Derivation of inner magnetospheric electric field (UNH-IMEF) model using Cluster data set

Matsui, H.; Puhl-Quinn, P.; Jordanova, V. K.; Khotyaintsev, Yuri V.; Lindqvist, Per‐Arne; Torbert, R. B.

doi:10.5194/angeo-26-2887-2008

Cited by 21 publications

(28 citation statements)

References 62 publications

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“…Although the L ‐shell range of the storm‐time convection electric field is large (∼3 R E ), the spatial relation between the storm‐time electric field and plasma boundaries in the dusk is similar to subauroral polarization streams (SAPS) [ Anderson et al , 1993]. Statistical studies of electric field distributions during magnetically disturbed periods [ Rowland and Wygant , 1998; Nishimura et al , 2007; Matsui et al , 2008] pointed out existence of the localized electric fields in the inner magnetosphere. However, no clear signature was found corresponding to the outer boundary of intense electric fields, while the inner edge was clearly related to the inner edge of the ring current injection.…”

Section: Discussionmentioning

confidence: 99%

Response of convection electric fields in the magnetosphere to IMF orientation change

et al. 2009

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[1] The transient response of convection electric fields in the inner magnetosphere to southward turning of the interplanetary magnetic field (IMF) is investigated using in-situ electric field observations by the CRRES and Akebono spacecraft. Electric fields earthward of the inner edge of the electron plasma sheet show quick responses simultaneously with change in ionospheric electric fields, which indicates the arrival of the first signal related to southward turning. A coordinated observation of the electric field by the CRRES and Akebono spacecraft separated by 5 R E reveals a simultaneous increase in the dawn-dusk electric field in a wide region of the inner magnetosphere. A quick response associated with the southward turning of the IMF is also identified in in-situ magnetic fields. It indicates that the southward turning of the IMF initiates simultaneous (less than 1 min) enhancements of ionospheric electric fields, convection electric fields in the inner magnetosphere, and the ring or tail current and region 2 FACs. In contrast, a quick response of convection electric fields is not identified in the electron plasma sheet. A statistical study using 161 events of IMF orientation change in 1991 confirms a prompt response within 5 min for 80% of events earthward of the electron plasma sheet, while a large time lag of more than 30 min is identified in electric fields in the electron plasma sheet. The remarkable difference in the response of electric fields indicates that electric fields in the electron plasma sheet are weakened by high conductance in the magnetically conjugated auroral ionosphere.

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Section: Discussionmentioning

confidence: 99%

Response of convection electric fields in the magnetosphere to IMF orientation change

et al. 2009

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“…These two instruments are complementary so that combination of both data enhances data availability. Using these data, we developed an empirically‐based, inner magnetospheric electric field (UNH‐IMEF) model in the equatorial plane [ Puhl‐Quinn et al , ; Matsui et al , ]. This model is useful for comparison with quantities derived from other measurements and/or simulations, such as locations of the inner edges of the electron plasmasheet and the plasmapause, electric fields themselves, etc.…”

Section: Introductionmentioning

confidence: 99%

“…In order to develop the original model [ Matsui et al , ], we mainly used data from Cluster for >5 years. The database was complemented by data from ground radars and an ionospheric spacecraft.…”

Section: Introductionmentioning

confidence: 99%

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Revision of empirical electric field modeling in the inner magnetosphere using Cluster data

et al. 2013

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[1] Using Cluster data from the Electron Drift (EDI) and the Electric Field and Wave (EFW) instruments, we revise our empirically-based, inner-magnetospheric electric field (UNH-IMEF) model at 2 < L < 10. We pick more EFW data during large activities when wake effects are expected to be small. The model is organized by either the interplanetary electric field (IEF) merging with the magnetosphere or the K p index. IEF and K p ranges for which we get potential patterns are, respectively: IEF<0.282 mV/m, 0.2822.662 mV/m;, and K p 4 + . Patterns consist of one set of data and processing for smaller activities, and another for higher activities. As activity increases, the skewed potential contour related to the partial ring current appears on the nightside. With the revised analysis, we find that the skewed potential contours get clearer and potential contours get denser on the nightside and morningside. Since the fluctuating components are not negligible, standard deviations from the modeled values are included in the model. In this study, we perform validation of the derived model more extensively. We find experimentally that the skewed contours are located close to the last closed equipotential, consistent with previous theories. This gives physical context to our model and serves as one validation effort. As another validation effort, the derived results are compared with other models/measurements. From these comparisons, we conclude that our model has some clear advantages over the others.

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“…The sampling interval is 1-4 s, although there are data gaps. We pick good quality data as in a previous study (Matsui et al, 2008). EDI data are suitable to investigate DC components.…”

Section: H Matsui Et Al: Small-scale Fluctuations In Plasmaspheric mentioning

confidence: 99%

Multi-spacecraft observations of small-scale fluctuations in density and fields in plasmaspheric plumes

et al. 2012

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Abstract. In this event study, small-scale fluctuations in plasmaspheric plumes with time scales of ∼10 s to minutes in the spacecraft frame are examined. In one event, plasmaspheric plumes are observed by Cluster, while IMAGE measured density enhancement at a similar location. Fluctuations in density exist in plumes as detected by Cluster and are accompanied by fluctuations in magnetic fields and electric fields. Magnetic fluctuations are transverse and along the direction of the plumes. The E/B ratio is smaller than the Alfvén velocity. Another similar event is briefly presented. We then consider physical properties of the fluctuations. Alfvén mode modulated by the feedback instability is one possibility, although non-local generation is likely. It is hard to show that the fluctuations represent a fast mode. Interchange motion is possible due to the consistency between measurements and expectations. The energy source could be a pressure or density gradient in plasmaspheric plumes. When more events are accumulated so that statistical analysis becomes feasible, this type of study will be useful to understand the time evolution of plumes.

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Derivation of inner magnetospheric electric field (UNH-IMEF) model using Cluster data set

Cited by 21 publications

References 62 publications

Response of convection electric fields in the magnetosphere to IMF orientation change

Response of convection electric fields in the magnetosphere to IMF orientation change

Revision of empirical electric field modeling in the inner magnetosphere using Cluster data

Multi-spacecraft observations of small-scale fluctuations in density and fields in plasmaspheric plumes

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