Physics
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh71a..01f&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #SH71A-01
Physics
1
2104 Cosmic Rays, 2134 Interplanetary Magnetic Fields, 2151 Neutral Particles, 7843 Numerical Simulation Studies
Scientific paper
Galactic cosmic ray propagation in the heliosphere has traditionally been the domain of modulation studies for the past three decades. To date, virtually all such models have lacked a self consistent treatment of the three principal particle species -- plasma with magnetic field, interstellar neutral atoms and galactic cosmic rays. To overcome this drawback we have developed a global self-consistent model of the heliosphere which we use to study the entry of the galactic cosmic rays into the heliosphere directly from the local interstellar medium population. An important improvement over the previous global heliospheric models is that a kinetic description for the cosmic rays is used instead of the usual fluid approach, which allows us to study the evolution of the particle spectra with distance. Our model is axisymmetric with respect to the interstellar flow, but includes a complete three-dimensional heliospheric magnetic field. Cosmic-ray diffusion coefficients are computed from the quasi-linear theory assuming a constant (but different) power spectrum of the fluctuations in both the solar wind and the interstellar medium. Our results show that low energy particles are strongly attenuated by the magnetic wall in the inner heliosheath and do not reach the termination shock. The model predicts small cosmic rays gradients implying little modification to the heliospheric boundaries. Particle spectra in the inner heliosphere are found to be in agreement with the observations. We also find the inner heliospheric galactic cosmic-ray population is not sensitive to the upstream-downstream asymmetry of the termination shock.
Florinski Vladimir
Pogorelov Nikolai V.
Zank Gary P.
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