Different Mars-solar wind interaction models: implications for ENA imaging

Details Different Mars-solar wind interaction models: implications for ENA imaging Different Mars-solar wind interaction models: implications for ENA imaging

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....5798g&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #5798

Physics

Scientific paper

We present ENA images that are calculated from plasma parameters given by three different simulation models of the interaction between the solar wind and Mars. The ENA images are calculated by combining a model for the ion flow and temperature with a model of the neutral atmosphere using the cross sections for the charge exchange collisions. The three ion models are: an empirical model that is based on Phobos 2 measurements (Kallio, Luhmann, and Barabash, JGR, vol.~102, pp.~22183--22197, 1997); a 3D hybrid simulation (Kallio and Janhunen, JGR, vol.~107, 19 March 2002); and a 3D MHD simulation (Ma, et al., JGR, vol.~107, 09 October 2002). For the empirical and MHD models the ENA images are obtained by integration of the ENA emission along lines of sight to a virtual ENA instrument. The hybrid model generates discrete ENAs through a Monte Carlo procedure. Images of hydrogen ENAs in the empirical model were calculated by Holmström, et al. (M.~Holmström, S.~Barabash, and E.~Kallio, JGR, vol.~107, 09 October 2002.), and images of oxygen ENAs were calculated by Barabash, et al. (S.~Barabash, M.~Holmström, A.~Lukyanov, and E.~Kallio, JGR, vol.~107, 09 October 2002). We examine the differences between the different models and how these differences influence the ENA images. To understand the processes that influence the topology and count rates of ENA images is necessary when interpreting measurements made by ENA instruments in space. This study shows the importance of considering not only the type of simulation model used, but also the proper inclusion of relevant physical phenomena and boundary conditions, when modelling the interaction between planets and the solar wind.

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