Saturn's magnetosphere interaction with Titan for T5 encounter: 3D hybrid modeling. First results

Details Saturn's magnetosphere interaction with Titan for T5 encounter: 3D hybrid modeling. First results Saturn's magnetosphere interaction with Titan for T5 encounter: 3D hybrid modeling. First results

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p11d1609s&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #P11D-1609

Physics

Plasma Physics

[6281] Planetary Sciences: Solar System Objects / Titan, [7823] Space Plasma Physics / Ionization Processes, [7867] Space Plasma Physics / Wave/Particle Interactions

Scientific paper

Wave-particle interactions play a very important role in the plasma dynamics near Titan: mass loading, excitation of low-frequency waves and formation of the particle velocity distribution function (e.g. ring/shell-like distributions, etc.) The kinetic approach is important for estimating collision processes; e.g., charge exchange. In this report we discuss results of 3D hybrid modeling of the interaction between Saturn's magnetosphere and Titan's atmosphere/ionosphere. The modeling is based on recent analysis of the Cassini Plasma Spectrometer (CAPS) and the Cassini Ion, and Neutral Mass Spectrometer (INMS) measurements during the T5 flyby through Titan's ram-side and polar ionosphere [1,2]. Magnetic field data was used from the MAG instrument [3]. In our model the background ions (O+, H+), all pickup ions, and ionospheric ions are considered as a particles, whereas the electrons are described as a fluid. Inhomogeneous photoionization (in the dayside ionosphere), electron-impact ionization, and charge exchange are included in our model. The temperature of the background electrons and pickup electrons was also incorporated into the generalized Ohm's law. We also take into account collisions between ions and neutrals. In our hybrid simulations we use Chamberlain profiles for the exosphere's components. The moon is considered as a weakly conducting body. Special attention will be paid to comparing the modeling results with a single-fluid multi-species 3D MHD model [4], which included complex chemistry but does not produce finite gyroradius and kinetic effects. References [1] Sittler, E.C., et al., Energy Deposition Processes in Titan's Atmosphere and Its Induced Magnetosphere. In: Titan from Cassini-Huygens, Brown, R.H., Lebreton, J.P., Waite, J.H., Eds., Springer, (Dordrecht, Heidelberg, London, New York), pp. 393-455. [2] Agren, K., et al., On magnetosphere electron impact ionization and dynamics in Titan's ram-side and polar ionosphere -- a Cassini case study, Ann. Geophys., 25, 2359-2369, 2007. [3] Dougherty, M.K., and 12 colleagues, The Cassini magnetic field investigation. Space Sci. Rev., 114 (1-4), 331-383, 2004. [4] Ulusen, D., et al., Investigation of the force balance in Titan ionosphere: Cassini T5 flyby, Icarus, 210, 867-880, 2010.

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