Detailed Examination of Ion Kinetics For Foreshock Density Holes

Details Detailed Examination of Ion Kinetics For Foreshock Density Holes Detailed Examination of Ion Kinetics For Foreshock Density Holes

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh13a0381w&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH13A-0381

Other

7514 Energetic Particles (2114), 7827 Kinetic And Mhd Theory, 7839 Nonlinear Phenomena (4400, 6944), 7863 Turbulence (4490)

Scientific paper

The upstream density holes described in the previous paper by Parks et al. are non-linear structures observed in the ion foreshock. From multi-spacecraft timing analysis we know that these structures can stand relative to the solar wind, in which cases their formation and time development requires an interaction with the solar wind, as well as with particles emerging from the bow shock downstream. Our approach to understanding the factors leading to their development begins with a detailed examination of ion kinetics placed in context with solar wind conditions, bow shock geometry and local structure geometry. Ion distributions within density holes show an isotropic energetic population that appears much like the diffuse ions seen in quasi-parallel foreshock regions, indicating flux tubes or limited domains in which rapid diffusive heating occurs. The very low densities observed neccesitate a depletion of the main solar wind beam, and this results from an inbalance of inflow and outflow, and possibly due to flow around the structures. Remote sensing distributions confirm the very sharp ion-scale gradients inferred from timing analysis. We present indications that these structures are usually seen in close proximity to the shock, which may point to a direct role of that structure in their occurrence. Finally, we will compare the ion dynamics of foreshock density holes with those occuring in association with other upstream structures, including SLAMS, diamagnetic cavities and hot flow anomolies.

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