Hostname: page-component-77c89778f8-sh8wx Total loading time: 0 Render date: 2024-07-25T03:30:02.147Z Has data issue: false hasContentIssue false
  • English
  • Français

Formation of Spiral Galaxies

Published online by Cambridge University Press:  12 April 2016

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

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Conventionally, two major components of spiral galaxies are distinguished: (1) a “spheroidal component”, which includes the central bulge and the surrounding halo, and (2) a “disc component”, which is basically flat and circular but is often warped at the edges. Other structures, such as bars or rings, may also be present, but they are probably of less fundamental significance for the processes of galaxy formation, and therefore they will not be considered here. The distinction between bulge and disc components corresponds approximately to the classical distinction between Population II, as exemplified by the globular clusters which have a nearly spherical distribution, and Population I, which is confined to the galactic plane and is relatively young and metal-rich. However, unlike the “classical” Population II objects which are old and metal-poor, the inner part of the bulge of our galaxy and of other galaxies is in fact metal-rich, and may even contain some young stars.

Type
Part I: Formation and Evolution of Disc Galaxies
Information
International Astronomical Union Colloquium , Volume 45: Chemical and Dynamical Evolution of our Galaxy , September 1977 , pp. 3 - 10
Copyright
Copyright © Geneva Observatory 1977

References

Audouze, J., and Tinsley, B. M., 1976. Ann. Rev. Astron. Astrophys. 14, 43.Google Scholar
Demarque, P., and McClure, R. D., 1977. The Evolution of Galaxies and Stellar Populations, ed. Tinsley, B. M. and Larson, R. B., p. 199. Yale University Observatory, New Haven.Google Scholar
Eggen, O. J., Lynden-Bell, D., and Sandage, A. R., 1962; Astrophys. J. 136, 748.Google Scholar
Gott, J. R., 1977. Ann. Rev. Astron. Astrophys. 15, in press.Google Scholar
Janes, K. A., 1975. Astrophys. J. Suppl. 29, 161.Google Scholar
Larson, R. B., 1972. Nature 235, 21.Google Scholar
Larson, R. B., 1974. Mon. Not. Roy. Astr. Soc. 166, 585.Google Scholar
Larson, R. B., 1975. Mon. Not. Roy. Astr. Soc. 173, 671.Google Scholar
Larson, R. B., 1976a. Mon. Not. Roy. Astr. Soc. 176, 31.Google Scholar
Larson, R. B., 1976b. Galaxies, Sixth Advanced Course of the Swiss Society of Astronomy and Astrophysics, ed. Martinet, L. and Mayor, M., p. 67. Geneva Observatory.Google Scholar
Larson, R. B., 1978a. J. Computational Physics, in press.Google Scholar
Larson, R. B., 1978b. In preparation.Google Scholar
Oort, J. H., 1970. Astron. Astrophys. 7, 381.Google Scholar
Ostriker, J. P., 1977. The Evolution of Galaxies and Stellar Populations, ed. Tinsley, B. M. and Larson, R. B., p. 369. Yale University Observatory, New Haven.Google Scholar
Ostriker, J. P., and Thuan, T. X., 1975. Astrophys. J. 202, 353.Google Scholar
Rees, M. J., 1977. The Evolution of Galaxies and Stellar Populations, ed. Tinsley, B. M. and Larson, R. B., p. 339. Yale University Observatory, New Haven.Google Scholar
Sancisi, R., 1976. Astron. Astrophys. 53., 159.Google Scholar
Searle, L., 1977. The Evolution of Galaxies and Stellar Populations, ed. Tinsley, B. M. and Larson, R. B., p. 219. Yale University Observatory, New Haven.Google Scholar
Tinsley, B. M., and Larson, R. B., 1978. Astrophys. J., submitted.Google Scholar
Toomre, A., 1977. The Evolution of Galaxies and Stellar Populations, ed. Tinsley, B. M. and Larson, R. B., p. 401. Yale University Observatory, New Haven.Google Scholar