Dense cores in dark clouds. VI - Shapes

Details Dense cores in dark clouds. VI - Shapes Dense cores in dark clouds. VI - Shapes

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...376..561m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 376, Aug. 1, 1991, p. 561-572.

Astronomy and Astrophysics

Astrophysics

231

Dark Matter, Molecular Clouds, Star Formation, Carbon Monoxide, Interstellar Matter, Nebulae

Scientific paper

A comparison is presently conducted between 48 line-intensity maps of 16 dense cores in dark clouds, based on observations in the 13-mm line of NH3 and the 3-mm lines of CS and C(O-18). Core elongation in this sample does not differ significantly between cores with and without embedded stars; elongation appears to be a condition prior to star formation, rather than the consequence of formation. The characteristic elongation of dense cores implies that models of equilibrium between self-gravity and isotropic random motions are incomplete. The observed elongation of dense cores in projection is modeled as arising from a group of either prolate or oblate spheroids.

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