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Smith, C. W.; L'Heureux, J.; Ness, N. F.; Acuña, M. H.; Burlaga, L. F.; Scheifele, J. L.

doi:10.1023/a:1005092216668

Cited by 868 publications

(372 citation statements)

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“…One-minuteresolution solar wind and IMF data are provided by the OMNI Definitive, 1 AU 1 min IMF and Plasma database, courtesy of CDAWeb. Plasma and magnetic field data from the ACE [McComas et al, 1998;Smith et al, 1998;Stone et al, 1998], Wind [Lepping et al, 1995;Ogilvie et al, 1995;Franz et al, 2001], and Geotail [Nishida et al, 1992;Frank et al, 1994;Kokubun et al, 1994] spacecraft were used to produce averaged 1 min resolution plasma and IMF data sets shifted to Earth's bow shock nose using a minimal variance technique [see Weimer et al, 2003]. All solar wind data used in this paper are in GSM coordinates.…”

Section: Methodsmentioning

confidence: 99%

A superposed epoch investigation of the relation between magnetospheric solar wind driving and substorm dynamics with geosynchronous particle injection signatures

et al. 2011

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Section: Methodsmentioning

confidence: 99%

A superposed epoch investigation of the relation between magnetospheric solar wind driving and substorm dynamics with geosynchronous particle injection signatures

et al. 2011

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“…The 1 min resolution solar wind ion data detected by the instrument of Solar Wind Electron, Proton, and Alpha Monitor [McComas et al, 1998] and 16 s resolution magnetic field data acquired by the magnetic field detected instrument of MAG [Smith et al, 1998] on the ACE satellite are collected from the years of 1998 to 2005.…”

Section: Data Descriptionmentioning

confidence: 99%

X lines in the magnetotail for southward and northward IMF conditions

et al. 2015

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Utilizing associated observations of Geotail and ACE satellites from the year of 1998 to 2005, we investigated the X lines in the near‐Earth tail under different interplanetary magnetic field (IMF) conditions. The X lines are recognized by the tailward fast flows with negative Bz. Statistically, the X lines in the tail can be observed for southward as well as northward IMF, but more frequently observed for southward IMF. A typical case on 26 April 2005 showed clear evidence that the X line can occur for northward IMF while the geomagnetic activity is particularly quiet. Further analysis showed that the X line‐related solar wind has stronger Ey and Bz components for southward than northward IMF. In addition, the X line‐related geomagnetic activities are stronger for southward than northward IMF.

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“…Figure 2 shows data from the mag- netic field (MAG) and solar wind (SWEPAM) instruments (Smith et al, 1998;McComas et al, 1998); the data have been time-shifted to the bowshock using a minimum variance analysis technique based upon the work of Weimer et al (2003). The top two panels (a-b) display the IMF B Y and B Z components respectively; B Y was predominantly westward throughout the day except for an hour after midnight and B Z was mostly negative (southward), moving gradually northward as the day progressed.…”

Section: Overviewmentioning

confidence: 99%

Energetic electron precipitation during sawtooth injections

Kavanagh

Donovan

et al. 2007

Ann. Geophys.

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Abstract. We present simultaneous riometer observations of cosmic noise absorption in the nightside and dawn-noon sectors during sawtooth particle injections during 18 April 2002. Energetic electron precipitation (>30 keV) is a feature of magnetospheric substorms and cosmic radio noise absorption acts as a proxy for qualitatively measuring this precipitation. This event provides an opportunity to compare the absorption that accompanies periodic electron injections with the accepted paradigm of substorm-related absorption. We consider whether the absorption is consistent with the premise that these injections are quasi-periodic substorms and study the effects of sustained activity on the level of precipitation. Four consecutive electron injection events have been identified from the LANL (Los Alamos National Laboratory) geosynchronous data; the first two showing that additional activity can occur within the 2-4 h sawtooth periodicity. The first three events have accompanying absorption on the nightside that demonstrate good agreement with the expected pattern of substorm-absorption: discrete spike events with poleward motion at the onset followed by equatorward moving structures and more diffuse absorption, correlated with optical observations. Dayside absorption is linked to gradient-curvature drifting electrons observed at geostationary orbit and it is shown that low fluxes can lead to a lack of absorption as precipitation is suppressed; precipitation begins when the drifting electron flux surpasses some critical level following continuous injections of electrons from the magnetotail. In addition it is shown that the apparent motion of absorption determined from an azimuthal chain of riometers exhibits an acceleration that may be indicative of an energisation of the drifting electron population.

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Cited by 868 publications

References 0 publications

A superposed epoch investigation of the relation between magnetospheric solar wind driving and substorm dynamics with geosynchronous particle injection signatures

A superposed epoch investigation of the relation between magnetospheric solar wind driving and substorm dynamics with geosynchronous particle injection signatures

X lines in the magnetotail for southward and northward IMF conditions

Energetic electron precipitation during sawtooth injections

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