Non-recurrent geomagnetic disturbances from high-speed streams

Bobrov, M. S.

doi:10.1016/0032-0633(83)90140-x

Cited by 8 publications

(7 citation statements)

References 5 publications

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“…We include only those CIR events that recur for two or more solar rotation cycles. These events do not include transient stream interaction regions which only can produce very weak geomagnetic activity in most cases [ Bobrov , ]. Figure shows the numbers of CIR and CME events between 2002 and 2007.…”

Section: Methodsmentioning

confidence: 99%

A comparison of the effects of CIR‐ and CME‐induced geomagnetic activity on thermospheric densities and spacecraft orbits: Statistical studies

Chen

Wang

et al. 2014

JGR Space Physics

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Enhanced energy input from the magnetosphere to the upper atmosphere during geomagnetic storms has a profound effect on thermospheric density and consequently near-Earth satellite orbit decay. These geomagnetic storms are caused by two different processes. The first is coronal mass ejections (CMEs) and the second is corotating interaction regions (CIRs). CME-driven storms are characterized by large maximum energy input but relatively short duration, whereas CIR-driven storms have relatively small maximum energy input but are of a considerably longer duration. In this paper we carried out a statistical study to assess the relative importance of each kind of storm to satellite orbital decay. The results demonstrate that CIR storms have a slightly larger effect on total orbital decay than CME storms do in a statistical sense. During the declining phase and the minimum years of a solar cycle, CIR storms occur frequently and quasiperiodically. These storms have a large effect on thermospheric densities and satellite orbits because of their relatively long duration. Thus, it is important to fully understand their behavior and impact.

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Section: Methodsmentioning

confidence: 99%

A comparison of the effects of CIR‐ and CME‐induced geomagnetic activity on thermospheric densities and spacecraft orbits: Statistical studies

Chen

Wang

et al. 2014

JGR Space Physics

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“…The occurrence rate of well‐formed CIR (with 27‐day recurrence) peaks during the late declining phase of the solar cycle [ Mursula and Zeiger , 1996], so storms in the declining phase tend to be CIR driven [ Richardson et al , 2001]. Note that interaction regions (IRs) produced by nonrecurrent high‐speed streams can occur throughout the solar cycle [ Bobrov , 1983; L. Jian, private communication, 2005] and can drive nonrecurring geomagnetic activity throughout the solar cycle [ Richardson et al , 2000], although the geomagnetic events that they drive are weaker than the recurring events of the declining phase [ Bobrov , 1983].…”

Section: Introductionmentioning

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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“…As for the nonrecurring SIR‐driven events, they are even weaker than those driven by CIR (Bobrov, ). Even though the lower Dst limit was set at −300 nT, the actual values of Sym‐H do not descend below −160 nT for the SIR‐induced and −140 nT for the CME‐induced storms of Type 2.…”

Section: Data Subsamplesmentioning

confidence: 99%

Empirical Modeling of the Geomagnetosphere for SIR and CME‐Driven Magnetic Storms

Andreeva

Tsyganenko

2019

JGR Space Physics

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During geomagnetic disturbances, the solar wind arrives in the form of characteristic sequences lasting from tens of hours to days. The most important magnetic storm drivers are the coronal mass ejections (CMEs) and the slow‐fast stream interaction regions (SIRs). Previous data‐based magnetic field models did not distinguish between these types of the solar wind driving. In the present work we retained the basic structure of the Tsyganenko and Andreeva (2015) model but fitted it to data samples corresponding to (1) SIR‐driven storms, (2) CME‐driven storms preceded with a shock ahead of the CME, and (3) CME‐driven storms without such shocks. The storm time dynamics of the model current systems has been represented using the parametrization method developed by Tsyganenko and Sitnov (2005), based on dynamical variables Wi, calculated from concurrent solar wind characteristics and their previous history. The database included observations of THEMIS, Polar, Cluster, Geotail, and Van Allen Probes missions during 155 storms in 1997–2016. The model current systems drastically differ from each other with respect to decay rate and total current magnitudes. During SIR‐induced storms, all current systems saturate, while during CME‐induced disturbances, the saturation occurs only for the symmetric ring current and the tail current. The partial ring current parameters are drastically different between SIR‐ and CME‐induced storm sets. In the case of SIR‐driven storms, the total partial ring current is comparable with symmetric ring current, whereas for all CME‐induced events it is nearly twice higher. The results are compared with GOES 15 magnetometer observations.

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Non-recurrent geomagnetic disturbances from high-speed streams

Cited by 8 publications

References 5 publications

A comparison of the effects of CIR‐ and CME‐induced geomagnetic activity on thermospheric densities and spacecraft orbits: Statistical studies

A comparison of the effects of CIR‐ and CME‐induced geomagnetic activity on thermospheric densities and spacecraft orbits: Statistical studies

Differences between CME‐driven storms and CIR‐driven storms

Empirical Modeling of the Geomagnetosphere for SIR and CME‐Driven Magnetic Storms

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