Small-Scale Structure of Low-Density Molecular Gas in Nearby Clouds

Details Small-Scale Structure of Low-Density Molecular Gas in Nearby Clouds Small-Scale Structure of Low-Density Molecular Gas in Nearby Clouds

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..108s&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

Computer Science

Scientific paper

Extensive and high-resolution 12CO J=1--0 observations were carried out toward low-density molecular gas in three high-latitude clouds (MBM 32, MBM 54, and MBM 55) and in the periphery of L1641. We resolved low-density (~102 cm-3) substructures with sizes down to ~ 0.02 pc. Some of them are isolated from the rest of the molecular components, suggesting their (quasi-) stable dynamical state. They are most likely formed through thermal instability in interstellar shocks, and provide a clear case for structure formation not caused by gravitational contraction. We unexpectedly discovered in these high-latitude clouds a number of ``pseudo-outflows'' which have a typical size of ~ 0.05 pc and a typical velocity gradient of ~40 km s-1 pc-1. They lack YSO candidates or H2 v=1--0 S(1) emission features in their vicinity. They are most likely weak shocks excited by collisions of clumps.

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