Dynamical Simulations of Plasmapause Deformations

Pierrard, Viviane; Cabrera, J.

doi:10.1007/s11214-006-5670-3

Cited by 24 publications

(18 citation statements)

References 9 publications

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“…They are formed in the afternoon sector and then rotate eastward with the core of the plasmasphere. Other examples of IMAGE observations during quiet and disturbed periods that have been compared to results of simulations based on the interchange mechanism (IC E5D) have been presented by Pierrard and Cabrera [2005, 2006] and Pierrard [2006].…”

Section: Discussion Of the Resultsmentioning

confidence: 99%

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Influence of the convection electric field models on predicted plasmapause positions during magnetic storms

et al. 2008

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[1] In the present work, we determine how three well documented models of the magnetospheric electric field, and two different mechanisms proposed for the formation of the plasmapause influence the radial distance, the shape and the evolution of the plasmapause during the geomagnetic storms of 28 October 2001 and of 17 April 2002. The convection electric field models considered are: McIlwain's E5D electric field model, Volland-Stern's model, and Weimer's statistical model compiled from low-Earth orbit satellite data. The mechanisms for the formation of the plasmapause to be tested are: (1) the MHD theory where the plasmapause should correspond to the last-closed-equipotential (LCE) or last-closed-streamline (LCS), if the E-field distribution is stationary or timedependent respectively; (2) the interchange mechanism where the plasmapause corresponds to streamlines tangent to a Zero-Parallel-Force surface where the field-aligned plasma distribution becomes convectively unstable during enhancements of the E-field intensity in the nightside local time sector. The results of the different time dependent simulations are compared with concomitant EUV/IMAGE observations when available. The plasmatails or plumes observed after both selected geomagnetic storms are predicted in all simulations and for all E-field models. However, their shapes are quite different depending on the E-field models and the mechanisms that are used. Despite the partial success of the simulations to reproduce plumes during magnetic storms and substorms, there remains a long way to go before the detailed structures observed in the EUV observations during periods of geomagnetic activity can be accounted for very precisely by the existing E-field models. Furthermore, it cannot be excluded that the mechanisms currently identified to explain the formation of ''Carpenter's knee'' during substorm events, will have to be revised or complemented in the cases of geomagnetic storms.Citation: Pierrard, V., G. V. Khazanov, J. Cabrera, and J. Lemaire (2008), Influence of the convection electric field models on predicted plasmapause positions during magnetic storms,

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Section: Discussion Of the Resultsmentioning

confidence: 99%

“…This mechanism has been used in numerical simulations performed by Lemaire [1985, 2000] and by Pierrard and Lemaire [2004]. The positions of the plasmapause predicted by this mechanism with the E5D model have been compared to observations of IMAGE for typical dates [ Pierrard and Cabrera , 2005, 2006; Pierrard , 2006].…”

Section: Dynamical Simulationsmentioning

confidence: 99%

Influence of the convection electric field models on predicted plasmapause positions during magnetic storms

et al. 2008

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“…Plumes are then formed in the afternoon MLT sector and rotate with the Earth [ Spasojević et al , 2003; Pierrard and Lemaire , 2004; Darrouzet et al , 2006]. The results of the model have been compared to recent observations of Cluster and IMAGE [ Pierrard and Cabrera , 2005, 2006; Pierrard , 2006; Darrouzet et al , 2009] and have shown that the model globally reproduces the dynamic features of the plasmasphere.…”

Section: Introductionmentioning

confidence: 99%

The 3D model of the plasmasphere coupled to the ionosphere

Pierrard

Voiculescu

2011

Geophys. Res. Lett.

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[1] The 3D dynamic model of the plasmasphere developed by Pierrard and Stegen (2008) has been coupled with the ionospheric IRI model. In addition to the electron number density, the plasmaspheric model is also developed to include the temperature profiles of the different particles and ion composition at altitudes from 60 to 2000 km. Results of the model for the F region trough are compared with coincident observations of middle and top ionosphere by means of satellite tomography and radar measurements. A good match between the model and observations supports the idea that the present model is useful for investigating physical mechanism involved in the plasmasphere-ionosphere coupling and for acquiring information about the plasmaspheric behaviour based on ionospheric observations. Citation: Pierrard, V., and M. Voiculescu (2011), The 3D model of the plasmasphere coupled to the ionosphere, Geophys. Res. Lett., 38, L12104,

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“…They found that the timescale of the plasmapause response to the IMF is about 30 min in their case studies. Furthermore, Pierrard and Cabrera [2005, 2006] presented the simulations of the plasmapause formation and compared the predicted plasmapause positions with the EUV observations. They remarked the correlation between the inward motion of the plasmapause and the southward turning of the IMF in numerical simulations.…”

Section: Introductionmentioning

confidence: 99%

The plasmapause response to the southward turning of the IMF derived from sequential EUV images

2007

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[1] We statistically examined the plasmapause response to the southward turning of the interplanetary magnetic field (IMF) using sequential global images of the plasmasphere, in order to understand how the convection electric field propagates to the inner magnetosphere. The extreme ultraviolet (EUV) imager on the Imager for Magnetopause-to-Aurora Global Exploration satellite clearly observed inward motion of the plasmapause driven by the southward turning of the IMF. We surveyed the EUV data in the 2000-2001 period and found 16 events. Using the sequential EUV images, we calculated the plasmapause radial velocity, and then estimated the time development of the convection electric field at the plasmapause (E pp ). E pp and the solar wind electric field derived from the measurement by the ACE satellite had very similar variations each other, but there surely was a time lag. Consequently, our research indicates that the plasmapause response to the southward turning of the IMF takes 10-30 min. This timescale suggests that the convection electric field penetrates from the magnetopause to the inner magnetosphere through the ionosphere.

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Dynamical Simulations of Plasmapause Deformations

Cited by 24 publications

References 9 publications

Influence of the convection electric field models on predicted plasmapause positions during magnetic storms

Influence of the convection electric field models on predicted plasmapause positions during magnetic storms

The 3D model of the plasmasphere coupled to the ionosphere

The plasmapause response to the southward turning of the IMF derived from sequential EUV images

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