Modeling Heliospheric Interface: Observational and Theoretical Challenges

Details Modeling Heliospheric Interface: Observational and Theoretical Challenges Modeling Heliospheric Interface: Observational and Theoretical Challenges

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh14a..08p&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH14A-08

Physics

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

Scientific paper

Observational data provided by Voyager 1 and Voyager 2 spacecraft ahead of the heliospheric termination shock (TS) and in the heliosheath require considerate reassessment of theoretical models of the solar wind (SW) interaction with the magnetized interstellar medium (LISM). Contemporary models, although sophisticated enough to take into account kinetic processes accompanying charge exchange between ions and atoms and address the coupling of the interstellar and interplanetary magnetic fields (ISMF and IMF) at the heliospheric interface, are still unable to analyze the effect of non-thermal pick-up ions (PUI's) in the heliosheath. The presence of PUI's undermines the assumption of a Maxwellian distribution of the SW ions. We discuss the ways to improve physical models in this respect. The TS asymmetry observed by Voyagers can be attributed to the combination of 3D, time- dependent behavior of the SW and by the action of the ISMF. It is clear, however, that the ISMF alone can account for the TS asymmetry of about 10 AU only if it is unexpectedly strong (greater than 4 microgauss). We analyze the consequences of such magnetic fields for the neutral hydrogen deflection in the inner heliosphere from its original direction in the unperturbed LISM. We also discuss the conditions for the 2-3 kHz radio emission, which is believed to be generated in the outer heliosheath beyond the heliopause, and analyze possible location of radio emission sources under the assumption of strong magnetic field. The quality of the physical model becomes crucial when we need to address modern observational and theoretical challenges. We compare the plasma, neutral particle, and magnetic field distributions obtained with our MHD-kinetic and 5-fluid models. The transport of neutral particles is treated kinetically in the former and by a multiple neutral-fluid approach in the latter. We also investigate the distribution of magnetic field in the inner heliosheath for large angles between the Sun's rotation and magnetic-dipole axes.

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