Source of Diffuse Upstream Ions: Injection from the Thermal Solar Wind Distribution, Acceleration of a Suprathermal Population, or from the Magnetosphere?

Details Source of Diffuse Upstream Ions: Injection from the Thermal Solar Wind Distribution, Acceleration of a Suprathermal Population, or from the Magnetosphere? Source of Diffuse Upstream Ions: Injection from the Thermal Solar Wind Distribution, Acceleration of a Suprathermal Population, or from the Magnetosphere?

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh51b..09k&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH51B-09

Physics

2154 Planetary Bow Shocks, 7843 Numerical Simulation Studies, 7851 Shock Waves

Scientific paper

We discuss the origin of the diffuse ions upstream of the Earth's bow shock. It is argued that the parallel bow shock cannot exist without upstream waves, which are excited by backstreaming ions. These ions are further accelerated by their interaction with the shock. From the analysis of individual orbits obtained in one-dimensional (1-D) hybrid simulations it is argued that part of the solar wind thermal ions are reflected by the shock potential. These ions gain energy by resonant interaction in an upsteam wave. Subsequently non-resonant interaction in the upstream and downstream wave field accelerates them further. We have investigated questions such as: (1) does a hot solar wind inject more diffuse ions, (2) what is the time scale for the apperance of diffuse ions during directional changes of the interplanetary magnetic field, and (3) why do diffuse protons and alpha particles exhibit the same spectra in terms of energy per charge. Since 1-D simulations are often critisized on the basis that particles are strictly tied to field lines we will also compare the 1-D simulations with three-dimensional quasi-parallel shock simulations.

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