Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...217..916s&link_type=abstract
Astrophysical Journal, Part 1, vol. 217, Nov. 1, 1977, p. 916-927.
Astronomy and Astrophysics
Astrophysics
56
Galactic Structure, Gas Dynamics, Spiral Galaxies, Star Distribution, Stellar Motions, Density Distribution, Density Wave Model, Fluid Pressure, Orbit Calculation, Viscosity
Scientific paper
The time-dependent response of a ensemble of noninteracting test particles to a rotating oval distortion of a realistic axisymmetric galactic disk is numerically calculated for several assumed values of the distortion angular velocity. The test-particle response is found to be barlike and to strongly reinforce the imposed perturbation if the angular velocity of the distortion permits only one inner Lindblad resonance. The calculations are then repeated, with the mass of each particle distributed over some sufficiently large volume. In such a representation, the test particles become fluid elements in a Lagrangian sense, and an artificial viscosity may be defined in the usual manner. If this bulk viscosity is the only gas dynamical effect considered, the 'gas' responds to the rotating oval distortion by forming a material bar inside the inner resonance and trailing spiral density waves beyond the resonance. It is only the dissipation provided by the artificial viscosity which distinguishes the bar response of the stars from the bar-plus-spiral-density waves of the gas response.
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