P51B-3951:
Response of the Martian environment to solar wind dynamic pressure change
Friday, 19 December 2014
Ronan Modolo1, Francois Leblanc1, Jean-Yves Chaufray2, Shannon Curry3, Ludivine Leclercq4, Gerard Marcel Chanteur5 and Philippe Savoini6, (1)LATMOS Laboratoire Atmosphères, Milieux, Observations Spatiales, Paris Cedex 05, France, (2)LATMOS Laboratoire Atmosphères, Milieux, Observations Spatiales, Guyancourt, France, (3)Space Sciences Laboratory, Berkeley, CA, United States, (4)Université de Versailles St Quentin, paris, CDX, France, (5)Ecole Polytechnique, Palaiseau Cedex, France, (6)Laboratoire de Physique des Plasmas, Saint-Maur Des Fossés Cedex, France
Abstract:
The main structures of the solar wind plasma interaction with the upper atmosphere can be usually described using a steady state picture, however time-dependent effects play important roles. In the last couple of years sophisticated 3D simulation try to address the response of the induced magnetosphere and its escape to different time-dependent drivers. Modolo et al (2012) discussed about timescales required for the induced magnetosphere to recover from an IMF rotation. Ma et al (2013) used time-varying solar wind conditions (density and velocity enhancement) and concluded that the ionospheric/atmospheric system reach a new equilibrium in few hours. We use a 3D parallel multi-species hybrid simulation model to study the response of the induced magnetosphere to a time-varying solar wind dynamic pressure. The hybrid model (Modolo et al, 2014, in prep) includes crustal fields, a ionospheric chemistry scheme and uses a 3D description of the Martian thermosphere (Chaufray et al, 2014) and exosphere (Yagi et al, 2012). The impact of a solar wind dynamic pressure change on plasma boundaries is discussed. A special attention is focused on the time-varying energy deposition in the upper atmosphere by O+ ions precipitation as well as the escape flux of planetary ions.
