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Dynamical History of the Solar Neighbourhood

Published online by Cambridge University Press:  14 August 2015

J. P. Vader
J. P. Vader*
Affiliation:
Astronomical Institute of Amsterdam

Extract

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The dynamical evolution of the solar neighbourhood is described by an accretion model in which the gas accretion rate decays exponentially with time. Stars form at a rate proportional to the local gas volume density and their velocity dispersion is increased after birth by star-cloud collisions. The present mass density distribution of stars and of gas perpendicular to the galactic plane (Oort 1965) and the observed increase of stellar velocity dispersion with age (Mayor 1974; Mayor and Martinet 1977) are reproduced for an e-folding time of 3 × 109 y of the gas accretion rate and a characteristic star formation time scale of 2.8 × 109 y.

Type
August 28 Open Clusters
Information
Symposium - International Astronomical Union , Volume 85: Star Clusters , 1980 , pp. 191 - 193
Copyright
Copyright © Reidel 1980 

References

Mayor, M.: 1974, Astron. Astrophys. 32, 327.Google Scholar
Mayor, M. and Martinet, L.: 1977, ibid. 55, 221.Google Scholar
Oort, J.H.: 1965 in Blaauw, A. and Schmidt, M. (eds.) Galactic Structure, University of Chicago Press, Chicago, Chap. 21.Google Scholar
Spitzer, L. and Schwarzschild, M.: 1953, Astrophys. J. 118, 106.Google Scholar
Vader, J.P. and de Jong, T.: 1979, to be published in the Proceedings of the 22nd Liege Symposium on “Les éléments et leurs isotopes dans l'univers”.Google Scholar