Magnetic field disturbances in the sheath region of a super-sonic interplanetary magnetic cloud
It is well-known that interplanetary magnetic clouds can cause strong geomagnetic storms due to the high magnetic field magnitude in their interior, especially if there is a large negative <I>B<sub>z</sub></I> component present. In addition, the magnetic disturbances aroun...
| Main Authors: | , , |
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| Format: | Article |
| Language: | English |
| Published: |
Copernicus Publications
2008-10-01
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| Series: | Annales Geophysicae |
| Online Access: | https://www.ann-geophys.net/26/3153/2008/angeo-26-3153-2008.pdf |
| Summary: | It is well-known that interplanetary magnetic clouds can cause strong
geomagnetic storms due to the high magnetic field magnitude in their
interior, especially if there is a large negative <I>B<sub>z</sub></I> component present. In
addition, the magnetic disturbances around such objects can play an important
role in their "geo-effectiveness". On the other hand, the magnetic and flow
fields in the CME sheath region in front of the body and in the rear of the
cloud are important for understanding both the dynamics and the evolution of
the interplanetary cloud. The "eventual" aim of this work is to calculate the
magnetic field in this CME sheath region in order to evaluate the possible
geo-efficiency of the cloud in terms of the maximum |<I>B<sub>z</sub></I>|-component in this
region. In this paper we assess the potential of this approach by introducing
a model with a simplified geometry. We describe the magnetic field between
the CME shock surface and the cloud's boundary by means of a vector
potential. We also apply our model and present the magnetic field
distribution in the CME sheath region in front of the body and in the rear of
the cloud formed after the event of 20 November 2003. |
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| ISSN: | 0992-7689 1432-0576 |