Injection of relativistic electrons during the giant SSC and the greatest magnetic storm of the space era

Tverskaya, L. V.; Ginzburg, E. A.; Pavlov, N. N.; Svidsky, P. M.

doi:10.1016/s0273-1177(02)00813-x

Cited by 11 publications

(4 citation statements)

References 18 publications

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“…As has been shown in numerous works [see, e.g., Lorentzen et al, 2002;Tverskaya et al, 2003;Obara and Li, 2003;Hudson et al, 2004;Looper et al, 2005;Borovsky and Denton, 2006, and references therein], the interplanetary shocks and pressure jumps in the solar wind can result in the compression of magnetosphere, the formation of new ion and electron radiation belts, and the generation of magnetic storms. Both Sheath and CIR are characterized by high pressure and can have the shock in front of them and, therefore, they can compress magnetosphere and generate storms.…”

Section: Discussionmentioning

confidence: 95%

“…In contrast with data of Tables 1 and 2 Figures One of the possible mechanisms of generation of magnetic storms is formation of new ion and electron radiation belts during magnetosphere compression by interplanetary shocks (see, e.g., [Lorentzen et al, 2002;Tverskaya et al, 2003;Obara and Li , 2003;Hudson et al, 2004;Looper et al, 2005;Borovsky and Denton, 2006], and references therein). Both 1.…”

Section: Relations Between Durations Of Two Phasesmentioning

confidence: 88%

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Influence of the interplanetary driver type on the durations of the main and recovery phases of magnetic storms

et al. 2014

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We study the durations of the main and recovery phases of magnetic storms induced by different types of large‐scale solar‐wind streams (Sheath, magnetic cloud (MC), Ejecta, and corotating interaction region (CIR)) on the basis of OMNI data for 1976–2000. The durations of both the main and recovery phases depend on the type of interplanetary drivers. On average, the duration of the main phase of storms induced by compressed regions (CIR and Sheath) is shorter than for MC and Ejecta, while the duration of the recovery phase of CIR‐ and Sheath‐induced storms is longer. Analysis of the durations of individual storms shows that the durations of the main and recovery phases anticorrelate for CIR‐ and Sheath‐induced storms and there is no dependence between them for (MC + Ejecta)‐induced storms.

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Section: Discussionmentioning

confidence: 95%

Section: Relations Between Durations Of Two Phasesmentioning

confidence: 88%

Influence of the interplanetary driver type on the durations of the main and recovery phases of magnetic storms

et al. 2014

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“…One of the possible mechanisms of generation of magnetic storms is formation of new ion and electron radiation belts during magnetosphere compression by interplanetary shocks [see, e.g., Lorentzen et al , 2002; Tverskaya et al , 2003; Obara and Li , 2003; Hudson et al , 2004; Looper et al , 2005; Borovsky and Denton , 2006, and references therein]. Both Sheath and CIR can have shock in front of them and compress magnetosphere.…”

Section: Discussionmentioning

confidence: 99%

Recovery phase of magnetic storms induced by different interplanetary drivers

Yermolaev¹,

Лодкина²,

Nikolaeva³

et al. 2012

J. Geophys. Res.

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[1] Statistical analysis of Dst behavior during recovery phase of magnetic storms induced by different types of interplanetary drivers is made on the basis of OMNI data in period 1976-2000. We study storms induced by ICMEs (including magnetic clouds (MC) and Ejecta) and both types of compressed regions: corotating interaction regions (CIR) and Sheaths. The shortest, moderate and longest durations of recovery phase are observed in ICME-, CIR-, and Sheath-induced storms, respectively. Recovery phases of strong (Dst min ≤ À100 nT) magnetic storms are well approximated by hyperbolic functions Dst(t) = a/(1 + t/t h ) with constant t h times for each types of drivers while for moderate (À100 < Dst min ≤ À50 nT) storms Dst profile can not be approximated by hyperbolic function with constant t h times because hyperbolic t h times increase with increasing time of recovery phase. Dependence of t h times on types of interplanetary drivers is the same as indicated above. Relation between duration and value Dst min for storms induced by MC and Sheath has 2 parts: module of Dst min and duration correlate at small durations while they anticorrelate at large durations. Obtained results show that recovery phase Dst variations depend on type of interplanetary drivers inducing magnetic storms.

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“…SEPs and strong shocks are both CME‐driven phenomena, and the formation of a new ion radiation belt is therefore a manifestation of CME‐driven storms. The formation of a new inner electron radiation belt has been observed coincident with the compression of the magnetosphere by SSCs [ Blake et al , 1992; Tverskaya et al , 2003; Obara and Li , 2003; Looper et al , 2005]. The mechanism is believed to be a displacement of trapped electrons during a rapid compression and relaxation of the magnetosphere caused by a CME‐driven interplanetary shock [ Li et al , 1993].…”

Section: Differencesmentioning

confidence: 99%

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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Injection of relativistic electrons during the giant SSC and the greatest magnetic storm of the space era

Cited by 11 publications

References 18 publications

Influence of the interplanetary driver type on the durations of the main and recovery phases of magnetic storms

Influence of the interplanetary driver type on the durations of the main and recovery phases of magnetic storms

Recovery phase of magnetic storms induced by different interplanetary drivers

Differences between CME‐driven storms and CIR‐driven storms

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