Physics
Scientific paper
Sep 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989esoc...33...61l&link_type=abstract
ESO Workshop on Low Mass Star Formation and Pre-Main Sequence Objects, p. 61 - 74
Physics
Molecular Clouds: Star Formation, Molecular Clouds: Magnetic Fields, Molecular Clouds: Condensation, Molecular Clouds: Kinematics
Scientific paper
The author discusses the results of 3-D axisymmetric models of the quasistatic condensation of dense cores from a more extended background as the magnetic field is lost by ambipolar diffusion. In addition to magnetic support, the effects of thermal and "turbulent" pressures, with the latter receiving a semi-empirical treatment consistent with observational measurements of nonthermal line widths in molecular clouds are included. The author finds two regimes for the evolution of the cores according to their mass. For a mass greater than an umbral mass, the process of ambipolar diffusion produces a centrally condensed core, that ultimately collapses, from inside out, to form a star. In contrast, a subumbral region evolves towards a stable final configuration where the mean magnetic field asymptotically become uniform and straight with thermal and turbulent pressure providing support against gravity. This region, will not be either dense enough or big enough to excite measurable ammonia emission. Only if the turbulence decays, these type of regions will be able to form stars.
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