Heliospheric Phenomena due to Ion-atom Interactions

Details Heliospheric Phenomena due to Ion-atom Interactions Heliospheric Phenomena due to Ion-atom Interactions

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agusmsh24a..05p&link_type=abstract

American Geophysical Union, Spring Meeting 2009, abstract #SH24A-05

Physics

2124 Heliopause And Solar Wind Termination, 2126 Heliosphere/Interstellar Medium Interactions, 2164 Solar Wind Plasma, 7827 Kinetic And Mhd Theory, 7837 Neutral Particles (2151)

Scientific paper

We review physical phenomena occurring in the outer heliosphere due to the solar wind (SW) interaction with the partially-ionized circum-heliospheric interstellar medium (CHISM) illustrating them by observational data and numerical simulations. In particular, we compare Voyager 1 (V1) and Voyager 2 (V2) observations with the results of our 3D, MHD-neutral model of the SW-CHISM interaction. It is shown that the increase in the interstellar magnetic field (ISMF) strength, although increasing the difference in the heliocentric distance at which V1 and V2 crossed the termination shock (TS), also increases the discrepancy in the SW velocity distributions measured in the spacecraft frames. We show that the gradual decrease in the SW dynamic pressure being observed by Ulysses for more than 3 years is a likely explanation of the above-mentioned 10 AU difference. We discuss the implications of different scenarios resulting in the 2-3 kHz radio emission and their possible consequences for the distribution of radio emission sources. The effect of the solar cycle on the 3D, time-dependent distribution of neutral atoms is analyzed, while taking into account variations in the latitudinal extent of the slow SW and the angle between the Sun's rotation and magnetic axes.

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