Density holes in the upstream solar wind

Details Density holes in the upstream solar wind Density holes in the upstream solar wind

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aipc..932....9p&link_type=abstract

TURBULENCE AND NONLINEAR PROCESSES IN ASTROPHYSICAL PLASMAS; 6th Annual International Astrophysics Conference. AIP Conference P

Astronomy and Astrophysics

Astrophysics

5

Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind, Mhd Waves, Plasma Waves, Turbulence

Scientific paper

Larmor size transient structures with depletions as large as 99% of ambient solar wind density levels occur commonly upstream of Earth's collisionless bow shock. These ``density holes'' have a mean duration of ~17.9 +/- 10.4s but holes as short as 4s have been observed. The average fractional density depletion (δn/n) inside the holes is ~0.68 +/- 0.14. The density of the upstream edge moving in the sunward direction can be enhanced by five or more times the solar wind density. Particle distributions show the steepened edge can behave like a shock, and measured local field geometries and Mach number support this view. Similarly shaped magnetic holes accompany the density holes indicating strong coupling between fields and particles. The density holes are only observed with upstream particles, suggesting that back-streaming particles interacting with the solar wind are important.

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