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. ([[ICRP Publication 123]], 2013) | 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. ([[ICRP Publication 123]], 2013) | ||
| + | ''ICRP Glossary entry - June 2019'' | ||
| − | ''[[ICRP Glossary]] | + | |
| + | '''Return to [[ICRP Glossary|Glossary]]''' | ||
Revision as of 20:14, 12 September 2019
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. (ICRP Publication 123, 2013)
ICRP Glossary entry - June 2019
Return to Glossary
