AffiliationUniv Arizona, Dept Planetary Sci
Interstellar magnetic fields
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PublisherIOP PUBLISHING LTD
CitationE. J. Zirnstein et al 2020 ApJ 888 29
RightsCopyright © 2020. The American Astronomical Society. All rights reserved
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractThe effects of turbulence in the very local interstellar medium (VLISM) have been proposed by Giacalone & Jokipii to be important in determining the structure of the Interstellar Boundary Explorer (IBEX) ribbon via particle trapping by magnetic mirroring. We further explore this effect by simulating the motion of charged particles in a turbulent magnetic field superposed on a large-scale mean field, which we consider to be either spatially uniform or a draped field derived from a three-dimensional magnetohydrodynamic simulation. We find that the ribbon is not double-peaked, in contrast to Giacalone & Jokipii. However, the magnetic mirror force still plays an important role in trapping particles. Furthermore, the ribbon is considerably thicker if the large-scale mean field is draped around the heliosphere. Voyager 1 observations in the VLISM show a turbulent field component that is stronger than previously thought, which we test in our simulation. We find that the inclusion of turbulent fluctuations at scales greater than or similar to 100 au and power consistent with Voyager 1 observations produces a ribbon whose large-scale structure is inconsistent with IBEX observations. However, restricting fluctuations to IBEX observations. Different realizations of turbulence produce different small-scale features (less than or similar to 10 degrees) in the ribbon, but its large-scale structure is robust if the maximum fluctuation size is less than or similar to 50 au. This suggests that the magnetic field structure at scales less than or similar to 50 au is determined by the heliosphere-VLISM interaction and cannot entirely be represented by pristine interstellar turbulence.
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