Other
Scientific paper
Jun 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.208..687l&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 208, June 1, 1984, p. 687-707. Research supported by th
Other
120
Disk Galaxies, Gravitational Effects, Interstellar Gas, Stellar Motions, Approximation, Molecular Clouds, Orbit Calculation, Orbit Perturbation, Velocity Distribution
Scientific paper
The present calculation of the evolution of the three velocity dispersion components of galactic disk stars, due to the influence of massive gas clouds in circular orbits in the disk, indicates the existence of two evolutionary phases: an initial transient phase, in which the velocity ellipsoid shape assumes its final form as a function of the circular-to-radial epicyclic frequencies' ratio, and then a steady heating phase in which the velocity dispersion of disk stars varies. It is also noted that the amount of stellar heating predicted will be comparable with that observed, provided that cloud masses are near the upper end of the observationally permissible range. The ratio of vertical to horizontal velocity dispersions predicted, however, disagrees with that observed. In light of this, other disk heating mechanisms may be important.
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