Effects of a Local Interstellar and Interplanetary Magnetic Field on the Heliosheath

Details Effects of a Local Interstellar and Interplanetary Magnetic Field on the Heliosheath Effects of a Local Interstellar and Interplanetary Magnetic Field on the Heliosheath

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsh22a..04o&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH22A-04

Physics

2124 Heliopause And Solar Wind Termination, 2134 Interplanetary Magnetic Fields, 2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2164 Solar Wind Plasma

Scientific paper

In this talk we review some of our recent results showing that that an interstellar magnetic field can produce a north/south asymmetry in solar wind termination shock. Using Voyager 1 and 2 measurements, we suggest that the angle α between the interstellar wind velocity and magnetic field is 30 < α < 60°. The distortion of the shock is such that termination shock particles could stream outward along the spiral interplanetary magnetic field connecting Voyager 1 to the shock when the spacecraft was within ~ 2~AU of the shock. The shock distortion is larger in the southern hemisphere, and Voyager 2 could be connected to the shock when it is within ~ 5~AU of the shock, but with particles from the shock streaming inward along the field. Tighter constraints on the interstellar magnetic field should be possible when Voyager 2 crosses the shock in the next several years. We comment additionally on previous work (Opher et al. 2003, 2004) that show that the magnetic field shape dramatically the heliosheath flows. We indicate future directions of research to probe these effects.

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