Spectral characteristics of great auroras during two superstorms

Yevlashin, L. S.

doi:10.1016/s1464-1909(00)00065-4

Cited by 1 publication

(2 citation statements)

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“…Great auroras have “high visual brightness with a progression to exceptionally low latitudes” [ Jones , 1992]. An examination of the catalog of great aurora events of Jones [1992], supplemented by Yevlashin [2000], Pallamraju and Chakrabarti [2005], and Mikhalev et al [2004], finds that the great aurora chiefly occur during solar maximum. A display of the solar cycle dependence of great aurora is shown in Figure 14, where the sunspot number is plotted as a function of time and the reported occurrences of great aurora are indicated by the circles.…”

Section: Differencesmentioning

confidence: 99%

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Differences between CME‐driven storms and CIR‐driven storms

2006

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[1] Twenty one differences between CME-driven geomagnetic storms and CIR-driven geomagnetic storms are tabulated. (CME-driven includes driving by CME sheaths, by magnetic clouds, and by ejecta; CIR-driven includes driving by the associated recurring high-speed streams.) These differences involve the bow shock, the magnetosheath, the radiation belts, the ring current, the aurora, the Earth's plasma sheet, magnetospheric convection, ULF pulsations, spacecraft charging in the magnetosphere, and the saturation of the polar cap potential. CME-driven storms are brief, have denser plasma sheets, have strong ring currents and Dst, have solar energetic particle events, and can produce great auroras and dangerous geomagnetically induced currents; CIR-driven storms are of longer duration, have hotter plasmas and stronger spacecraft charging, and produce high fluxes of relativistic electrons. Further, the magnetosphere is more likely to be preconditioned with dense plasmas prior to CIR-driven storms than it is prior to CME-driven storms. CME-driven storms pose more of a problem for Earth-based electrical systems; CIR-driven storms pose more of a problem for space-based assets.Citation: Borovsky, J. E., and M. H. Denton (2006), Differences between CME-driven storms and CIR-driven storms,

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Section: Differencesmentioning

confidence: 99%

“…The sunspot number is plotted as a function of time. Occurrences of great aurora [from Jones , 1992; Yevlashin , 2000; Pallamraju and Chakrabarti , 2005; Mikhalev et al , 2004] are plotted as the circles with diamond centers.…”

Section: Differencesmentioning

confidence: 99%