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On the Cooling of Interstellar Matter

Published online by Cambridge University Press:  03 August 2017

E. Schatzman
E. Schatzman*
Affiliation:
Institut d'Astrophysique, Paris, France

Extract

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We shall not discuss here in detail the problem of the temperature equilibrium of interstellar matter. Some improvement of our knowledge has been effected by Seaton's results concerning the collisional cross sections of the ions C+, Si+, Fe+, which are important for the temperature equilibrium of the HI regions, and by his results concerning the excitation of the forbidden lines in gaseous nebulae.

Type
Part IV: Cooling and Condensation of Interstellar Matter
Information
Symposium - International Astronomical Union , Volume 8: Cosmical Gas Dynamics , July 1958 , pp. 1009 - 1011
Copyright
Copyright © American Physical Society 1958 

References

1 Seaton, M. J., Ann. Astrophys. 18, 188 (1955).Google Scholar

2 Seaton, M. J., Proc. Roy. Soc. (London) A218, 400 (1953).Google Scholar

3 Spitzer, L. Jr., Astrophys. J. 120, 1 (1954); Spitzer, L. Jr., and Savedoff, M., Astrophys. J. 111, 593 (1950).Google Scholar

4 Kahn, F. D., Gas Dynamics of Cosmic Clouds , edited by van de Hulst, H. C. and Burgers, J. M. (North-Holland Publishers, Amsterdam, the Netherlands, 1955), p. 60.Google Scholar

5 Zanstra, H., Gas Dynamics of Cosmic Clouds , edited by van de Hulst, H. C. and Burgers, J. M. (North-Holland Publishers, Amsterdam, the Netherlands, 1955), p. 70.Google Scholar