Statistics – Computation
Scientific paper
Feb 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...156..354m&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 156, no. 1-2, Feb. 1986, p. 354-380. ZWO-supported research.
Statistics
Computation
16
Barred Galaxies, Computational Fluid Dynamics, Gas Flow, Interstellar Gas, Quasi-Steady States, Computational Grids, Convergence, Euler Equations Of Motion, Galactic Structure, Isothermal Processes, Numerical Integration
Scientific paper
An efficient numerical method for the integration of the Euler equations for gas dynamics is presented. The key assumption is the existence of a stationary solution. The several elements of the method, most of which have been described elsewhere, are reviewed in some detail to provide a reference in the astronomical literature and to promote its use in astrophysics. The method is applied to the well-studied problem of the quasi-steady isothermal gas flow in the gravitational potential of a weakly barred galaxy. Convergence on a 64×64 grid typically takes 100 to 300 multigrid cycles for a second-order-accurate solution. Comparison with first-order-accurate solutions shows that second-order schemes are to be preferred, despite their slower convergence. There are two fundamentally different types of quasi-steady solutions, depending on the strength of the bar and the size of the sound speed. Type I has only shocks inside co-rotation. Type II solutions have shocks inside and outside co-rotation. The solutions display strong non-circular motions. It is suggested that the tilted-ring model for the observed neutral-hydrogen velocity fied of disk galaxies may just as well be interpreted as a rotated-ellipse model. A set of edge-on rotation curves is presented that can be compared with those based on neutral-hydrogen observations.
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