Dust in the Local Interstellar Wind

Details Dust in the Local Interstellar Wind Dust in the Local Interstellar Wind

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...193.6523f&link_type=abstract

American Astronomical Society, 193rd AAS Meeting, #65.23; Bulletin of the American Astronomical Society, Vol. 31, p.661

Astronomy and Astrophysics

Astronomy

2

Scientific paper

Observations by the Ulysses and Galileo satellites of interstellar dust within the heliosphere are compared with the properties of interstellar dust inferred from measurements of nearby stars, after applying plasma-dust interaction models to correct for the exclusion of small (radius <0.1 μ m) charged grains by the heliopause and solar wind plasmas. Observed enhanced abundances of refractory elements in the surrounding cloud are modeled using velocity-dependent grain destruction by interstellar shocks, so that interstellar absorption data towards nearby stars indicate that the cloud surrounding the solar system has been shocked by a shock with velocity 150 km/s. The gas-to-dust mass ratios implied by the in situ data are at least a factor of three smaller than values inferred from astronomical data for the surrounding cloud if solar reference abundances are assumed, and the discrepancy becomes larger if B-star references are assumed instead. Possible explanations for this anomaly include the presence of an additional population of grains which has not yet exchanged atoms with the gas phase, such as swept up stardust or grains in the molecular clouds from which the surrounding interstellar material emerged. Interstellar grain properties are compared briefly with presolar grains embedded in meteorites.

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