Exospheric Model With a Non-Monotonic Potential : Behavior close to the maximum

Details Exospheric Model With a Non-Monotonic Potential : Behavior close to the maximum Exospheric Model With a Non-Monotonic Potential : Behavior close to the maximum

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh32a0718l&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH32A-0718

Physics

2164 Solar Wind Plasma, 2169 Sources Of The Solar Wind, 7511 Coronal Holes, 7827 Kinetic And Mhd Theory

Scientific paper

In exospheric models of the solar wind, the exobase is defined as the altitude where Coulomb collisions between particles become negligible. In slow solar wind models of Lemaire and Scherer (1971), the exobase is located at 5-7 Rs. However in coronal holes, this exobase is located closer to the Sun than the source region of the slow solar wind. In this case, the total potential energy of the protons is first attractive near the Sun, it reaches a maximum at a distance rmax and decreases at larger distances. For the electrons, the total potential energy is always attractive. We extend the exospheric models to the case where the exobase is located below rmax and show that this helps to accelerate the wind to higher speeds as observed at Earth's orbit in the fast solar wind. The behavior of the electrons and protons velocity distribution functions, before and after the maximum, will be shown as well as the method to calculate the radial dependence of the electrical potential. Particular emphasis will be made on how to determine precisely the altitude of the maximum of the protons potential energy. Finally, some links between our model and the Khazanov description in the B - μ space will be developed.

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