Numerical study of protostellar formation

Details Numerical study of protostellar formation Numerical study of protostellar formation

Mar 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974phdt.........2w&link_type=abstract

Ph.D. Thesis Lawrence Livermore National Lab., CA.

Physics

Interstellar Gas, Mathematical Models, Protostars, Stellar Evolution, Clouds, Hydrodynamic Equations, Magnetohydrodynamics, Thermodynamic Equilibrium

Scientific paper

The earliest phase in the evolution of a star is the formation of a gravitationally bound gas cloud from the interstellar medium. This cloud mass is not, in general, in hydrostatic equilibrium, and will evolve hydrodynamically until equilibrium is attained. The protostellar evolution of these gas clouds is examined. A mathematical model is presented treating all the appropriate physical processes which are important during protostar formation including hydrodynamics, thermodynamics and equation of state, radiation transport, and convective energy transport. Important features of the mathematical model are use of temperature or specific energy density as an independent parameter rather than energy flux or luminosity and inclusion of all time derivatives from the differential equations.

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