Constraining the Local Interstellar Magnetic Field Direction from Source Location of the Heliospheric 2-3kHz Radio Emissions

Details Constraining the Local Interstellar Magnetic Field Direction from Source Location of the Heliospheric 2-3kHz Radio Emissions Constraining the Local Interstellar Magnetic Field Direction from Source Location of the Heliospheric 2-3kHz Radio Emissions

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh53b1488o&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH53B-1488

Physics

2124 Heliopause And Solar Wind Termination, 2126 Heliosphere/Interstellar Medium Interactions, 2134 Interplanetary Magnetic Fields, 2144 Interstellar Gas, 2164 Solar Wind Plasma

Scientific paper

Using an MHD model, we have investigated the recent suggestion by Gurnett et al. (2006) that the sources of the heliospheric 2-3~kHz radio detected by Voyager 1 and 2 should be located where the interstellar magnetic field is tangential to the surface of the shock that excites the plasma. Because the field is draped over the heliopause surface that is distorted by the field, we ran models with different interstellar field directions. The best agreement is obtained for an interstellar magnetic field parallel to the plane perpendicular to the galactic plane (PPG) as suggested by Gurnett et al. and having a small angle with respect to the velocity of the interstellar wind. The PPG plane is similar to the plane suggested by Lallement et al. 2005 (differing by 16°) that Opher et al. (2006) showed to be consistent with the streaming directions of energetic particles from the termination shock as observed by Voyager 1 and 2. We suggest the radio source locations can be used to further constraint a more complete model.

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