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On the Cooling of Interstellar Matter
Published online by Cambridge University Press: 03 August 2017
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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
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