Мақола

Dust in the Local Interstellar Wind

P. C. FrischDepartment of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637J. DorschnerJohannes GeissInternational Space Science Institute, Bern, SwitzerlandJ. Mayo GreenbergLeiden Observatory Laboratory, Postbus 9504, 2300 RA Leiden, The NetherlandsE. GrünMax-Planck-Institut für Kernphysik, Heidelberg, GermanyMarkus LandgrafCurrent address: Johnson Space Center, Houston, TX 77058P. HöppeMax-Planck-Institut für Chemistry, Cosmochemistry Department, P.O. Box 3060, D-55020 Mainz, GermanyAnthony P. JonesInstitut d’Astrophysique Spatiale, Université Paris XI, Bâtiment 121, 91405 Orsay Cedex, FranceWolfgang KrätschmerMax-Planck-Institut für Kernphysik, Heidelberg, GermanyT. LindeCurrent address: Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637Gregor E. MorfillMax-Planck-Institut für extraterrestrische Physik, 85740 Garching, GermanyW. T. ReachInfrared Processing and Analysis Center, California Institute of Technology, Mail Stop 100-22, Pasadena, CA 91125Jonathan D. SlavinCurrently at Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637. Also University of California, Space Sciences Laboratory, Berkeley, CA 94720. Postal address: NASA/Ames Research Center, MS 245-3, Moffett Field, CA 94035-1000J. ŠvestkaAdolf N. WittRitter Astrophysical Research Center, University of Toledo, Toledo, OH 43606G. P. ZankBartol Research Institute, University of Delaware, Newark, DE 19716

1999en

ABI

Аннотация

The gas-to-dust mass ratios found for interstellar dust within the Solar System, versus values determined astronomically for the cloud around the Solar System, suggest that large and small interstellar grains have separate histories, and that large interstellar grains preferentially detected by spacecraft are not formed exclusively by mass exchange with nearby interstellar gas. Observations by the Ulysses and Galileo satellites of the mass spectrum and flux rate of interstellar dust within the heliosphere are combined with information about the density, composition, and relative flow speed and direction of interstellar gas in the cloud surrounding the solar system to derive an in situ value for the gas-to-dust mass ratio, $R_{g/d} = 94^{+46}_{-38}$. Hubble observations of the cloud surrounding the solar system yield a gas-to-dust mass ratio of Rg/d=551+61-251 when B-star reference abundances are assumed. The exclusion of small dust grains from the heliosheath and heliosphere regions are modeled, increasing the discrepancy between interstellar and in situ observations. The shock destruction of interstellar grains is considered, and comparisons are made with interplanetary and presolar dust grains.

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DOI: 10.1086/307869

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