Velocity streaming of IRAS main-sequence disk stars and the episodic enhancement of particulate disks by interstellar clouds

Details Velocity streaming of IRAS main-sequence disk stars and the episodic enhancement of particulate disks by interstellar clouds Velocity streaming of IRAS main-sequence disk stars and the episodic enhancement of particulate disks by interstellar clouds

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...388..190w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 388, March 20, 1992, p. 190-195. Research supported by NASA and Louisiana E

Astronomy and Astrophysics

Astronomy

13

A Stars, Main Sequence Stars, Molecular Clouds, Stellar Envelopes, Infrared Astronomy Satellite, Interstellar Matter, Monte Carlo Method

Scientific paper

We have discovered evidence of velocity streaming in a set of nearby main-sequence A-type IRAS disk stars. This conservatively chosen set of the five most significant particulate-disk stars consists of β Pic, α Lyr, α Psa, β Leo, and ζ Lep. Monte Carlo simulations were used to compare the velocity dispersion of this set to the dispersions of sets chosen at random from the remaining 17 main-sequence A stars listed in the Gliese catalog (<22 pc). It was found that dispersion velocities less than those of the particulate-disk star set occurred by chance in only 2% of the cases.
Small dispersion velocities are normally indicative of streaming clusters or young field stars. However, the velocity dispersion of the set of particulate-disk stars is inconsistent with either interpretation. These stars did not originate in the local association but, within velocity uncertainties, their centroid trajectory did pass through a major cloud in the local association which today lies in the general direction of Centaurus We suggest that the streaming is a selection artifact of a model in which observable particulate disks are produced or greatly enhanced by episodic passages through interstellar clouds. The disk area enhancement is due to multiple impact fragmentation of ambient circumstellar grains by interstellar grains.

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