Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh21b1600b&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SH21B-1600
Physics
7524 Magnetic Fields, 7837 Neutral Particles (2151)
Scientific paper
The distribution of interplanetary magnetic field (IMF) in the distant solar wind and in the heliosheath is of great interest for solar wind (SW) interaction with local interstellar medium (LISM). This is because it is measured by Voyager spacecraft and therefore can be used to tune up theoretical models on the basis of observational data. One of the main difficulties one encounters when modeling IMF is the necessity to resolve the heliospheric current sheet (HCS). The angle between the Sun's rotation and magnetic-dipole axes is never zero, varying from about 8-9 degrees during solar minima to 90 degrees at solar maxima. As a result of Sun's rotation, the distance between two consecutive crossings of the ecliptic plane by the HCS becomes as small as about 3 AU in the supersonic SW and about 1 AU in the inner heliosheath. In this study we investigate HCS evolution in the SW using our global multi-fluid simulations. To achieve desired resolution we use three-dimensional adaptive spherical meshes implemented in the framework of Multi-Scale Fluid-Kinetic Simulation Suite (MS-FLUKSS) - a software package developed with the support of the NASA and NSF grants.
Borovikov S.
Kryukov I.
Pogorelov Nikolai
Zank Gary
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