Erosion of the inner magnetosphere during geomagnetic storms
Using the empirical magnetic field model dependent on the <i>Dst</i> index and solar wind dynamic pressure, we calculated the behaviour of the contour <i>B</i> = <i>B<sub>s</sub></i> in the equatorial plane of the magnetosphere where <i>B<s...
| Main Authors: | , |
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| Format: | Article |
| Language: | English |
| Published: |
Copernicus Publications
1997-12-01
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| Series: | Annales Geophysicae |
| Online Access: | https://www.ann-geophys.net/15/1532/1997/angeo-15-1532-1997.pdf |
| Summary: | Using the empirical magnetic field model
dependent on the <i>Dst</i> index and solar wind dynamic pressure, we calculated
the behaviour of the contour <i>B</i> = <i>B<sub>s</sub></i> in the equatorial
plane of the magnetosphere where <i>B<sub>s</sub></i> is the magnetic field in
the subsolar point at the magnetopause. The inner domain of the magnetosphere
outlined by this contour contains the bulk of geomagnetically trapped particles.
During quiet time the boundary of the inner magnetosphere passes at the distance
~10 R<sub>E</sub> at noon and at ~7 R<sub>E</sub> at midnight. During very
intense storms this distance can be reduced to 4–5 R<sub>E</sub> for all MLT.
The calculation results agree well with the satellite measurements of the
magnetopause location during storms. The ionospheric projection of the <i>B</i> = <i>B<sub>s</sub></i>
contour calculated with the Euler potential technique is close to the
equatorward edge of the auroral oval. |
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| ISSN: | 0992-7689 1432-0576 |