Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...243..168b&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 243, no. 1, March 1991, p. 168-186.
Astronomy and Astrophysics
Astrophysics
6
Protostars, Star Formation, Stellar Mass Accretion, Flow Stability, Optical Thickness, Radiation Pressure, Shock Fronts, Steady Flow, Thermodynamic Properties
Scientific paper
Developments concerning spherically symmetric one-dimensional numerical models of protostellar evolution indicate that steady protostellar accretion flows may be unstable at least at the very early and late accretion stages. A detailed semianalytical analysis of the structure of the relaxation region of steady protostellar accretion shocks with a discontinuous shock front is presented to test the reliability of the codes utilized in the calculations and to clarify the physical situation. Analyzing the structure of steady protostellar accretion flows in detail with their shocks, a fine structuring is found at very small length scales compared to those of the overall problem. An oscillatory instability of the shock front due to critical cooling in the region between shock and core is found. The nonlinear time-dependent radiation hydrodynamic calculations show satisfactory agreement with the linear analysis with regard to eigenfunctions and time scales in all cases examined.
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