Density holes in the upstream solar wind

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

doi:10.1063/1.2778939

Density holes in the upstream solar wind

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

^*Corresponding author for this work

University of California at Berkeley
Imperial College London
Institute de Recherche en Astrophysique et Planétologie
CAS - National Space Science Center
IPSL
Université d'Orléans
NASA Goddard Space Flight Center
ESA/ESTEC

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution › peer-review

12 Scopus citations

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.

Original language	English
Title of host publication	TURBULENCE AND NONLINEAR PROCESSES IN ASTROPHYSICAL PLASMAS
Subtitle of host publication	6th Annual International Astrophysics Conference
Pages	9-15
Number of pages	7
DOIs	https://doi.org/10.1063/1.2778939
State	Published - 2007
Externally published	Yes
Event	TURBULENCE AND NONLINEAR PROCESSES IN ASTROPHYSICAL PLASMAS: 6th Annual International Astrophysics Conference - Oahu, HI, United States Duration: 16 Mar 2007 → 22 Mar 2007

Publication series

Name	AIP Conference Proceedings
Volume	932
ISSN (Print)	0094-243X
ISSN (Electronic)	1551-7616

Conference

Conference	TURBULENCE AND NONLINEAR PROCESSES IN ASTROPHYSICAL PLASMAS: 6th Annual International Astrophysics Conference
Country/Territory	United States
City	Oahu, HI
Period	16/03/07 → 22/03/07

Keywords

Density hole

Access to Document

10.1063/1.2778939

Cite this

Parks, G. K., Lee, E., Lin, N., Mozer, F., Wilber, M., Lucek, E., Dandouras, I., Rème, H., Cao, J. B., Canu, P., Cornilleau-Wehrlin, N., Décréau, P., Goldstein, M. L., & Escoubet, P. (2007). Density holes in the upstream solar wind. In TURBULENCE AND NONLINEAR PROCESSES IN ASTROPHYSICAL PLASMAS: 6th Annual International Astrophysics Conference (pp. 9-15). (AIP Conference Proceedings; Vol. 932). https://doi.org/10.1063/1.2778939

@inproceedings{20e2572f97254f3a817a43c54f414d05,

title = "Density holes in the upstream solar wind",

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.",

keywords = "Density hole",

author = "Parks, \{G. K.\} and E. Lee and N. Lin and F. Mozer and M. Wilber and E. Lucek and I. Dandouras and H. R{\`e}me and Cao, \{J. B.\} and P. Canu and N. Cornilleau-Wehrlin and P. D{\'e}cr{\'e}au and Goldstein, \{M. L.\} and Philippe Escoubet",

year = "2007",

doi = "10.1063/1.2778939",

language = "英语",

isbn = "0735404437",

series = "AIP Conference Proceedings",

pages = "9--15",

booktitle = "TURBULENCE AND NONLINEAR PROCESSES IN ASTROPHYSICAL PLASMAS",

note = "TURBULENCE AND NONLINEAR PROCESSES IN ASTROPHYSICAL PLASMAS: 6th Annual International Astrophysics Conference ; Conference date: 16-03-2007 Through 22-03-2007",

}

Parks, GK, Lee, E, Lin, N, Mozer, F, Wilber, M, Lucek, E, Dandouras, I, Rème, H, Cao, JB, Canu, P, Cornilleau-Wehrlin, N, Décréau, P, Goldstein, ML & Escoubet, P 2007, Density holes in the upstream solar wind. in TURBULENCE AND NONLINEAR PROCESSES IN ASTROPHYSICAL PLASMAS: 6th Annual International Astrophysics Conference. AIP Conference Proceedings, vol. 932, pp. 9-15, TURBULENCE AND NONLINEAR PROCESSES IN ASTROPHYSICAL PLASMAS: 6th Annual International Astrophysics Conference, Oahu, HI, United States, 16/03/07. https://doi.org/10.1063/1.2778939

TY - GEN

T1 - Density holes in the upstream solar wind

AU - Parks, G. K.

AU - Lee, E.

AU - Lin, N.

AU - Mozer, F.

AU - Wilber, M.

AU - Lucek, E.

AU - Dandouras, I.

AU - Rème, H.

AU - Cao, J. B.

AU - Canu, P.

AU - Cornilleau-Wehrlin, N.

AU - Décréau, P.

AU - Goldstein, M. L.

AU - Escoubet, Philippe

PY - 2007

Y1 - 2007

N2 - 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.

AB - 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.

KW - Density hole

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T2 - TURBULENCE AND NONLINEAR PROCESSES IN ASTROPHYSICAL PLASMAS: 6th Annual International Astrophysics Conference

Y2 - 16 March 2007 through 22 March 2007

ER -

Density holes in the upstream solar wind

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Keywords

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