Small dense molecular clouds which envelope groups of T-Tauri stars

Details Small dense molecular clouds which envelope groups of T-Tauri stars Small dense molecular clouds which envelope groups of T-Tauri stars

Oct 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978m%26p....19..185l&link_type=abstract

(Conference on Protostars and Planets, Tucson, Ariz., Jan. 3-7, 1978.) Moon and the Planets, vol. 19, Oct. 1978, p. 185-198.

Physics

1

Hydrogen Clouds, Star Clusters, Stellar Envelopes, T Tauri Stars, Ammonia, Gravitational Collapse, Hydroxyl Emission, Molecular Gases, Stellar Evolution, Thermodynamic Equilibrium

Scientific paper

This paper presents radio observations of molecular clouds of OH and NH3 which have linear extents of the order of 1 pc and envelop groups of T Tauri stars whose masses range from about 0.5 to 2 solar masses. The observational results are briefly summarized, and the physical conditions within the clouds are investigated. Consideration of the excitation of the NH3 molecules leads to the conclusion that the molecular hydrogen densities are approximately 4000 per cu cm and the cloud kinetic temperatures are about 20 K. Cloud masses of the order of 100 solar masses are inferred, suggesting that the inward pressure of gravity may be supported by the outward pressure of the moving molecules (i.e., the clouds may be in a state of hydrostatic equilibrium). It is concluded that the formation of the visible T Tauri stars apparently results from fragmentation of a massive cloud followed by the concentration of a small fraction of the cloud mass in a few rapidly collapsing protostars.

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