Density holes in the upstream solar wind

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Density_holes_in_the_upstream_solar_wind.pdf (2.27 MB)

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https://pubs.aip.org/aip/acp/article-abstract/932/1/9/645173/Density-holes-in-the-upstream-solar-wind

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https://doi.org/10.1063/1.2778939
 http://hdl.handle.net/11603/30750

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UMBC Goddard Planetary Heliophysics Institute (GPHI)

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https://orcid.org/0000-0002-5317-988X

Date

2007-08-28

Type of Work

conference papers and proceedings
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Citation of Original Publication

G. K. Parks, E. Lee, N. Lin, F. Mozer, M. Wilber, E. Lucek, I. Dandouras, H. Rème, J. B. Cao, P. Canu, N. Cornilleau‐Wehrlin, P. Décréau, M. L. Goldstein, Philippe Escoubet; Density holes in the upstream solar wind. AIP Conf. Proc. 28 August 2007; 932 (1): 9–15. https://doi.org/10.1063/1.2778939

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This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
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Abstract

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.