Global simulations of gas flow in disc galaxies. I - Response to a spiral density wave

Details Global simulations of gas flow in disc galaxies. I - Response to a spiral density wave Global simulations of gas flow in disc galaxies. I - Response to a spiral density wave

May 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.220..165j&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 220, May 1, 1986, p. 165-183.

Astronomy and Astrophysics

Astronomy

11

Density Wave Model, Disk Galaxies, Galactic Structure, Gas Dynamics, Codes, Density Distribution, Galactic Rotation, Perturbation Theory

Scientific paper

In the present numerical investigation of the gas flow in a simple disk galaxy model with mild logarithmic spiral perturbation in the force field due to a postulated, low amplitude density wave, a two-dimensional finite difference-type code, and one using particles moving in a three-dimensional mesh (where interparticle forces generate pressure effects), are employed to calculate various pattern speeds, pitch angles, and perturbation lengths. Both codes furnish higher dimensionality for tightly wound spirals than many previous studies, and a global picture of gaseous response is obtained which demonstrates some aspects of the behavior expected on the basis of previous, quasi-one-dimensional calculations. In addition, evidence of more complex behavior resulting from the additional degree of freedom in fluid motion is obtained. Reasonably good agreement is obtained between the two codes as to the position and strength of the spiral arms over the first few rotation periods. The models predict a small amplitude modulation along the spiral arms to be rotationally symmetric to a good approximation, allowing a qualitative test of the current conclusions.

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