Difference between revisions of "Galactic cosmic radiation"
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| − | Charged particle radiation that enters the heliosphere continuously from outer space from all directions. The radiation contains electrons (approximately 2%) and a broad range of charged particles from protons up to high Z particles with energies up to several hundreds of GeV and even higher. The fluence rate of GCR in the heliosphere is inversely correlated with the solar activity. It is caused by the solar magnetic field, which is coupled to the solar wind. | + | Charged particle radiation that enters the heliosphere continuously from outer space from all directions. The radiation contains electrons (approximately 2%) and a broad range of charged particles from protons up to high Z particles with energies up to several hundreds of GeV and even higher. The fluence rate of GCR in the heliosphere is inversely correlated with the solar activity. It is caused by the solar magnetic field, which is coupled to the solar wind. |
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| + | (Adapted from [[ICRP Publication 123]], 2013) | ||
'''Return to [[ICRP Glossary|Glossary]]''' | '''Return to [[ICRP Glossary|Glossary]]''' | ||
Latest revision as of 14:27, 7 September 2021
Charged particle radiation that enters the heliosphere continuously from outer space from all directions. The radiation contains electrons (approximately 2%) and a broad range of charged particles from protons up to high Z particles with energies up to several hundreds of GeV and even higher. The fluence rate of GCR in the heliosphere is inversely correlated with the solar activity. It is caused by the solar magnetic field, which is coupled to the solar wind.
(Adapted from ICRP Publication 123, 2013)
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