Heating of galactic discs with realistic vertical potentials

Details Heating of galactic discs with realistic vertical potentials Heating of galactic discs with realistic vertical potentials

Aug 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.257..620j&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 257, no. 4, Aug. 15, 1992, p. 620-632. Research support

Astronomy and Astrophysics

Astronomy

56

Galactic Structure, Molecular Clouds, Stellar Evolution, Stellar Motions, Accretion Disks, Density Distribution, Fokker-Planck Equation, Monte Carlo Method

Scientific paper

The heating of galactic disks through scattering by molecular clouds and spiral waves is investigated by solving the orbit-averaged Fokker-Planck equation by Monte Carlo simulation. The vertical potential in the disk is handled in two ways: (1) by using a fixed and realistic anharmonic potential, or (2) by generating the potential self-consistently, assuming that the disk can be approximated as a 1D self-gravitating layer. The shape of the velocity ellipsoid is found to be little changed from earlier work in which a fixed harmonic potential was used. Self-consistent simulations have been run of coeval and star-forming disks with and without accretion. Predictions of the density distribution and the dependence of the vertical component of the velocity dispersion on height are made. It is found that the assumed strength of spiral heating does not significantly affect the shape of rho(z) or sigma-z(z). The age-velocity relation is derived for the accreting disk and a best fit is made to data from Wielen (1977).

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