Solar Cosmic RaysSpringer Science & Business Media, 29 июн. 2013 г. - Всего страниц: 480 It 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. |
Содержание
Observational Features and Databases of Solar Cosmic Rays | 23 |
Energetic Particles and HighEnergy Solar Phenomena | 65 |
Solar Cosmic Rays at High Energies | 91 |
Particle Acceleration at the Sun | 119 |
Interactions of Accelerated Particles with the Solar Atmosphere | 171 |
Acceleration and Release of Particles from the Corona | 205 |
Solar Cosmic Rays in the Interplanetary Space | 257 |
Spectrum of Solar Cosmic Rays near the Earth | 297 |
Solar Cosmic Rays in the Geosphere | 331 |
Energetic Solar Particles and Radiation Hazard in Space | 367 |
Problems and Prospects | 407 |
| 421 | |
Figure Captions | 467 |
Другие издания - Просмотреть все
Solar Cosmic Rays, Том 2 Lev Isaakovich Dorman,Leontiĭ Ivanovich Miroshnichenko Просмотр фрагмента - 1976 |
Часто встречающиеся слова и выражения
accelerated particles anisotropy atmosphere Bazilevskaya bursts Cliver cm² component coronal coronal mass ejections current sheet density detectors distribution Earth effect ejection electric field electrons emission energetic particles energy range energy spectra equation estimates Figure fluence function gamma gamma-ray geomagnetic GLEs high-energy intensity intensity-time profiles interaction interplanetary medium interplanetary space ions Kahler loop magnetic field Mandzhavidze maximum mean free path measurements MeV protons MeV/nucleon neutron monitor observed onset parameters particle acceleration particle events peak pitch angle plasma power-law prediction problem processes propagation proton flux radiation Ramaty Reames reconnection references therein region relativistic protons rigidity SCR flux SEP events September 29 Shea and Smart shock Smart and Shea solar activity solar cosmic rays solar cycle solar energetic particles solar flares solar neutron solar particle solar proton events solar wind spacecraft values variations Vashenyuk velocity waves X-ray