Computer Science
Scientific paper
Jun 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aipc..471..791d&link_type=abstract
The solar wind nine conference. AIP Conference Proceedings, Volume 471, pp. 791-794 (1999).
Computer Science
Solar Wind Plasma, Sources Of Solar Wind, Atomic, Molecular, And Chemical, And Grain Processes
Scientific paper
Influence of cosmic ray pressure and kinetic stream instability on space plasma dynamics and magnetic structure in the Heliosphere are considered as additional effects to well known effects of solar wind interaction with interstellar medium. It is shown that in the outer Heliosphere are important dynamics effects of galactic cosmic ray pressure on solar wind and interplanetary shock wave propagation as well as on the formation of terminal shock wave of the Heliosphere and subsonic region between Heliosphere and interstellar medium. We determined the behavior of solar wind's Mach number with taking into account cosmic ray nonlinear processes and show that the transition from supersonic to subsonic region can be gradual or shock wave transition in dependence of cosmic ray pressure gradient in the outer Heliosphere. Investigation of cosmic ray convection-diffusion and drift anisotropies shows that kinetic stream instability effects must be especially important on distances more than 40-60 AU from the Sun: formation of great anisotropy of galactic cosmic rays in about spiral interplanetary magnetic field leads to the Alfven turbulence generation by non isotropic cosmic ray fluxes; generated Alfven turbulence influences on cosmic ray propagation, increases the cosmic ray modulation, decreases the cosmic ray anisotropy and increases the cosmic ray pressure gradient in the outer Heliosphere (the last is also important for terminal shock wave formation). The self-consistent problem is formulated and considered for some noncomplicated case.
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