Computer Science – Numerical Analysis
Scientific paper
Mar 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983stin...8333809c&link_type=abstract
Presented at the Swiss Society of Astrophysics and Astronomy, Saas Fee, Switzerland, 21-26 Mar. 1983
Computer Science
Numerical Analysis
Conservation Laws, Gravitation, Hydrodynamics, Lagrange Coordinates, Mathematical Models, Computer Techniques, Nonlinearity, Numerical Analysis, Stability, Statistical Distributions, Thermodynamics
Scientific paper
A method for calculating the stability and pulsations of stars which make contact with actual observations of the stellar behavior, in which hydrodynamic calculations are very simple in principle is discussed. Conservation of mass can be accounted for by having mass shells that are fixed with their mass for all time. Motions of these shells are calculated by taking the difference between the external force of gravity and that from the local pressure gradient. The conservation of energy is coupled to this momentum conservation equation to give the current temperatures, densities, pressures, and opacities at the shell centers, as well as the positions, velocities, and accelerations of the mass shell interfaces. Energy flow across these interfaces is calculated from the current conditions, and this energy is partitioned between internal energy and the work done on or by the mass shell. The purely radial case for hydrodynamics because which is useful for stellar pulsation studies is outlined.
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