Correlation of Pc5 wave power inside and outside themagnetosphere during high speed streams
R. L. Kessel,Ian R. Mann,Ian R. Mann,Shing F. Fung,David K. Milling,David K. Milling,N. O'Connell +6 more
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In this paper, the authors show a clear correlation between the ULF wave power (Pc5 range) inside and outside the Earth's magnetosphere during high speed streams in 1995.Abstract:
. We show a clear correlation between the ULF wave power (Pc5 range) inside and outside the Earth's magnetosphere during high speed streams in 1995. We trace fluctuations beginning 200RE upstream using Wind data, to fluctuations just upstream from Earth's bow shock and in the magnetosheath using Geotail data and compare to pulsations on the ground at the Kilpisjarvi ground station. With our 5-month data set we draw the following conclusions. ULF fluctuations in the Pc5 range are found in high speed streams; they are non-Alfvenic at the leading edge and Alfvenic in the central region. Compressional and Alfvenic fluctuations are modulated at the bow shock, some features of the waveforms are preserved in the magnetosheath, but overall turbulence and wave power is enhanced by about a factor of 10. Parallel (compressional) and perpendicular (transverse) power are at comparable levels in the solar wind and magnetosheath, both in the compression region and in the central region of high speed streams. Both the total parallel and perpendicular Pc5 power in the solar wind (and to a lesser extent in the magnetosheath) correlate well with the total Pc5 power of the ground-based H-component magnetic field. ULF fluctuations in the magnetosheath during high speed streams are common at frequencies from 1–4mHz and can coincide with the cavity eigenfrequencies of 1.3, 1.9, 2.6, and 3.4mHz, though other discrete frequencies are also often seen. Key words. Interplanetary physics (MHD waves and turbulence) – Magnetospheric physics (solar wind-magnetosphere interactions; MHD waves and instabilities)read more
Citations
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Journal ArticleDOI
Differences between CME‐driven storms and CIR‐driven storms
TL;DR: In this paper, the differences between CME-driven and CIR-driven geomagnetic storms are compared and twenty one differences between the two types of storms are tabulated, including the bow shock, the magnetosheath, the radiation belts, the ring current, the aurora, Earth's plasma sheet, magnetospheric convection, ULF pulsations, spacecraft charging in the magnetosphere, and the saturation of the polar cap potential.
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Magnetospheric ULF Waves: A Review
TL;DR: In this article, the authors reviewed recent developments in these areas and discussed the generation, propagation, and consequences of the ULF wave in the Earth's magnetosphere and on the ground.
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Depleting effects of ICME-driven sheath regions on the outer electron radiation belt
TL;DR: In this paper, the effect of interplanetary coronal mass ejection (ICME)-driven sheath regions on relativistic outer radiation belt electron fluxes was studied.
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Solar wind excitation of Pc5 fluctuations in the magnetosphere and on the ground
TL;DR: In this paper, the authors show that pressure fluctuations, a nearly ubiquitous feature of the solar wind, drive magnetospheric compressional Pc5, whose amplitude and power increase in direct proportion to the amplitude of solar wind pressure fluctuations.
Book ChapterDOI
Response of the Upper/Middle Atmosphere to Coronal Holes and Powerful High‐Speed Solar Wind Streams in 2003
Janet U. Kozyra,G. Crowley,B. A. Emery,Xiaohua Fang,G. Maris,M. G. Mlynczak,Rick J. Niciejewski,Scott Palo,Larry J. Paxton,Cora E. Randall,Pingping Rong,J. M. Russell,W. R. Skinner,Stanley C. Solomon,E. Talaat,Qian Wu,J. Yee +16 more
TL;DR: In this paper, high-speed solar wind streams originating from large coronal holes reached a maximum in 2003 during the descending phase of solar cycle 23, and magnetic activity reached the highest levels of the last four solar cycles.
References
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Journal ArticleDOI
The WIND magnetic field investigation
R. P. Lepping,M. H. Acũna,L. F. Burlaga,William M. Farrell,James A. Slavin,K. H. Schatten,F. Mariani,Norman F. Ness,Fritz M. Neubauer,Y. C. Whang,J. B. Byrnes,R. S. Kennon,P. V. Panetta,John Scheifele,E. M. Worley +14 more
TL;DR: The magnetic field experiment on WIND will provide data for studies of a broad range of scales of structures and fluctuation characteristics of the interplanetary magnetic field throughout the mission, and, where appropriate, relate them to the statics and dynamics of the magnetosphere.
Journal ArticleDOI
Some features of field line resonances in the magnetosphere
TL;DR: In this paper, the authors examined the circumstances under which finite disturbance amplitude solutions of the coupled wave equation can be obtained in the vicinity of the resonant field line, and the relevance of recent experimental work to the problem was pointed out.
Book ChapterDOI
Initial ISEE magnetometer results - Magnetopause observations
TL;DR: The magnetic field profiles across the magnetopause obtained by the ISEE-1 and -2 spacecraft separated by only a few hundred kilometers are examined for four passes as discussed by the authors, during which the magnetosheath field was northward, during one pass it was slightly southward, and in two it was strongly southward.
Introduction to Space Physics
TL;DR: A brief history of solar terrestrial physics can be found in this paper, where the authors describe the solar wind, the solar magnetic field, and the solar ionosphere of outer planets, as well as the aurora and the auroral ionosphere.
Journal ArticleDOI
Turbulence, viscosity, and dissipation in the solar-wind plasma
TL;DR: In this paper, the authors discuss the solar wind magnetic field power spectra and plasma velocity, discussing turbulence, viscosity and dissipation, and discuss the effect of solar wind energy on the environment.
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