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Star Formation in Disks

Published online by Cambridge University Press:  30 March 2016

Richard B. Larson
Richard B. Larson*
Affiliation:
Yale University Observatory

Extract

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The basic characteristics of the stellar populations in galaxies are determined by the history of star formation and by the initial mass spectrum with which the stars are formed. Many attempts have been made to model the history of star formation in galaxies using various quasi-theoretical descriptions of star formation, but star formation remains a very poorly understood process and no theoretical understanding with any real predictive power has yet been attained. However, recent work suggests the importance for star formation of some mechanisms that have so far not been very extensively studied, and I shall mention some of these possible processes here, undeveloped though these ideas still are at present.

First, I shall review briefly the observational evidence concerning the history of star formation in galaxies of different Hubble type. Most of the information we have for galaxies other than our own comes from their colors, which can be compared with the predictions of models constructed with various assumed histories of star formation. Ever since the work of Tinsley (1968), it has been clear that most of the observed variation of color with Hubble type can be understood in terms of differing time scales for star formation, the reddest galaxies (E and SO) having formed the bulk of their stars at a relatively early stage, while the much bluer Sc galaxies have formed their stars much more gradually and at a rate that has remained nearly constant up to the present time. Recent studies of normal elliptical galaxies, reviewed by Faber in this volume, confirm that they have no detectable present star formation.

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 6 , 1983 , pp. 191 - 198
Copyright
Copyright © Reidel 1983

References

Butcher, H.R.: 1977, Astrophys. J. 216, 372.Google Scholar
de Vaucouleurs, G.: 1977, in The Evolution of Galaxies and Stellar Populations, ed. Tinsley, B. M. and Larson, R. B., Yale University Observatory, New Haven, p. 43.Google Scholar
Dressier, A.: 1980, Astrophys, J. 236, 351.Google Scholar
Elmegreen, B.G., and Elmegreen, D. M.: 1982, Mon. Not. Roy. Astron. Soc., in press.Google Scholar
Gerola, H., Seiden, P.E., and Schulman, L.S.: 1980, Astrophys. J. 242, 517.Google Scholar
Goldreich, P., and Lynden-Bell, D.: 1965, Mon. Not. Roy. Astron. Soc. 130, 125.Google Scholar
Janes, K., and Adler, D. : 1982, Astrophys. J. Suppl. 49, 425.Google Scholar
Larson, R.B.: 1981, Mon. Not. Roy. Astron. Soc. 194, 809.Google Scholar
Larson, R.B.: 1982, Mon. Not. Roy. Astron. Soc. 200, 159.Google Scholar
Larson, R.B., and Tinsley, B.M.: 1978, Astrophys. J. 219, 46.Google Scholar
Stryker, L.L.: 1981, Ph.D. thesis, Yale University.Google Scholar
Tinsley, B.M.: 1968, Astrophys. J. 151, 547.Google Scholar
Tinsley, B.M., and Larson, R.B.: 1979, Mon. Not. Roy. Astron. Soc. 186, 503.Google Scholar
Toomre, A.: 1981, in The Structure and Evolution of Normal Galaxies, ed. Fall, S. M. and Lynden-Bell, D., Cambridge University Press, p. 111.Google Scholar
Tully, R.B., Mould, J.R., and Aaronson, M.: 1982, Astrophys. J. 257, 527.Google Scholar
Twarog, B.A.: 1980, Astrophys. J. 242, 242.Google Scholar