Orientation and Magnitude of the Interstellar Magnetic Field from Heliosheath Flows

Details Orientation and Magnitude of the Interstellar Magnetic Field from Heliosheath Flows Orientation and Magnitude of the Interstellar Magnetic Field from Heliosheath Flows

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh32a..04o&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH32A-04

Physics

[2124] Interplanetary Physics / Heliopause And Solar Wind Termination, [2126] Interplanetary Physics / Heliosphere/Interstellar Medium Interactions, [2134] Interplanetary Physics / Interplanetary Magnetic Fields, [2164] Interplanetary Physics / Solar Wind Plasma

Scientific paper

We show that the heliosheath flows can be used as a new and highly important data set to determine the interstellar magnetic field orientation and magnitude. We use a new three-dimensional model that includes both the plasma and the neutral H atoms as well as the interplanetary and interstellar magnetic fields. The field orientation and magnitude that we derive differ substantially from the those previously reported (Opher et al. 2006, 2007). We comment on the consequences of this result on the heliospheric global asymmetries (such as the field-aligned streaming of low energy particles, the distance of the termination shock, and the shape of the heliopause). We comments as well on the inference on the conditions on the local interstellar medium. We study the effect of numerical resolution and non-stationary on the model shock and find them to be negligible. We also comment on the possible effects of the tilt of current sheet, not included currently in the model (which at the time of the termination shock crossings of Voyager 1 and 2 was about 30 degrees). We present a simulation with a scaled down heliosphere which includes a dynamic time dependent current sheet.

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