Spiral heating of galactic discs

Details Spiral heating of galactic discs Spiral heating of galactic discs

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.245..305j&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 245, July 15, 1990, p. 305-317. Research supported by t

Astronomy and Astrophysics

Astronomy

111

Disk Galaxies, Fokker-Planck Equation, Galactic Structure, Molecular Clouds, Monte Carlo Method, Gravitational Fields, Heating, Solar Neighborhood, Spiral Galaxies

Scientific paper

The Fokker-Planck equation that describes the heating of a stellar disk under the combined influence of stochastic spiral structure and giant molecular clouds is solved by Monte Carlo simulation. The velocity ellipsoid near the sun is expected to depend on the relative importance of spiral structure and molecular clouds in the sense that sigma(z)/sigma(R) decreases as clouds become less important. The intensity of stochastic spiral structure near the sun is derived. Velocity distributions in the r- and z-directions are predicted for both a coeval stellar population and a population that grows at a constant rate. The v(z)-distribution of a uniformly growing population is expected to be remarkably Gaussian.

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