Cluster-forming Molecular Cloud Cores

Details Cluster-forming Molecular Cloud Cores Cluster-forming Molecular Cloud Cores

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...496l.109m&link_type=abstract

Astrophysical Journal Letters v.496, p.L109

Astronomy and Astrophysics

Astronomy

63

Stars: Formation, Ism: Clouds, Turbulence

Scientific paper

We model a turbulent cloud core ionized by cosmic rays, having Bonnor-Ebert condensations that are both critically stable and cut off from MHD waves in the core. We take these condensations to be the precursors of stars in clusters. The model predicts that such condensations can exist in "massive" cores having a FWHM line width greater than 0.9 km s ^{-1} and a column density greater than 1x1022 cm ^{-2} , as is observed in cluster-forming cores in Perseus, Orion, and Cepheus, but cannot exist in the less turbulent, less opaque "low-mass" cores in Taurus, which have no associated clusters. In cluster-forming cores, these condensations are predicted to have mass ~1 Msolar and radius ~0.03 pc, consistent with the mass and spacing of most young stars in clusters. Such critically stable, cutoff condensations may be identified by their small size and narrow spectral lines, if observed with sufficient sensitivity, spectral resolution, and angular resolution.

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