
| publishDate | 2009 |
| record_format | dspace |
| spelling | oxford-uuid:3691f8b6-b42d-4f48-b8b2-01b9aa774c812022-03-26T13:38:44ZTesting astrophysical models for the PAMELA positron excess with cosmic ray nuclei.Journal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:3691f8b6-b42d-4f48-b8b2-01b9aa774c81EnglishSymplectic Elements at Oxford2009Mertsch, PSarkar, SThe excess in the positron fraction measured by PAMELA has been interpreted as due to annihilation or decay of dark matter in the Galaxy. More prosaically it has been ascribed to direct production of positrons by nearby pulsars or due to pion production during diffusive shock acceleration of hadronic cosmic rays in nearby sources. We point out that measurements of secondary cosmic ray nuclei can discriminate between these possibilities. New data on the titanium-to-iron ratio support the hadronic source model above and enable a prediction for the boron-to-carbon ratio at energies above 100 GeV. |
| spellingShingle | Mertsch, P Sarkar, S Testing astrophysical models for the PAMELA positron excess with cosmic ray nuclei. |
| title | Testing astrophysical models for the PAMELA positron excess with cosmic ray nuclei. |
| title_full | Testing astrophysical models for the PAMELA positron excess with cosmic ray nuclei. |
| title_fullStr | Testing astrophysical models for the PAMELA positron excess with cosmic ray nuclei. |
| title_full_unstemmed | Testing astrophysical models for the PAMELA positron excess with cosmic ray nuclei. |
| title_short | Testing astrophysical models for the PAMELA positron excess with cosmic ray nuclei. |
| title_sort | testing astrophysical models for the pamela positron excess with cosmic ray nuclei |
| work_keys_str_mv | AT mertschp testingastrophysicalmodelsforthepamelapositronexcesswithcosmicraynuclei AT sarkars testingastrophysicalmodelsforthepamelapositronexcesswithcosmicraynuclei |