Electrodynamics in the duskside inner magnetosphere and plasmasphere during a super magnetic storm on March 13–15, 1989

Shinbori, Atsuki; Nishimura, Y.; Ono, Takayuki; Iizima, M.; Kumamoto, A.; Oya, Hiroshi

doi:10.1186/bf03351843

Cited by 20 publications

(24 citation statements)

References 68 publications

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“…As a result, six million residents in the province of Quebec were left without electrical power for more than 9 h. Furthermore, a low-latitude aurora was visible across the southern United States during the night of March 13 and early hours of March 14 (Allen et al 1989). Although the solar wind information is not available for this period, geospace disturbances during this extreme storm have been studied by using satellite data (e.g., Fujii et al 1992;Greenspan et al 1991;Okada et al 1993;Rasmussen and Greenspan 1993;Rich and Denig 1992;Shinbori et al 2005;Sojka et al 1994) and ground-based ionospheric data (e.g., Batista et al 1991;Hajkowicz 1991;Lakshmi et al 1991;Walker and Wong 1993;Yeh et al 1992).…”

Section: Overview Of the March 13-14 1989 Storm Eventmentioning

confidence: 99%

Estimating the solar wind conditions during an extreme geomagnetic storm: a case study of the event that occurred on March 13–14, 1989

2015

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The solar wind conditions of an extreme geomagnetic storm were examined using magnetic field observations obtained from geosynchronous satellites and the disturbance storm-time (Dst) index. During geosynchronous magnetopause crossings (GMCs), magnetic field variations at the magnetosheath, which is the modulated interplanetary magnetic field (IMF), were observed by geosynchronous satellite. The dawn to dusk solar wind electric field (VB S ) was estimated from the Dst index by using an empirical formula for Dst prediction; these data were then used to estimate the IMF and solar wind speed. This method was applied in the analysis of an extreme geomagnetic storm event that occurred on March 13-14, 1989, for which no direct solar wind information was available. A long duration of the GMC was observed after the second storm sudden commencement (SSC) of this event. The solar flare possibly associated with the second SSC of this storm event was identified as the March 12 M7.3/2B flare. The IMF B z was estimated to be about −50 nT with a solar wind speed of about 960 km/s during the 5 h in which the main phase of the storm rapidly developed, assuming an Alfvén Mach number (M A ) during this period of more than 2.

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Section: Overview Of the March 13-14 1989 Storm Eventmentioning

confidence: 99%

Estimating the solar wind conditions during an extreme geomagnetic storm: a case study of the event that occurred on March 13–14, 1989

2015

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“…Wilson et al (2001) suggested that the electric field associated with the DP2 currents might have contributed to the development of the storm ring current in the inner magnetosphere. Actually, strong convection electric fields have been observed by CRRES and Akebono at L = 2-6 (Wygant et al 1998;Shinbori et al 2005;Nishimura et al 2006). The electric field is as strong as 46 mV/m during the major storm on 13 March, 1989 (Shinbori et al 2005).…”

Section: Stormtime Electric Field and Eej/cejmentioning

confidence: 95%

“…Actually, strong convection electric fields have been observed by CRRES and Akebono at L = 2-6 (Wygant et al 1998;Shinbori et al 2005;Nishimura et al 2006). The electric field is as strong as 46 mV/m during the major storm on 13 March, 1989 (Shinbori et al 2005). The convection electric field penetrates to the equatorial ionosphere, intensifying the EEJ on the dayside (Kikuchi et al 2008).…”

Section: Stormtime Electric Field and Eej/cejmentioning

confidence: 97%

Transmission of the electric fields to the low latitude ionosphere in the magnetosphere-ionosphere current circuit

Kikuchi

Hashimoto

2016

Geosci. Lett.

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The solar wind energy is transmitted to low latitude ionosphere in a current circuit from a dynamo in the magnetosphere to the equatorial ionosphere via the polar ionosphere. During the substorm growth phase and storm main phase, the dawn-to-dusk convection electric field is intensified by the southward interplanetary magnetic field (IMF), driving the ionospheric DP2 currents composed of two-cell Hall current vortices in high latitudes and Pedersen currents amplified at the dayside equator (EEJ). The EEJ-Region-1 field-aligned current (R1 FAC) circuit is completed via the Pedersen currents in midlatitude. On the other hand, the shielding electric field and the Region-2 FACs develop in the inner magnetosphere, tending to cancel the convection electric field at the mid-equatorial latitudes. The shielding often causes overshielding when the convection electric field reduces substantially and the EEJ is overcome by the counter electrojet (CEJ), leading to that even the quasi-periodic DP2 fluctuations are contributed by the overshielding as being composed of the EEJ and CEJ. The overshielding develop significantly during substorms and storms, leading to that the mid and low latitude ionosphere is under strong influence of the overshielding as well as the convection electric fields. The electric fields on the day-and night sides are in opposite direction to each other, but the electric fields in the evening are anomalously enhanced in the same direction as in the day. The evening anomaly is a unique feature of the electric potential distribution in the global ionosphere. DP2-type electric field and currents develop during the transient/short-term geomagnetic disturbances like the geomagnetic sudden commencements (SC), which appear simultaneously at high latitude and equator within the temporal resolution of 10 s. Using the SC, we can confirm that the electric potential and currents are transmitted near-instantaneously to low latitude ionosphere on both day-and night sides, which is explained by means of the light speed propagation of the TM 0 mode waves in the Earth-ionosphere waveguide.© 2016 Kikuchi and Hashimoto. This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made.

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“…In order this mechanism to work, energetic electrons need to be injected into the inner plasmasphere during geomagnetic storms. Storm-time enhanced convection electric fields, which are larger than a few mV/m (Shinbori et al, 2005) may contribute to the injection of energetic particles into the inner plasmasphere and these particles cause a direct generation of fast Z-mode waves through cyclotron-type interactions.…”

Section: Discussionmentioning

confidence: 99%

Statistical studies of fast and slow Z-mode plasma waves in and beyond the equatorial plasmasphere based on long-term Akebono observations

et al. 2006

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In order to investigate spatial and temporal variations of fast and slow Z-mode waves frequently observed in the equatorial plasmasphere, statistical studies have been performed by using plasma wave observation data obtained by the Akebono satellite within a period from 1989 to 1995. It has been clarified that fast and slow Z-mode waves are intensified within ±5• of geomagnetic latitudes in an altitude range from 6000 km to the apogee (10500 km) of the satellite without obvious local time dependence. Long-term averaged intensity of fast Z-mode waves has almost the same orders of magnitude as that of slow Z-mode waves. These results indicate that significant part of fast Z-mode waves are not produced by the linear mode conversion process from slow Z-mode waves, but excited by more direct process. Furthermore, the region of intensified fast and slow Z-mode waves has been spread in a wider geomagnetic latitude range of ±10• during geomagnetic storms. These evidences suggest that one of the possible free energy sources is ring current particles injected into the equatorial region of the plasmasphere during geomagnetic storms.

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Electrodynamics in the duskside inner magnetosphere and plasmasphere during a super magnetic storm on March 13–15, 1989

Cited by 20 publications

References 68 publications

Estimating the solar wind conditions during an extreme geomagnetic storm: a case study of the event that occurred on March 13–14, 1989

Estimating the solar wind conditions during an extreme geomagnetic storm: a case study of the event that occurred on March 13–14, 1989

Transmission of the electric fields to the low latitude ionosphere in the magnetosphere-ionosphere current circuit

Statistical studies of fast and slow Z-mode plasma waves in and beyond the equatorial plasmasphere based on long-term Akebono observations

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