Modeling the Motion and Distribution of Interstellar Dust inside the Heliosphere

Abstract

The interaction of dust grains originating from the local interstellar cloud with the environment inside the heliosphere is investigated. As a consequence of this interaction the spatial distribution of interstellar dust grains changes with time. Since dust grains are charged in the interplanetary plasma and radiation environment, the interaction of small grains with the heliosphere is dominated by their coupling to the solar wind magnetic field. The change of the field polarity with the solar cycle imposes a temporal variation of the spatial distribution and the flux of small (radius smaller than $0.4\mu m$) interstellar dust grains in the Solar System, whereas the flux of large grains is constant because of their negligible coupling to the solar wind magnetic field. The flux variation observed by in-situ measurements of the Galileo and Ulysses spacecraft are reproduced by simulating the interaction of interstellar grains with charge-to-mass ratios between $0.5C/k{g}^{-1}$ and $1.4C/kg$ with the interplanetary environment.

18 pages, 9 figures (5 color figures are in separate jpeg-files), 2 tables, to appear in JGR Space physics special issue on interstellar dust and the heliosphere

References in corpus (4)

• Dust in the Local Interstellar Wind
• Aspects of the Mass Distribution of Interstellar Dust Grains in the Solar System from In-Situ Measurements
• Interstellar Dust Inside and Outside the Heliosphere
• Prediction of the In-Situ Dust Measurements of the Stardust Mission to Comet 81P/Wild 2

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