Physics
Scientific paper
Aug 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992phdt.........4y&link_type=abstract
Ph.D. Thesis Indiana Univ., Bloomington.
Physics
6
Protostars, Stellar Cores, Stellar Evolution, Stellar Structure, Collapse, Hydrodynamics, Molecular Clouds, Simulation, Stability, Stellar Gravitation, Stellar Mass Accretion, Stellar Rotation
Scientific paper
It is widely believed that young stars (protostars) are formed in dark, dense molecular clouds in which gravitational forces cannot be balanced by gas pressure. Clumps in such clouds may undergo 'inside out' collapse to form central protostellar equilibrium cores. With an initial rotation, the collapsing gas first forms a slowly rotating core. As material with greater specific angular momentum collapses later, an equatorial disk around the core develops. A study of protostellar core models at this stage shows that three important events in the evolution of a protostellar core always occur in the same temporal order. First the core surpasses the limit above which overall uniform rotation is impossible; then the accretion flow streamlines begin to form a massive disk; and finally the star/disk structure becomes unstable to the growth of nonaxisymmetric structures. By means of 3P hydrodynamics simulations, the stability of protostellar cores is further investigated. Rapid exponential growth of nonaxisymmetric structures is detected in a model in which a Keplerian disk has just formed. An m = 1 mode dominates during the evolution. The driving mechanism of the nonaxisymmetric structure appears to be the amplification of density waves. A second-order 3D hydrodynamics code with self-gravity is developed and used for the study of protostellar core stability.
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