Heliospheric structure due to magnetic fields and neutral particles from the three- dimensional MHD-kinetic model

Details Heliospheric structure due to magnetic fields and neutral particles from the three- dimensional MHD-kinetic model Heliospheric structure due to magnetic fields and neutral particles from the three- dimensional MHD-kinetic model

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh12b..04p&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH12B-04

Physics

2124 Heliopause And Solar Wind Termination, 2126 Heliosphere/Interstellar Medium Interactions

Scientific paper

Neutral particles play a major role in determining the structure of the outer heliosphere. This is primarily due to the low degree of ionization of the local interstellar medium (LISM). Charge exchange and collisions among atoms and solar wind (SW) ions results in the deceleration of the latter. It is responsible for the birth of pickup ions (PUIs). Secondary neutrals can propagate far upstream of the LISM and modify its parameters. By decreasing the ratio of the SW and LISM ram pressures neutral particles decrease the distance of the heliopause to the Sun, so affecting the location and strength of the SW termination shock (TS). We have shown recently that charge exchange considerably decreases the effect of the interstellar magnetic field (ISMF) on the TS asymmetry -- the phenomenon very well known from ideal MHD simulations performed over the last decade. Since the mean free-path of neutral hydrogen, which is the most important atomic component of the LISM, is comparable with the characteristic lengths (the distances between major discontinuities) of the solar wind (SW) interaction with the LISM, a physically-consistent way to model its behavior is based on the solution of the kinetic Boltzmann equation. An efficient way to solve the Boltzmann equation is provided by stochastic simulations with a direct simulation Monte Carlo method. We apply the Riverside MHD-kinetic model of the heliospheric interface, incorporated into a parallel, adaptive mesh refinement code MS-FLUKSS (Multi-Scale FLUid-Kinetic Simulation Suite) to investigate the the structure of the heliosphere under the assumption that the plane formed by the ISMF and the LISM velocity vectors belongs to the hydrogen deflection plane (HDP) identified in the recent observations from the SOHO SWAN experiment. The actual deflection of the neutral hydrogen flow from its original orientation in the LISM is determined in the presence of the interplanetary magnetic field and ISMF. We present the results in the form of distributions of the plasma and magnetic field quantities in the directions of the Voyager 1 and Voyager 2 spacecraft. Connection of different points on the Voyager trajectories to the TS is investigated. We also analyze the regions of favorable 2-3 kHz radio emission occurring in the outer heliosheath due to charge exchange of the LISM plasma and hot secondary H atoms born in the inner heliosheath.

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