Hostname: page-component-78c5997874-mlc7c Total loading time: 0 Render date: 2024-11-02T22:40:14.157Z Has data issue: false hasContentIssue false
  • English
  • Français

Hot Gas in Galactic Haloes and Winds

Published online by Cambridge University Press:  30 March 2016

Lennox L. Cowie
Lennox L. Cowie*
Affiliation:
Princeton University

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.

At this time we have no direct evidence for the presence of hot gaseous haloes or winds associated with galaxies. We do know that hot gas exists in conjunction with cold gas in the disks of the spirals and that this gas is hot enough to form a substantial corona. There are also a number of indirect observations which would suggest that hot gas flows and possibly bound hot gas occur in both elliptical and spiral galaxies.

In the case of elliptical galaxies the expected accumulated mass loss from the stars is not observed. Typical upper limits to the mass of cold gas at less than 1040K are around 108 M based on 21cm emission studies of the galaxies (reviewed by Van Woerden 1977). We would expect almost two orders of magnitude more material than this to have been ejected from the stars. Burke (1968), Johnson and Axford (1971) and Mathews and Baker (1971) postulated the existance of a hot galactic wind with temperatures of a few times 1060K powered by supernovae, in order to clear material from these galaxies. The evidence for hot galactic haloes around spiral galaxies is even more indirect and is based on the existance of high latitude cold clouds in our own galaxy. The velocities and number of these clouds imply that they almost certainly lie high above the galactic cold gas which extends only to a height of 130 Fc in the solar neighborhood. Spitzer therefore suggested in 1956 that an intercloud gas would have to exist to keep these clouds confined, and that to have such a large scaleheight it would have to be hot with temperatures of around 1060K. (An alternative suggestion by Pickelner (1955) was that the halo was cold but supported by turbulent velocities of around 70 km s-1.) The Spitzer Halo was assumed to be maintained by energetic particles from SN in the plane.

Type
Joint Discussion
Information
Highlights of Astronomy , Volume 5: Highlights of Astronomy. As presented at the XVIIth General Assembly of the IAU, 1979 , 1980 , pp. 411 - 417
Copyright
Copyright © Cambridge University Press 1980

References

Blades, J. C, 1979, preprint.Google Scholar
Bregman, J.N., 1978, Ap. J., 224, 768.Google Scholar
Burke, J.A., 1968, M.N.R.A.S., 140, 241.Google Scholar
Chevalier, R. and Oegerle, W., 1979, Ap.J., 227, 398.CrossRefGoogle Scholar
Collins, L.A. and Weisheit, J. 1976, Ap.J., 210, 299.Google Scholar
Cox, D.P., 1979, Ap. J. in press.Google Scholar
Field, G.B., 1974, in Physique Atomique et Moleculaire et Materie Interstellaire (les Houches) ed. Bailan, R., Encrenaz, P. and Lequeux, J., North Holland Amsterdam Google Scholar
Hayakawa, S., Kato, T., Nagase, k., Yamashita, K., and Tanaka, Y., 1978, Astron. Astrophys., 62, 21.Google Scholar
Ipavich, F.M., 1975, Ap.J., 196, 107.CrossRefGoogle Scholar
Johnson, H.E. and Axford, W.I., 1971, Ap.J., 165, 381.Google Scholar
Mathews, W.G. and Baker, J. C, 1971, Ap. J., 170, 241.CrossRefGoogle Scholar
McKee, C.F. and Ostriker, J.P., 1977, Ap. J., 218, 148.Google Scholar
Pickelner, S.B. 1955, MeM Soc. R. Sci. Liege, 4-15, 595.Google Scholar
Savage, B. and de Boer, K. 1979, Ap. J. (letters), 230, L77.CrossRefGoogle Scholar
Shapiro, P.R. and Field, G.B., 1976, Ap. J., 205, 762.Google Scholar
Songaila, A. and York, D.G., 1979, preprint.Google Scholar
Spitzer, L., 1956, Ap. J., 124, 20.Google Scholar
Van Woerden, H., 1977, in Topics in Interstellar Matter (pp. 261–283) ed. by H., Van Woerden (D. Reidel: Dordrecht)Google Scholar
Walborn, N., 1979, preprint.Google Scholar