Physics – Plasma Physics
Scientific paper
Jan 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aipc..813.1272o&link_type=abstract
SPACE TECH.& APPLIC.INT.FORUM-STAIF 2006: 10th Conf Thermophys Applic Microgravity; 23rd Symp Space Nucl Pwr & Propulsion; 4th C
Physics
Plasma Physics
Space Plasma Physics, Solar Wind Plasma, Sources Of Solar Wind, Random Walks And Levy Flights
Scientific paper
Two coupled finite-difference solutions to the adjoint heliospheric transport equation have been solved using a random-walk method. The heliosphere has been represented as a 140 AU sphere with the sun at 100 AU from the boundary in the bow-shock direction and 40 AU from the center of the heliosphere. The dependence of the solar wind on latitude is included, varying from 400 to 800 km/s. Flux spectra and angular distributions in the heliosphere, leakage spectra from the heliosphere and the transit time of cosmic ray particles from the boundary of the heliosphere to earth orbit have been calculated. The diffusion coefficient was represented by a simple scalar and the solar-wind termination shock has been so far neglected. Solar activity was represented by a recent solar minimum. The results of these calculations are fluxes, angular distributions and transit times for cosmic rays in interplanetary space. Good values for fluxes and their angular distributions are necessary for the calculation of radiation doses to astronauts, and knowledge of transit times makes it possible to estimate interplanetary fluxes from earth-bound measurements.
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