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On Solar Type Protostars

Published online by Cambridge University Press:  12 April 2016

Karl-Heinz A. Winkler  and
Michael J. Newman
Karl-Heinz A. Winkler
Affiliation:
Lawrence Livermore Lab, Los Alamos Scientific Lab, and Max-Planck-Institut für Physik und Astrophysik
Michael J. Newman
Affiliation:
Los Alamos Scientific Laboratory

Extract

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The formation of a 1 M⊙ protostar in spherical symmetry has been followed in time dependent hydrodynamics with a detailed description of the equation of state and a careful treatment of radiative transport. The comparison of the dynamic evolution with observation is made in terms of the Hertzprung-Russell diagram. It is found that the evolution following from Larson’s initial condition produces quantitatively and qualitatively better agreement than that following from the initial condition of Hayashi, including the first appearance of the object as an infrared source. Of particular importance for a correct physical understanding of the formation process is an adequate description of the accretion shock. Pressure ionization and electron degeneracy effects are of increasing importance for the internal structure of lower mass objects.

Type
I. ID, 2D, and 3D Collapse of Interstellar Clouds
Information
International Astronomical Union Colloquium , Volume 58: Stellar Hydrodynamics , August 1980 , pp. 261 - 266
Copyright
Copyright © Reidel 1980

References

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