Collisional Consequences of Big Interstellar Grains

Details Collisional Consequences of Big Interstellar Grains Collisional Consequences of Big Interstellar Grains

Jul 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997dps....29.3605g&link_type=abstract

American Astronomical Society, DPS meeting #29, #36.05; Bulletin of the American Astronomical Society, Vol. 29, p.1045

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Identification by Ulysses of interstellar grains inside the planetary system provides new window for study of the local interstellar medium. Dust particles found by Ulysses and confirmed by Galileo are bigger (3* 10(-13) \ g) than the typical interstellar grains (10(-14) \ g). Recently even bigger (about 10(-7) \ g) interstellar meteors have been identified (Taylor et al., Nature, 380, 323, 1996). The goal of this analysis is the investigation of collisional effects of big interstellar grains. Interstellar dust is conventionally described by the MRN size distribution (Mathis, Rumpl and Nordsieck, ApJ, 217, 105, 1977) ranging from 5 to 250\ nm in size (about 10(-18) to 10(-13) \ g). On the basis of this size distribution Jones et al. (ApJ, 469, 740, 1996) find that collisional shattering is a source of the smallest of these grains, but grains bigger than about 30\ nm are rapidly depleted. In this study it is investigated whether collisions with the newly found bigger particles could provide a source for the classic interstellar grains, thereby, solving the mystery of the rapid destruction times of interstellar grains compared to the transport and injection times of grains into the diffuse interstellar medium.

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