Dynamics of the Solar Wind-induced Cusp-associated sputtering emission from the surface of Mercury

Details Dynamics of the Solar Wind-induced Cusp-associated sputtering emission from the surface of Mercury Dynamics of the Solar Wind-induced Cusp-associated sputtering emission from the surface of Mercury

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....12412m&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #12412

Computer Science

Scientific paper

The direct solar wind influx throughout Mercury’s cusps, due to the magnetic reconnection occurring on the dayside magnetopause, is the main plasma source inducing sputtering emission from the surface of the planet. The dynamics of the sputtering emission is firstly determined by the variability of the impinging solar wind as well as the interplanetary magnetic field strength and orientation, especially during strong solar events as CMEs and flares. A second contribution arises from the inhomogeneities of the surface portion that is exposed to the particle bombardment from the cusps: this produces a spatial variability that develops into a temporal variability as the planet rotates with respect to its magnetosphere. Surface features with diverse chemical compositions would lead to a particle release characterised by different relative ratios of elements (like K, Ca, Na, O) that can be measured and used as proxy of the soil properties. Moreover, the cusp-associated sputtering emission is expected to contribute to the refilling of the planet’s exosphere, affecting as well the plasma circulation in Mercury’s magnetosphere. In the present study we model the mentioned effects by means of spatial and temporal animated simulations of the particle flux intensities.

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