Physics
Scientific paper
Oct 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986inpr.conf...38w&link_type=abstract
In its Summer School on Interstellar Processes: Abstracts of Contributed Papers p 38-39 (SEE N87-15043 06-90)
Physics
Cosmic Dust, Grains, Interstellar Matter, Protostars, Star Formation, Stellar Mass, Stellar Mass Accretion, Stellar Models, Graphite, Hydrodynamics, Infrared Radiation, Opacity, Radiation Pressure, Silicates, Stellar Envelopes
Scientific paper
Observational evidence suggests that stars greater than 100 M(solar) exist in the Galaxy and Large Magellanic Cloud (LMC), however classical star formation theory predicts stellar mass limits of only approx. 60 M(solar). A protostellar accretion flow consists of inflowing gas and dust. Grains are destroyed as they are near the central protostar creating a dust shell or cocoon. Radiation pressure acting on the grain can halt the inflow of material thereby limiting the amount of mass accumulated by the protostar. We first consider rather general constraints on the initial grain to gas ratio and mass accretion rates that permit inflow. We further constrain these results by constructing a numerical model. Radiative deceleration of grains and grain destruction processes are explicitly accounted for in an iterative solution of the radiation-hydrodynamic equations. Findings seem to suggest that star formation by spherical accretion requires rather extreme preconditioning of the grain and gas environment.
Cassinelli Joe P.
Wolfire Mark G.
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