Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992pasj...44..601k&link_type=abstract
PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 44, no. 6, p. 601-611.
Astronomy and Astrophysics
Astronomy
10
Equations Of Motion, Galactic Clusters, Molecular Clouds, Stellar Structure, Velocity Distribution, Gas Dynamics, Three Dimensional Models
Scientific paper
The evolution of the velocity dispersion of disk stars due to gravitational scattering by giant molecular clouds (GMCs) is studied here by 3D calculations. The evolution of the velocity dispersion can be divided into two phases. In the first phase, where the relative motion is dominated by the shear velocity, the planar components of the velocity dispersion evolve as the square root of the age of the stars t, while the vertical component evolves as the exp(t). After the velocity dispersions exceeds a characteristic shear velocity, the second phase starts in which all the components increase as t exp 1/4. In the solar neighborhood the ratios among the velocity dispersion component converge in a way that agrees well with observations. The observed magnitude of the velocity dispersion of nearby stars can be explained except for stars older than 5 Gyr if the GMC cluster into complexes of masses about 10 exp 7 solar masses.
Ida Shigeru
Kokubo Eiichiro
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