Density holes in the upstream solar wind

G. K. Parks (1) , E. Lee (1) , N. Lin (1) , F. Mozer (1) , M. Wilber (1) , E. Lucek (2) , I. Dandouras (3) , H. Rème (3) , J.B. Cao (4) , P. Canu (5) , Nicole Cornilleau-Wehrlin (5) , Pierrette Décréau (6) , M.L. Goldstein (7) , Philippe C. Escoubet (8)

1 SSL - Space Sciences Laboratory [Berkeley]
2 Blackett Laboratory
3 CESR - Centre d'étude spatiale des rayonnements
4 SKSW - State Key Laboratory of Space Weather [Beijing]
5 CETP - Centre d'étude des environnements terrestre et planétaires
6 LPCE - Laboratoire de physique et chimie de l'environnement
7 GSFC - NASA Goddard Space Flight Center
8 ESA - Agence Spatiale Européenne = European Space Agency

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.

Domains: Sciences of the Universe [physics]

G. K. Parks, E. Lee, N. Lin, F. Mozer, M. Wilber, et al.. Density holes in the upstream solar wind. 6th Annual International Astrophysics Conference, 2007, Oahu, United States. pp.9-15, ⟨10.1063/1.2778939⟩. ⟨insu-02926784⟩