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Modelling the Local Interstellar Medium As A Supernova Remnant In A Multiphase Gas

Published online by Cambridge University Press:  12 April 2016

Lennox L. Cowie
Lennox L. Cowie*
Affiliation:
Space Telescope Science Institute, Physics Department, M.I.T., and Physics Department, J.H.U.

Extract

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Trying to understand the local interstellar gas in detail may be a hopeless task for a theorist. In the interstellar medium as a whole, we can at least address global properties and perhaps come to some reasonable “time averaged” conclusions such as those of Cox and his collaborators (e.g. Cox and Smith 1974, Cox 1979) or McKee and Ostriker (1977). Even this is quite uncertain of course, both because the ISM gas has structure on scales from at least 1 Pc (and probably much smaller) all the way up to the size of the galaxy, and because none of us are quite sure which physical processes (such as thermal evaporation or heating of cooler gas by magnetohydrodynamic processes) are really important. However, in the local ISM things are significantly worse in that we no longer have even the ergodic hypothesis available to us – rather we have to try and deal with individual events and structures. On the other hand, we do have more detailed observations and hence a laboratory to try to decide on the importance of the various physical processes.

Type
Theoretical Models
Information
International Astronomical Union Colloquium , Volume 81: Local Interstellar Medium , 1984 , pp. 287 - 296
Copyright
Copyright © NASA 1984

References

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