Solar Cosmic RaysIt turned out to be really a rare and happy occasion that we know exact1y when and how a new branch of space physics was born, namely, a physics of solar cosmic rays. It happened on February 28 and March 7, 1942 when the fIrst "cosmic ray bursts" were recorded on the Earth, and the Sun was unambiguously identifIed for the fIrst time as the source of high-velocity 10 particles with energies up to > 10 eV. Just due to such a high energy these relativistic particles have been called "solar cosmic rays" (SCR), in distinction from the "true" cosmic rays of galactic origin. Between 1942 and the beginning ofthe space era in 1957 only extremely high energy solar particle events could be occasionally recorded by cosmic ray ground-Ievel detectors and balloon borne sensors. Since then the detection techniques varied considerably and the study of SCR turned into essential part of solar and solar-terrestrial physics. |
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acceleration activity associated atmosphere bursts calculated changes Chapter characteristics component coronal cosmic rays cycle dependence determined direction distribution Earth effect ejection electric electrons emission energetic energy equation estimates et al example Figure fluence flux function gamma-ray given important impulsive increase indicated intensity interaction interplanetary ions June limit magnetic field maximum mean measurements method Miroshnichenko neutron monitor noted observed obtained occurred October onset parameters particle acceleration particles particular peak period phase physics plasma possible prediction problem processes produced profiles propagation proton events radiation range recent region relativistic respectively rigidity scattering September 29 Shea shock shown shows Smart solar cosmic rays solar flares solar protons space spectra spectrum stations structure suggested Table transport values variations waves X-ray