Magnetic Storms at Mercury?

Details Magnetic Storms at Mercury? Magnetic Storms at Mercury?

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufm.p12d0521i&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #P12D-0521

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5719 Interactions With Particles And Fields, 5734 Magnetic Fields And Magnetism, 6235 Mercury

Scientific paper

A three-dimensional MHD code was used to simulate the solar wind interaction of Mercury's magnetosphere with interplanetary magnetic field (IMF) of different orientations. It can be shown that for norht-pointing IMF, the Hermean magnetosphere is nearly closed with the polar cap shrinking to a small area. On the other hand, the boundary of the polar cap expands to mid-latitude region (\sim30 degrees latitude) for south-pointing IMF. Such large changes in the size and morphology of the polar cap in response to directional variations of the IMF could be related to the observed temporal variabilities of the atomic sodium emission on Mercury's disk. That is, the production rate of the sodium atoms could be significantly modulated (i.e., weak for northward IMF and large for sourthward IMF) if solar wind sputtering of the surface material is an important source mechanism of the sodium atoms. Some preliminary results will be given in this presentation.

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