Dynamical stability and evolution of the discs of Sc galaxies

Details Dynamical stability and evolution of the discs of Sc galaxies Dynamical stability and evolution of the discs of Sc galaxies

1997-08-04

arxiv.org/abs/astro-ph/9708028v1

Astronomy and Astrophysics

Astrophysics

Latex, 11 pages, 8 figures, fig.7 available at anonymous ftp server ftp.lsw.uni-heidelberg.de under incoming/svlinden/fig7.ps,

Scientific paper

10.1046/j.1365-8711.1998.01024.x

We examine the local stability of galactic discs against axisymmetric density perturbations with special attention to the different dynamics of the stellar and gaseous components. In particular the discs of the Milky Way and of NGC 6946 are studied. The Milky Way is shown to be stable, whereas the inner parts of NGC 6946, a typical Sc galaxy from the Kennicutt (1989) sample, are dynamically unstable. The ensuing dynamical evolution of the composite disc is studied by numerical simulations. The evolution is so fierce that the stellar disc heats up dynamically on a short time scale to such a degree, which seems to contradict the morphological appearance of the galaxy. The star formation rate required to cool the disc dynamically is estimated. Even if the star formation rate in NGC 6946 is at present high enough to meet this requirement, it is argued that the discs of Sc galaxies cannot sustain such a high star formation rate for longer periods.

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