Protostellar rotation - Turbulence and heating of molecular clouds

Details Protostellar rotation - Turbulence and heating of molecular clouds Protostellar rotation - Turbulence and heating of molecular clouds

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...264..508f&link_type=abstract

Astrophysical Journal, Part 1, vol. 264, Jan. 15, 1983, p. 508-516.

Astronomy and Astrophysics

Astrophysics

15

Interstellar Gas, Molecular Clouds, Stellar Evolution, Stellar Rotation, Angular Momentum, Carbon Monoxide, Energy Dissipation, Star Formation Rate, Turbulence

Scientific paper

The formation of rapidly rotating protostellar objects in turbulent and clumpy molecular clouds is analyzed. It is shown that the early dissipation of the protostellar rotational energy via a rotationally driven wind can keep their parent molecular clouds at the observed temperatures and in the observed turbulent state. The model requires a low space density of protostellar shells in order to provide the energy requirements to stabilize molecular clouds against gravitational collapse in regions of star formation. The dependence of this mechanism on the star formation rate suggests that the star formation is self-regulated.

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