Cosmic Rays in Interplanetary Magnetic Fields by I.N. Toptygin

By I.N. Toptygin

Fast debris of typical or1g1n (cosmic rays) were used for a very long time as a tremendous resource of astrophysical and geophysical details. A research of cosmic ray spectra, time adaptations, abundances, gradients, and anisotropy presents a wealth of information on actual stipulations within the areas of cosmic ray iteration in addition to within the media during which cosmic rays propagate. Astrophysical elements of cosmic ray physics were thought of in a couple of monograpqs. the main unique appears "The starting place of Cosmic Rays" by means of V. L. Ginzburg and S. 1. Syrovatskij (1964) that is, despite the fact that, involved as a rule with galactic cosmic rays. The physics of the circumsolar house is mentioned during this booklet purely fairly in brief. numerous different monographs were committed often to the physics of the interplanetary medium and cosmic rays in interplanetary house. those comprise the books via Dorman (1963, 1975a, b), Parker (1963), Dorman and Miroshnichenko (1968). the current monograph differs from the above pointed out books in major elements: (i) It provides a unified theoretical method of analys{ng the homes of speedy debris in interplanetary area, established upon attention of cosmic rays as a hugely full of life part of the interplane~ary plasma, which uses the plasma physics how to describe the behaviour of cosmic rays.

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This may amplify plasma and magnetic field disturbances at large distances and affect significantly the behaviour of cosmic rays. Chromospheric flares and quieter manifestations of solar activity, such as eruptive plasma outbursts, coronal transients and magnetic filament decays, represent the second important source of interplanetary plasma disturbance. These phenomena lead to outbursts of accelerated plasmas, generation of shocks and high-speed streams; see §4 for details. Hagnetic field disturbances are most important for cosmic ray physics.

20) becomes dominant. For instance, the travel path of a wave with A = 103 km OSCILLATIONS AND WAVES IN SOLAR \VIND PLASMA 38 in a Maxwellian plasma with vTp ~ vA is as short as 5 x 10 4 km. 3) should have been generated near the place of observation. Their generation was likely to be caused by an interaction between solar wind streams with different velocities or by non-linear interactions of waves with larger wavelengths. The above estimates of Alfven wave travel paths in the solar wind should be regarded as rather approximate because the wave decrements are extremely sensitive to the distribution functions of protons and electrons in the background plasma.

With the amplitude growing. a fast magneto-acoustic wave may convert into a shock which leads to a change of the damping regime. 1, in particular vTp % vA. The linear decrement essentially depends on the angle 8. 03w, are realized only at 8 ~ 12° and 45° ~ 8 ~ 80° as well as in y~ ~ the corresponding ranges of angles at 8 > 90°. However, since the OSCILLATIONS AND \"AVES IN SOLAR WIND PLASMA 32 direction of BO varies with distance. 03w, e. lBO• The distance /:"r :t u/y~ which a wave is able to travel from where i t is generated is determined by the solar wind speed because v h «u.

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