Penetration of the solar wind electric field into the magnetosphere/ionosphere system

Kelley, M. C.; Makela, J. J.; Chau, Jorge L.; Nicolls, M. J.

doi:10.1029/2002gl016321

Cited by 244 publications

(318 citation statements)

References 9 publications

(16 reference statements)

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“…Koga et al (2011) concluded that there is an efficient coupling of the IEF and the equatorial ionosphere during a HILDCAA event. Wei et al (2008) suggested that the interplanetary electric field (IEF) penetrates into the equatorial ionosphere during HILDCAA events via short-time (<3 h) dawn-dusk IEF pulses without shielding (see also Kelley et al, 2003, for details on the physical mechanism). We suggest that HILDCAA with extended Alfvénic wave trains and southward excursions of IMF B z could drive observed global dayside VTEC (Fig.…”

Section: Discussionmentioning

confidence: 99%

“…The PPEF mechanism was originally invoked to explain extreme dayside VTEC increases and ionosphere uplifts during large geomagnetic storms around solar maximum (Tsurutani et al, 2004bMannucci et al, 2005;Verkhoglyadova et al, 2006. Kelley et al (1979Kelley et al ( , 2003 first noted similar occurrences with substorms. According to this mechanism, the IEF E y component, if directed in a dawn-to-dusk direction, can cause a dayside ionospheric uplift.…”

Section: Discussionmentioning

confidence: 99%

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Variability of ionospheric TEC during solar and geomagnetic minima (2008 and 2009): external high speed stream drivers

et al. 2013

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We study solar wind–ionosphere coupling through the late declining phase/solar minimum and geomagnetic minimum phases during the last solar cycle (SC23) – 2008 and 2009. This interval was characterized by sequences of high-speed solar wind streams (HSSs). The concomitant geomagnetic response was moderate geomagnetic storms and high-intensity, long-duration continuous auroral activity (HILDCAA) events. The JPL Global Ionospheric Map (GIM) software and the GPS total electron content (TEC) database were used to calculate the vertical TEC (VTEC) and estimate daily averaged values in separate latitude and local time ranges. Our results show distinct low- and mid-latitude VTEC responses to HSSs during this interval, with the low-latitude daytime daily averaged values increasing by up to 33 TECU (annual average of ~20 TECU) near local noon (12:00 to 14:00 LT) in 2008. In 2009 during the minimum geomagnetic activity (MGA) interval, the response to HSSs was a maximum of ~30 TECU increases with a slightly lower average value than in 2008. There was a weak nighttime ionospheric response to the HSSs. A well-studied solar cycle declining phase interval, 10–22 October 2003, was analyzed for comparative purposes, with daytime low-latitude VTEC peak values of up to ~58 TECU (event average of ~55 TECU). The ionospheric VTEC changes during 2008–2009 were similar but ~60% less intense on average. There is an evidence of correlations of filtered daily averaged VTEC data with Ap index and solar wind speed. We use the infrared NO and CO2 emission data obtained with SABER on TIMED as a proxy for the radiation balance of the thermosphere. It is shown that infrared emissions increase during HSS events possibly due to increased energy input into the auroral region associated with HILDCAAs. The 2008–2009 HSS intervals were ~85% less intense than the 2003 early declining phase event, with annual averages of daily infrared NO emission power of ~ 3.3 × 1010 W and 2.7 × 1010 W in 2008 and 2009, respectively. The roles of disturbance dynamos caused by high-latitude winds (due to particle precipitation and Joule heating in the auroral zones) and of prompt penetrating electric fields (PPEFs) in the solar wind–ionosphere coupling during these intervals are discussed. A correlation between geoeffective interplanetary electric field components and HSS intervals is shown. Both PPEF and disturbance dynamo mechanisms could play important roles in solar wind–ionosphere coupling during prolonged (up to days) external driving within HILDCAA intervals

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Variability of ionospheric TEC during solar and geomagnetic minima (2008 and 2009): external high speed stream drivers

et al. 2013

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“…The time scale for the shielding processes is typically less than one hour (Kikuchi et al 2000;Peymirat et al 2000) but subject to magnetospheric conditions (Senior and Blanc 1984;. During the main phase of a geomagnetic storm, the penetration electric field is sometimes observed to last for several hours without decay (Kelley et al 2003;Huang et al 2005aHuang et al , 2005b.…”

Section: Storm Effectmentioning

confidence: 99%

Sq and EEJ—A Review on the Daily Variation of the Geomagnetic Field Caused by Ionospheric Dynamo Currents

2016

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A record of the geomagnetic field on the ground sometimes shows smooth daily variations on the order of a few tens of nano teslas. These daily variations, commonly known as Sq, are caused by electric currents of several μA/m 2 flowing on the sunlit side of the Eregion ionosphere at about 90-150 km heights. We review advances in our understanding of the geomagnetic daily variation and its source ionospheric currents during the past 75 years. Observations and existing theories are first outlined as background knowledge for the nonspecialist. Data analysis methods, such as spherical harmonic analysis, are then described in detail. Various aspects of the geomagnetic daily variation are discussed and interpreted using these results. Finally, remaining issues are highlighted to provide possible directions for future work.

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“…Obayashi (1967), Nishida (1968), and Kelley et al (1979Kelley et al ( , 2003 have reported strong ionospheric effects associated with magnetospheric substorms. These effects are explained by the appearance of dawn-to-dusk electric fields in the dayside near-equatorial ionosphere which has received the name ''prompt penetrating electric fields'' or PPEFs.…”

Section: Introductionmentioning

confidence: 99%

Extreme changes in the dayside ionosphere during a Carrington-type magnetic storm

Tsurutani

Verkhoglyadova

Mannucci

et al. 2012

J. Space Weather Space Clim.

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It is shown that during the 30 October 2003 superstorm, dayside O + ions were uplifted to DMSP altitudes (~850 km). Peak densities were~9 · 10 5 cm À3 during the magnetic storm main phase (peak Dst = À390 nT). By comparison the 1-2 September 1859 Carrington magnetic storm (peak Dst estimated at À1760 nT) was considerably stronger. We investigate the impact of this storm on the low-to mid-latitude ionosphere using a modified version of the NRL SAMI2 ionospheric code. It is found that the equatorial region (LAT = 0°± 15°) is swept free of plasma within 15 min (or less) of storm onset. The plasma is swept to higher altitudes and higher latitudes due to E · B convection associated with the prompt penetration electric field. Equatorial Ionization Anomaly (EIA) O + density enhancements are found to be located within the broad range of latitudes~± (25°-40°) at~500-900 km altitudes. Densities within these peaks are~6 · 10 6 oxygen ions-cm À3 at~700 km altitude, approximately +600% quiet time values. The oxygen ions at the top portions (850-1000 km) of uplifted EIAs will cause strong low-altitude satellite drag. Calculations are currently being performed on possible uplift of oxygen neutrals by ion-neutral coupling to understand if there might be further significant satellite drag forces present.

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Penetration of the solar wind electric field into the magnetosphere/ionosphere system

Cited by 244 publications

References 9 publications

Variability of ionospheric TEC during solar and geomagnetic minima (2008 and 2009): external high speed stream drivers

Variability of ionospheric TEC during solar and geomagnetic minima (2008 and 2009): external high speed stream drivers

Sq and EEJ—A Review on the Daily Variation of the Geomagnetic Field Caused by Ionospheric Dynamo Currents

Extreme changes in the dayside ionosphere during a Carrington-type magnetic storm

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