Dayside magnetopause models

Suvorova, A. V.; Дмитриев, А. В.; Кузнецов, С. Н.

doi:10.1016/s1350-4487(99)00220-6

Cited by 18 publications

(19 citation statements)

References 15 publications

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“…A strong increase of solar wind dynamic pressures to approximately 30 to 40 nPa between 3 and 6 UT caused compression of the magnetosphere with a decrease of the nose magnetopause distance to ~7 Re as estimated using a model [ Kuznetsov et al . ; Suvorova et al ., ]. Maximal storm and auroral activity, as seen in the SYM‐H and AE indices, was observed several hours later between 08 and 14 UT on 27 July.…”

Section: Case Events For Great Electron Enhancementsmentioning

confidence: 97%

TEC evidence for near‐equatorial energy deposition by 30 keV electrons in the topside ionosphere

et al. 2013

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[1] Observations of energetic electrons (10 -300 keV) by NOAA/POES and DMSP satellites at heights <1000 km during the period from 1999 to 2010 allowed finding abnormal intense fluxes of~10 6 -10 7 cm À2 s À1 sr À1 for quasi-trapped electrons appearing within the forbidden zone of low latitudes over the African, Indo-China, and Pacific regions. Extreme fluxes appeared often in the early morning and persisted for several hours during the maximum and recovery phase of geomagnetic storms. We analyzed nine storm time events when extreme electron fluxes first appeared in the Eastern Hemisphere, then drifted further eastward toward the South-Atlantic Anomaly. Using the electron spectra, we estimated the possible ionization effect produced by quasi-trapped electrons in the topside ionosphere. The estimated ionization was found to be large enough to satisfy observed storm time increases in the ionospheric total electron content (TEC) determined for the same spatial and temporal ranges from global ionospheric maps. Additionally, extreme fluxes of quasi-trapped electrons were accompanied by the significant elevation of the low-latitude F-layer obtained from COSMIC/FORMOSAT-3 radio occultation measurements. We suggest that the storm time ExB drift of energetic electrons from the inner radiation belt is an important driver of positive ionospheric storms within low-latitude and equatorial regions.

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Section: Case Events For Great Electron Enhancementsmentioning

confidence: 97%

TEC evidence for near‐equatorial energy deposition by 30 keV electrons in the topside ionosphere

et al. 2013

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“…Location in GSM of geosynchronous and high‐apogee satellites at ~1850 UT on 21 January 2005 in (left) X‐Y plane and (right) X‐Z plane. In the X‐Y plane, the position of bow shock (red curve) and magnetopause (blue curve) are calculated, respectively, by BSV [ Verigin et al ., ] and KS98 [ Suvorova et al ., ] empirical models for the extreme solar wind conditions. Under such conditions, the subsolar bow shock and whole dayside magnetopause are located inside geosynchronous orbit.…”

Section: Geosynchronous Crossings Of the Magnetopause And Bow Shockmentioning

confidence: 99%

Anomalous dynamics of the extremely compressed magnetosphere during 21 January 2005 magnetic storm

et al. 2014

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The dayside magnetosphere and proton radiation belt were analyzed during unusual magnetic storm on 21 January 2005. We have found that from 1712 to 2400 UT, the subsolar magnetopause was continuously located inside geosynchronous orbit due to strong compression. The compression was extremely strong from 1846 to 2035 UT when the dense plasma of fast erupting filament produced the solar wind dynamic pressure that peaked up to > 100 nPa, and during the first time, the upstream solar wind was observed at geosynchronous orbit for almost 2 h. Under the extreme compression, the outer magnetosphere at L > 5 was pushed inward, and the outer radiation belt particles moved earthward, became adiabatically accelerated, and accumulated in the inner magnetosphere at L < 4 that produced the intensified ring current with an exceptionally long lifetime. The observations were compared with predictions of various empirical and first-principles models. All the models failed to predict the magnetospheric dynamics under the extreme compression when the minimal magnetopause distance was estimated to be~3 RE. The inconsistencies might result from distortions of plasma measurements by extreme heliospheric conditions consisting in very fast solar wind streams and intense fluxes of solar energetic particles. We speculated that anomalous dynamics of the magnetosphere could be well described by the models if the He abundance in the solar wind was assumed to be > 20%, which is well appropriate for erupting filaments and which is in agreement with the upper 27% threshold for the He/H ratio obtained from Cluster measurements.

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“…It is shown that r 0 decreases when B Y is increasing or when B Z is southward increasing, and r 0 does not change with the northward B Z . The southward B Z has stronger influences on r 0 than B Y , and the northward B Z does not affect r 0 , which is consistent with empirical models [e.g., Suvorova et al ., , ]. The middle panels show l as the function of B Y and B Z respectively.…”

Section: Magnetopause Surface Functions and Configuration Parametersmentioning

confidence: 99%

The IMF dependence of the magnetopause from global MHD simulations

Liu

Кабин

et al. 2013

JGR Space Physics

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[1] Numerical results from a physics-based global magnetohydrodynamic (MHD) model are used to investigate the controlling effects of the interplanetary magnetic field (IMF) components, B Y and B Z , on the location and shape of the magnetopause. The subsolar magnetopause is identified by using the plasma density and velocity, the cusp by using the current density, and the other area by streamlines and the current density. These data are fitted with a three-dimensional surface function constructed by Liu et al. (2012), which allows description of the cusp geometry as well as the north-south asymmetry and azimuthal asymmetry of the magnetopause. A new parameter which depends on the IMF B Y and B Z is introduced to describe the orientation of the elliptical cross section of the magnetopause. Effects of IMF B Y and B Z on the magnetopause configuration parameters are analyzed, and dependence of the magnetopause parameters in the IMF components are obtained. Magnetopause cross section is found to be largely controlled by the IMF clock angle. The stretch direction of the magnetopause cross section is always near the direction of the IMF but is a little closer to the meridional plane than the IMF. Increasing B Y or B Z increases the eccentricity of the magnetopause cross section. This effect is larger for southward IMF than for the northward IMF, and the stretching effect of B Y is smaller than that of B Z .

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Dayside magnetopause models

Cited by 18 publications

References 15 publications

TEC evidence for near‐equatorial energy deposition by 30 keV electrons in the topside ionosphere

TEC evidence for near‐equatorial energy deposition by 30 keV electrons in the topside ionosphere

Anomalous dynamics of the extremely compressed magnetosphere during 21 January 2005 magnetic storm

The IMF dependence of the magnetopause from global MHD simulations

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