Propagation And Thermodynamics Of ICMEs In The Heliosphere: Observations And Simulations

Details Propagation And Thermodynamics Of ICMEs In The Heliosphere: Observations And Simulations Propagation And Thermodynamics Of ICMEs In The Heliosphere: Observations And Simulations

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh33b..04l&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH33B-04

Other

7843 Numerical Simulation Studies, 7859 Transport Processes, 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma

Scientific paper

We conduct a statistical study of the propagation and thermodynamics of interplanetary coronal mass ejections (ICMEs) in the heliosphere. We base this study on a comprehensive survey of ICMEs from 0.3 to 30 AU observed at Helios 1 and 2, Ulysses, Wind and ACE, and Voyager 2 (Liu et al. 2004; Wang et al. 2004). We find that the radial width of ICMEs increases with distance out to 10-15 AU and then stays roughly constant; the radial width of near-Earth ICMEs has a solar cycle dependence, with a mean value of 0.34 AU. The expansion speed decreases very slowly, suggestive of a quasi-equilibrium expansion. The expansion is governed by a polytrope with γ = 1.1-1.3, indicating continuous heating in the ICME plasma. Coulomb collisions between alpha particles and protons are shown to play an important role in the heating process within ICMEs; other possible energy sources including heat flux electrons and dissipation of magnetic fluctuations are also investigated. A 1D MHD model including pickup ions is used to simulate the dynamical expansion of ICMEs with diverse artificial inputs at 1 AU; preliminary results predict that ICMEs over-expand, with maximum width near 5 AU. We will compare the model results and observations.

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