On the nonlinear time development of gas flow in spiral density waves

Details On the nonlinear time development of gas flow in spiral density waves On the nonlinear time development of gas flow in spiral density waves

Jan 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...195...61w&link_type=abstract

Astrophysical Journal, vol. 195, Jan. 1, 1975, pt. 1, p. 61-73.

Astronomy and Astrophysics

Astrophysics

60

Density Distribution, Galactic Structure, Gas Flow, Interstellar Gas, Time Dependence, Equations Of State, Flow Distribution, Galactic Rotation, Gravitational Effects, Harmonic Analysis, Spiral Galaxies

Scientific paper

Time-dependent calculations of the interstellar gas flow in a tightly wound spiral density wave have been performed. The gravitational potential of the gas is ignored, and the flow development is driven by the gravitational potential of the stars. For sufficiently large wave amplitudes, shocks form within one or two transits of the gas through the spiral pattern. The mechanism for steepening of the wave form is discussed by analyzing the roles played by terms in the flow equations as the flow develops. The dependence of the final, steady flow upon the wave amplitude is also investigated. The behavior of the flow is discussed for various pattern speeds in the context of ultraharmonic resonance. Because of the numerical viscosity, only a resonance of the second harmonic component is found, and no secondary shocks develop. Thus, unless self-gravity of the gas is important, explanation of spiral arm spurs in terms of ultraharmonic resonance is not possible if the gas has turbulence on scales of several parsecs (corresponding to the scale of the mesh spacing).

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