Journal article Open Access

Evidence for shock acceleration of high-energy electrons in the supernova remnant SN1006

Koyama, K.; Petre, R.; Gotthelf, E. V.; Hwang, U.; Matsuura, M.; Ozaki, M.; Holt, S. S.


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  <dc:creator>Koyama, K.</dc:creator>
  <dc:creator>Petre, R.</dc:creator>
  <dc:creator>Gotthelf, E. V.</dc:creator>
  <dc:creator>Hwang, U.</dc:creator>
  <dc:creator>Matsuura, M.</dc:creator>
  <dc:creator>Ozaki, M.</dc:creator>
  <dc:creator>Holt, S. S.</dc:creator>
  <dc:date>1995-11-16</dc:date>
  <dc:description>HIGH-ENERGY cosmic rays (relativistic heavy nuclei) play an important role in heating interstellar matter in the Milky Way1,2, and they affect chemical abundances through collisions with atoms in the interstellar gas2. Although it has long been thought that these cosmic rays arise from supernovae3,4, direct evidence for such an association has been lacking. Here we report X-ray observations of the remnant of supernova 1006, made by the ASCA satellite, which indicate that emission from the edges of the remnant shell is dominated by radiation from electrons accelerated to energies of ˜ 100 TeV within the shock front. Ions in the shell are likely to have been accelerated to similar energies, thus giving rise to very-high-energy cosmic rays.</dc:description>
  <dc:identifier>https://zenodo.org/record/1233170</dc:identifier>
  <dc:identifier>10.1038/378255a0</dc:identifier>
  <dc:identifier>oai:zenodo.org:1233170</dc:identifier>
  <dc:rights>info:eu-repo/semantics/openAccess</dc:rights>
  <dc:rights>https://creativecommons.org/publicdomain/zero/1.0/legalcode</dc:rights>
  <dc:title>Evidence for shock acceleration of high-energy electrons in the supernova remnant SN1006</dc:title>
  <dc:type>info:eu-repo/semantics/article</dc:type>
  <dc:type>publication-article</dc:type>
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