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Title: Trajectories and distribution of interstellar dust grains in the heliosphere

Abstract

The solar wind carves a bubble in the surrounding interstellar medium (ISM) known as the heliosphere. Charged interstellar dust grains (ISDG) encountering the heliosphere may be diverted around the heliopause or penetrate it depending on their charge-to-mass ratio. Here, we present new calculations of trajectories of ISDG in the heliosphere, and the dust density distributions that result. We include up-to-date grain charging calculations using a realistic UV radiation field and full three-dimensional magnetohydrodynamic fluid + kinetic models for the heliosphere. Models with two different (constant) polarities for the solar wind magnetic field (SWMF) are used, with the grain trajectory calculations done separately for each polarity. Small grains a gr ≲ 0.01 μm are completely excluded from the inner heliosphere. Large grains, a gr ≳ 1.0 μm, pass into the inner solar system and are concentrated near the Sun by its gravity. Trajectories of intermediate size grains depend strongly on the SWMF polarity. When the field has magnetic north pointing to ecliptic north, the field de-focuses the grains resulting in low densities in the inner heliosphere, while for the opposite polarity the dust is focused near the Sun. The ISDG density outside the heliosphere inferred from applying the model results tomore » in situ dust measurements is inconsistent with local ISM depletion data for both SWMF polarities but is bracketed by them. Our result points to the need to include the time variation in the SWMF polarity during grain propagation. This provides valuable insights for interpretation of the in situ dust observations from Ulysses.« less

Authors:
 [1];  [2];  [3];  [4];  [4];  [5];  [6]
+ Show Author Affiliations
  1. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
  2. Univ. of Chicago, IL (United States). Dept. of Astronomy and Astrophysics
  3. Dartmouth College, Hanover, NH (United States). Dept. of Physics and Astronomy
  4. Univ. of Alabama, Huntsville, AL (United States). Dept. of Physics and Center for Space Physics and Aeronomic Research
  5. Universities Space Research Association, Moffett Field, CA (United States)
  6. Univ. of Alabama, Huntsville, AL (United States). Dept. of Physics and Center for Space Plasma and Aeronomic Research
Publication Date:
Research Org.:
Univ. of Alabama, Huntsville, AL (United States)
Sponsoring Org.:
USDOE Office of Science (SC), Fusion Energy Sciences (FES)
OSTI Identifier:
1325988
Grant/Contract Number:  
SC0008334
Resource Type:
Accepted Manuscript
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 760; Journal Issue: 1; Journal ID: ISSN 0004-637X
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; dust; extinction; ISM: abundances; sun: heliosphere

Citation Formats

Slavin, Jonathan D., Frisch, Priscilla C., Müller, Hans-Reinhard, Heerikhuisen, Jacob, Pogorelov, Nikolai V., Reach, William T., and Zank, Gary. Trajectories and distribution of interstellar dust grains in the heliosphere. United States: N. p., 2012. Web. doi:10.1088/0004-637X/760/1/46.
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Slavin, Jonathan D., Frisch, Priscilla C., Müller, Hans-Reinhard, Heerikhuisen, Jacob, Pogorelov, Nikolai V., Reach, William T., & Zank, Gary. Trajectories and distribution of interstellar dust grains in the heliosphere. United States. https://doi.org/10.1088/0004-637X/760/1/46
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Slavin, Jonathan D., Frisch, Priscilla C., Müller, Hans-Reinhard, Heerikhuisen, Jacob, Pogorelov, Nikolai V., Reach, William T., and Zank, Gary. Thu . "Trajectories and distribution of interstellar dust grains in the heliosphere". United States. https://doi.org/10.1088/0004-637X/760/1/46. https://www.osti.gov/servlets/purl/1325988.
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@article{osti_1325988,
title = {Trajectories and distribution of interstellar dust grains in the heliosphere},
author = {Slavin, Jonathan D. and Frisch, Priscilla C. and Müller, Hans-Reinhard and Heerikhuisen, Jacob and Pogorelov, Nikolai V. and Reach, William T. and Zank, Gary},
abstractNote = {The solar wind carves a bubble in the surrounding interstellar medium (ISM) known as the heliosphere. Charged interstellar dust grains (ISDG) encountering the heliosphere may be diverted around the heliopause or penetrate it depending on their charge-to-mass ratio. Here, we present new calculations of trajectories of ISDG in the heliosphere, and the dust density distributions that result. We include up-to-date grain charging calculations using a realistic UV radiation field and full three-dimensional magnetohydrodynamic fluid + kinetic models for the heliosphere. Models with two different (constant) polarities for the solar wind magnetic field (SWMF) are used, with the grain trajectory calculations done separately for each polarity. Small grains a gr ≲ 0.01 μm are completely excluded from the inner heliosphere. Large grains, a gr ≳ 1.0 μm, pass into the inner solar system and are concentrated near the Sun by its gravity. Trajectories of intermediate size grains depend strongly on the SWMF polarity. When the field has magnetic north pointing to ecliptic north, the field de-focuses the grains resulting in low densities in the inner heliosphere, while for the opposite polarity the dust is focused near the Sun. The ISDG density outside the heliosphere inferred from applying the model results to in situ dust measurements is inconsistent with local ISM depletion data for both SWMF polarities but is bracketed by them. Our result points to the need to include the time variation in the SWMF polarity during grain propagation. This provides valuable insights for interpretation of the in situ dust observations from Ulysses.},
doi = {10.1088/0004-637X/760/1/46},
journal = {Astrophysical Journal},
number = 1,
volume = 760,
place = {United States},
year = {Thu Nov 01 00:00:00 EDT 2012},
month = {Thu Nov 01 00:00:00 EDT 2012}
}
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    Works referencing / citing this record:

    Momentum transfer from solar wind to interplanetary field enhancements inferred from magnetic field draping signatures
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