Macroscopic turbulence in molecular clouds

Details Macroscopic turbulence in molecular clouds Macroscopic turbulence in molecular clouds

May 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...292l..71s&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 292, May 15, 1985, p. L71-L74.

Statistics

Computation

16

Molecular Clouds, Pre-Main Sequence Stars, Stellar Evolution, Stellar Winds, Computational Astrophysics, Protostars, Spectral Line Width, Stellar Mass Ejection, T Tauri Stars, Turbulence

Scientific paper

The hypothesis that outflows driven by pre-main-sequence stellar winds are driving shells that fragment and energize molecular clouds, sustaining them so that they do not undergo free-fall collapse, leads to predicted correlations between line width, hydrogen density, and clump scale. Both the correlation scaling and normalization are in good accord with the correlations observed over a wide range of cloud scales. Implications are drawn for the efficiency of star formation and for cloud lifetimes.

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