Hall MHD Study of the Solar wind Interaction with Venus

Details Hall MHD Study of the Solar wind Interaction with Venus Hall MHD Study of the Solar wind Interaction with Venus

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm33d..01n&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM33D-01

Physics

[2780] Magnetospheric Physics / Solar Wind Interactions With Unmagnetized Bodies, [6295] Planetary Sciences: Solar System Objects / Venus

Scientific paper

A multi-species, global, Hall MHD model is used to study the solar wind interaction with Venus ionosphere/atmosphere. This model is based on the numerical model that has been successfully applied to Mars (Ma et al., 2004), with Hall effect included. A self-consistent Venus ionosphere is calculated in the model with three ion species (O+, O2+ and CO2+). The related chemical reactions and collision processes are also considered. Our simulation domain covers the region from 100km altitude to 16 Rv in the tail. An adaptive spherical grid structure is used with radial resolution of about 15 km in the lower ionosphere. Mass-loading effect is examined for both solar maximum and solar minimum conditions. The importance of the Hall effect will be discussed. We also show comparisons between our model results with the magnetic fields observed by the magnetometer carried aboard Venus Express.

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