Cosmic ray acceleration by stellar wind. Simulation for heliosphere

Details Cosmic ray acceleration by stellar wind. Simulation for heliosphere Cosmic ray acceleration by stellar wind. Simulation for heliosphere

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....4..196p&link_type=abstract

In NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 4 p 196-199 (SEE N85-34729 23-92)

Computer Science

Cosmic Rays, Interplanetary Medium, Particle Acceleration, Shock Waves, Solar Wind, Computerized Simulation, Heliosphere, Kinetic Energy, Shock Fronts

Scientific paper

The solar wind deceleration by the interstellar medium may result in the existence of the solar wind terminal shock. In this case a certain fraction of thermal particles after being heated at the shock would obtain enough energy to be injected to the regular acceleration process. An analytical solution for the spectrum in the frame of a simplified model that includes particle acceleration at the shock front and adiabatic cooling inside the stellar wind cavity has been derived. It is shown that the acceleration of the solar wind particles at the solar wind terminal shock is capable of providing the total flux, spectrum and radial gradients of the low-energy protons close to one observed in the interplanetary space.

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