Protostellar rotation: turbulence and heating of molecular clouds

Journal Article · Sat Jan 15 04:00:00 EST 1983 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/160618· OSTI ID:5911289

Franco, J

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.

• Research Organization: Department of Physics, University of Wisconsin-Madison
• OSTI ID: 5911289
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 264:2; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
640105 -- Astrophysics & Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ANGULAR MOMENTUM
ENERGY LOSSES
GRAVITATIONAL COLLAPSE
INTERSTELLAR GRAINS
LOSSES
MAGNETIC FIELDS
MOTION
NEBULAE
PARTICLES
PROTOSTARS
ROTATION
STAR ACCRETION
STAR EVOLUTION
STELLAR WINDS
TURBULENCE