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Free energy to drive equatorial magnetosonic wave instability at geosynchronous orbit

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Free energy to drive equatorial magnetosonic wave instability at geosynchronous orbit. / Thomsen, M. F.; Denton, Michael; Jordanova, V. K.; Chen, L.; Thorne, R. M.

In: Journal of Geophysical Research, Vol. 116, A08220, 23.08.2011, p. -.

Research output: Contribution to journalJournal article

Harvard

Thomsen, MF, Denton, M, Jordanova, VK, Chen, L & Thorne, RM 2011, 'Free energy to drive equatorial magnetosonic wave instability at geosynchronous orbit', Journal of Geophysical Research, vol. 116, A08220, pp. -. https://doi.org/10.1029/2011JA016644

APA

Thomsen, M. F., Denton, M., Jordanova, V. K., Chen, L., & Thorne, R. M. (2011). Free energy to drive equatorial magnetosonic wave instability at geosynchronous orbit. Journal of Geophysical Research, 116, -. [A08220]. https://doi.org/10.1029/2011JA016644

Vancouver

Thomsen MF, Denton M, Jordanova VK, Chen L, Thorne RM. Free energy to drive equatorial magnetosonic wave instability at geosynchronous orbit. Journal of Geophysical Research. 2011 Aug 23;116:-. A08220. https://doi.org/10.1029/2011JA016644

Author

Thomsen, M. F. ; Denton, Michael ; Jordanova, V. K. ; Chen, L. ; Thorne, R. M. / Free energy to drive equatorial magnetosonic wave instability at geosynchronous orbit. In: Journal of Geophysical Research. 2011 ; Vol. 116. pp. -.

Bibtex

@article{a95df660ef5e43b0a8c34fa8ae730f4e,
title = "Free energy to drive equatorial magnetosonic wave instability at geosynchronous orbit",
abstract = "The magnetosonic (or ion Bernstein) instability is driven by a positive slope in the ion distribution function perpendicular to the magnetic field at energies above about 1 keV. Fifteen years of multisatellite geosynchronous observations are used to determine the statistical occurrence of ion distributions with positive slopes as a function of energy, local time, geomagnetic activity, and phase of the solar cycle. There is no discernable dependence on phase of the solar cycle, but there are clear dependences on the other parameters. Positive slopes are seen primarily in the energy range between similar to 3 and similar to 24 keV. The peak occurrence of positive slopes is between midmorning and dusk and moves progressively toward earlier local times for higher energies. The occurrence is significantly greater and extends over a broader local time range for low levels of geomagnetic activity than for high activity, for all energies. At high activity levels, the occurrence tends to be more closely confined near noon. Peak occurrence rates are similar to 30% at energies just below 10 keV. A superposed epoch analysis of 77 coronal mass ejection (CME)-driven storms and 93 high-speed solar wind (HSS)-driven storms shows a relative suppression of the occurrence frequency of positive slopes during the recovery phase. The suppression is particularly long-lived for HSS-driven streams.",
keywords = "OUTER RADIATION BELT, ION-CYCLOTRON WAVES, LINEAR DIFFUSION-COEFFICIENTS, WHISTLER-MODE CHORUS, GEOMAGNETIC STORMS, RELATIVISTIC ELECTRONS, RING CURRENT, INNER MAGNETOSPHERE, MAGNETIC STORM, SOLAR-WIND",
author = "Thomsen, {M. F.} and Michael Denton and Jordanova, {V. K.} and L. Chen and Thorne, {R. M.}",
note = "{\textcopyright}2011. American Geophysical Union. All Rights Reserved.",
year = "2011",
month = aug
day = "23",
doi = "10.1029/2011JA016644",
language = "English",
volume = "116",
pages = "--",
journal = "Journal of Geophysical Research",
issn = "0148-0227",
publisher = "American Geophysical Union",

}

RIS

TY - JOUR

T1 - Free energy to drive equatorial magnetosonic wave instability at geosynchronous orbit

AU - Thomsen, M. F.

AU - Denton, Michael

AU - Jordanova, V. K.

AU - Chen, L.

AU - Thorne, R. M.

N1 - ©2011. American Geophysical Union. All Rights Reserved.

PY - 2011/8/23

Y1 - 2011/8/23

N2 - The magnetosonic (or ion Bernstein) instability is driven by a positive slope in the ion distribution function perpendicular to the magnetic field at energies above about 1 keV. Fifteen years of multisatellite geosynchronous observations are used to determine the statistical occurrence of ion distributions with positive slopes as a function of energy, local time, geomagnetic activity, and phase of the solar cycle. There is no discernable dependence on phase of the solar cycle, but there are clear dependences on the other parameters. Positive slopes are seen primarily in the energy range between similar to 3 and similar to 24 keV. The peak occurrence of positive slopes is between midmorning and dusk and moves progressively toward earlier local times for higher energies. The occurrence is significantly greater and extends over a broader local time range for low levels of geomagnetic activity than for high activity, for all energies. At high activity levels, the occurrence tends to be more closely confined near noon. Peak occurrence rates are similar to 30% at energies just below 10 keV. A superposed epoch analysis of 77 coronal mass ejection (CME)-driven storms and 93 high-speed solar wind (HSS)-driven storms shows a relative suppression of the occurrence frequency of positive slopes during the recovery phase. The suppression is particularly long-lived for HSS-driven streams.

AB - The magnetosonic (or ion Bernstein) instability is driven by a positive slope in the ion distribution function perpendicular to the magnetic field at energies above about 1 keV. Fifteen years of multisatellite geosynchronous observations are used to determine the statistical occurrence of ion distributions with positive slopes as a function of energy, local time, geomagnetic activity, and phase of the solar cycle. There is no discernable dependence on phase of the solar cycle, but there are clear dependences on the other parameters. Positive slopes are seen primarily in the energy range between similar to 3 and similar to 24 keV. The peak occurrence of positive slopes is between midmorning and dusk and moves progressively toward earlier local times for higher energies. The occurrence is significantly greater and extends over a broader local time range for low levels of geomagnetic activity than for high activity, for all energies. At high activity levels, the occurrence tends to be more closely confined near noon. Peak occurrence rates are similar to 30% at energies just below 10 keV. A superposed epoch analysis of 77 coronal mass ejection (CME)-driven storms and 93 high-speed solar wind (HSS)-driven storms shows a relative suppression of the occurrence frequency of positive slopes during the recovery phase. The suppression is particularly long-lived for HSS-driven streams.

KW - OUTER RADIATION BELT

KW - ION-CYCLOTRON WAVES

KW - LINEAR DIFFUSION-COEFFICIENTS

KW - WHISTLER-MODE CHORUS

KW - GEOMAGNETIC STORMS

KW - RELATIVISTIC ELECTRONS

KW - RING CURRENT

KW - INNER MAGNETOSPHERE

KW - MAGNETIC STORM

KW - SOLAR-WIND

U2 - 10.1029/2011JA016644

DO - 10.1029/2011JA016644

M3 - Journal article

VL - 116

SP - -

JO - Journal of Geophysical Research

JF - Journal of Geophysical Research

SN - 0148-0227

M1 - A08220

ER -