Larmor radius size density holes in the solar wind upstream of the bow shock

Details Larmor radius size density holes in the solar wind upstream of the bow shock Larmor radius size density holes in the solar wind upstream of the bow shock

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh11b..08p&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH11B-08

Physics

2159 Plasma Waves And Turbulence, 2164 Solar Wind Plasma, 7839 Nonlinear Phenomena (4400, 6944), 7851 Shock Waves (4455)

Scientific paper

Ion density holes of Larmor scale size have been observed in the solar wind upstream of the bow shock (Parks et al., 2006). These holes have densities well below that of the solar wind with average depletions ~?n/n ~0.7, but at the upstream edge the density can be enhanced by a factor of 3-5. The density holes have typical durations ~10-20s and are accompanied bysimilarly shaped magnetic structures. However the relationship is complicated. Deep holes with large edge enhancement can have shallow magnetic holes with weak B overshoots while shallow density holes with weak edge enhancements can have deep magnetic holes and large overshoots. These density holes are observed for solar wind velocities ~400 to ~800 km/s, densities nsw ~1-10 and temperature T~100000-1000000 oK. A necessary condition for observing the density holes is that backstreaming energetic particles are present but not all backstreaming particles produce density holes. We believe the density holes are fundamentally important for understanding how the solar wind interacts with the bow shock. The challenge is to develop theories to explain how these nonlinear density holes are produced. Parks, G. et al., Physics of Plasmas, 13, 050701, 2006

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