Overview

xxii CONTENTS In 1957 I was invited to work on special problems in Magnetic Laboratory of the Academy of Sciences of USSR as a Head of Department of Magnetic Hydrodynamics. In few years this Laboratory was transfered into the I. V. Kurchatov Institute of Atomic Energy, and I continued to work in this Institute up to 1965. In parallel I also worked at Moscow State University as Professor in the CR and Space Research Team. I also gave lectures in Irkutsk, Alma-Ata, Nalchik, Tbilisi, Erevan, Samarkand, and others places. Over about 40 years of teaching under my supervision more than hundred graduate students and scientists in USSR and some other countries gained their Ph. D. and several tenths became Doctors of Science. As my hobby I continued to work in CR research, and as Vice-President of All-Union Section of Cosmic Rays and Radiation Belts, took an active part in preparing the Soviet net of CR stations to the IGY (International Geophysical Year, 1957-1958): we equipped all soviet stations in USSR and in Antarctica with standard cubic and semi-cubic muon telescopes and with neutron monitors of IGY (or Simpson’s) type. In connection with preparing for the IQSY (the International Quiet Sun Year, 1964-1965), the soviet net of CR stations was extended about two fold and they were equipped with neutron super-monitors of IQSY type (with an effective surface about 10 times bigger than the previous monitor of IGY type).

Full Product Details

Author:   Lev Dorman ,  L I Dorman
Publisher:   Springer
Imprint:   Springer
Edition:   Softcover reprint of the original 1st ed. 2006
Volume:   339
Dimensions:   Width: 15.50cm , Height: 4.40cm , Length: 23.50cm
Weight:   1.781kg
ISBN:  

9789402404531

ISBN 10:   9402404538
Pages:   847
Publication Date:   23 August 2016
Audience:   Professional and scholarly ,  Professional & Vocational
Format:   Paperback
Publisher's Status:   Active
Availability:   Manufactured on demand  
We will order this item for you from a manufactured on demand supplier.

Table of Contents

CONTENTS Preface xxi Acknowledgments xxvii Frequently used Abbreviations and Notations xxix Chapter 1. Cosmic Ray Interactions in Space Plasmas 1 1.1. Main properties of space plasma 1 1.1.1. Neutrality of space plasma and Debay radius 1 1.1.2. Conductivity and magnetic viscosity of space plasma 1 1.1.3. The time of magnetic fields dissipation; frozen magnetic fields 1 1.1.4. Transport path of ions in space plasma 2 1.1.5. Space plasma as excited magneto-turbulent plasma 2 1.1.6. Main channels of energy transformation in space plasma 2 1.1.7. Particle acceleration in space plasma and the second fundamental low of thermodynamics 3 1.2. Main properties and origin of CR 4 1.2.1. Internal and external CR of different origin 4 1.2.2. On the main properties of primary and secondary CR 4 1.2.3. Five intervals in the observed CR energy spectrum 5 1.2.4. Main CR properties and origin of CR in the interval 1 7 1.2.5. The anisotropy in energy intervals 1 and 2 7 1.2.6. Relationships between the observed CR spectrum, the anisotropy, the relative content of the daughter nuclei, and the transport scattering path 9 1.2.7. Chemical composition in the range and the expected dependence of and on 11 1.2.8. Chemical composition in the energy range and the nature of the scattering elements in the Galaxy 11 1.2.9. The nature of the energy boundary between intervals 3 and 2 12 1.2.10. The mode of the dependence of L on particle rigidity R from solar modulation data of protons, electrons, and nuclei with various Z 13 1.2.11. The dependence of L on from data of solar CR propagation 15 1.2.12. The features of the solar modulation of the CR spectrum and the measurements of the radial gradient 16 1.2.13. The nature of the CR in energyintervals 3 - 5 16 1.3. Nuclear interactions of CR with space plasma matter 16 1.3.1. Cross sections, paths for absorption, and life time of CR particles relative to nuclear interactions in space plasma 16 1.3.2. CR fragmentation in space plasma 17 1.3.3. Expected fluxes of secondary electrons, positrons, g - quanta, and neutrinos 19 1.3.4. Expected fluxes of secondary protons and antiprotons 22 1.4. CR absorption by solid state matter (stars, planets, asteroids, meteorites, dust) and secondary CR albedo 22 1.5. CR interactions with electrons of space plasma and ionization losses 23 1.5.1. Ionization energy losses by CR nuclei during propagation in the space 23 1.5.2. Ionization and bremsstrahlung losses for CR electrons 25 1.6. CR interactions with photons in space 26 1.6.1. Interactions of CR nucleus with space photons 26 1.6.2. CR electron interactions with the photon field 27 1.7. Energy variations of CR particles in their interactions with magnetic fields 27 1.7.1. Synchrotron losses of energy by CR particles in magnetic fields 27 1.7.2. Acceleration and deceleration of particles in their interactions with moving magnetic fields 29 1.8. CR particle motion in magnetic fields; scattering by magnetic inhomogeneities 30 1.8.1. CR particle motion in the regular magnetic fields frozen into moving plasma formations 30 1.8.2. CR particle moving in essentially inhomogeneous magnetized plasma 31 1.8.3. Two-dimensional model of CR particle scattering by magnetic inhomogeneities of type 32 1.8.4. Scattering by cylindrical fibers with homogeneous field 32 1.8.5. Scattering by cylindrical fibers with field of type 33 1.8.6. Three-dimensional model of scattering by inhomogeneities of the type against the background of general field 35 1.9. The transport path o

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