Hostname: page-component-cd9895bd7-hc48f Total loading time: 0 Render date: 2024-12-25T03:15:37.785Z Has data issue: false hasContentIssue false
  • English
  • Français

Derivation of the initial luminosity function and the past rate of star formation

Published online by Cambridge University Press:  14 August 2015

M. Schmidt
M. Schmidt*
Affiliation:
Leiden 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.

The initial luminosity function ψ(Mv) was introduced by Salpeter. He assumed uniform formation of stars and derived the initial luminosity function from the observed main-sequence luminosity function and the life time of a star of magnitude Mv on the main sequence. Recently van den Bergh considered the depletion of the interstellar gas by star formation. He found that at a constant rate of star formation the gas in the solar vicinity will be exhausted about 7 × 108 years from now.

Type
II. Theoretical Interpretations of the Hertzsprung-Russell Diagram
Information
Symposium - International Astronomical Union , Volume 10: The Hertzsprung-Russell Diagram , 1959 , pp. 99 - 104
Copyright
Copyright © CNRS 1959 

References

[1] Salpeter, E. E., Ap. J. 121, 161, 1955.CrossRefGoogle Scholar
[2] van den Bergh, S., Zs. f. Ap. 43, 236, 1957.Google Scholar
[3] Walraven, Th., Muller, A. B., Oosterhoff, P. Th., B. A. N. 14, 81 (No. 484) 1958.Google Scholar
[4] Hoyle, F., this symposium, p. 83, 1959.CrossRefGoogle Scholar
[5] Schwarzschild, M., Structure and Evolution of the stars, Princeton University Press, 1958.CrossRefGoogle Scholar
[6] Mathis, J. S., Ap. J. 125, 328, 1957.CrossRefGoogle Scholar
[7] Schwarzschild, M., Howard, R., Harm, R., Ap. J. 125, 233, 1957.CrossRefGoogle Scholar