Asymmetries of the Venus plasma interaction in a global hybrid simulation (Invited)

Details Asymmetries of the Venus plasma interaction in a global hybrid simulation (Invited) Asymmetries of the Venus plasma interaction in a global hybrid simulation (Invited)

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm33d..02j&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM33D-02

Physics

[2753] Magnetospheric Physics / Numerical Modeling, [2780] Magnetospheric Physics / Solar Wind Interactions With Unmagnetized Bodies, [5443] Planetary Sciences: Solid Surface Planets / Magnetospheres, [6295] Planetary Sciences: Solar System Objects / Venus

Scientific paper

We discuss asymmetries of the Venusian plasma environment and the solar wind induced escape of planetary ions. Venus is a planet with an induced magnetosphere controlled by the the solar wind. Especially, since the solar wind carries the frozen-in interplanetary magnetic field (IMF), a large scale motional electric field is present in the planet's rest frame. The solar wind electric field results in differences between the hemispheres where the electric field is pointing towards the planet and away from the planet. Further, the IMF has usually a significant flow-aligned (Bx) component at Venus. The IMF Bx is related to differences between the hemispheres defined by the direction of the IMF cross-flow component, i.e. the magnetic dawn and dusk. We use the HYB-Venus hybrid simulation to study the asymmetries of the escaping planetary oxygen and hydrogen ions and the draping of the magnetic field lines around the planet. Possible causes for the asymmetries, such as mass-loading of the planetary ions to the magnetosheath flow, the Hall term of the electric field and other kinetic effects, are considered based on the modeling.

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