Star-gas density waves in spiral galaxies

Details Star-gas density waves in spiral galaxies Star-gas density waves in spiral galaxies

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...309..496l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 309, Oct. 15, 1986, p. 496-511.

Other

56

Density Wave Model, Interstellar Gas, Spiral Galaxies, Stellar Motions, Damping, Gas Density, Gas Dynamics, Mass Distribution, Viscosity

Scientific paper

The authors analyze the steady state dynamics of spiral galaxies as a two-component system consisting of stars and gas within the framework of the WKB density wave theory. The gravitational influence of the gas is included for the first time in a steady state calculation. The gas is modeled as an isothermal fluid of interacting gas clouds that satisfy a nonlinear viscous fluid equation. The stellar wave is treated linearly, using stellar dynamic equations. It is shown that gas gravity plays a fundamental role in the dynamics of spiral waves in many galaxies. The strength of the gas gravity is a result of the gas responsiveness, relative to the stars, and is due to the lower random velocities in the former. Gas gravity amplifies the gas response; however, gas gravity actually supresses the tendency of the gas to shock. From a dynamical point of view, the spiral gas gravity can overwhelm pressure and viscous forces. The strong wave damping effects caused by the gas gravity are yet another symptom of the power of the gas gravitational field. Like gas gravity, gas viscosity also causes the gas density profile to become smoother and more symmetrical.

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