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Turbulent Heating in the Galactic Diffuse Ionized Gas

Published online by Cambridge University Press:  12 April 2016

Anthony Minter  and
Dana S. Balser
Anthony Minter
Affiliation:
National Radio Astronomy Observatory**Green Bank, West Virginia, U.S.A.24944
Dana S. Balser
Affiliation:
National Radio Astronomy Observatory**Green Bank, West Virginia, U.S.A.24944

Abstract

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The observed properties of the diffuse ionized gas (DIG) in our Galaxy are not easily reconcilable with simple photoionization models. This suggests that there are different or additional physical processes at work in the DIG. We have developed a model of the DIG whereby it is ionized by a relatively soft ionizing spectrum (Teff ≤ 32,000 K) and is also heated by an additional thermal mechanism: the dissipation of turbulence. This model predicts the same electron temperature, [N II] λ 6583/Hα ratio, [S II] λ 6716/Hα ratio and He I λ 5876/Hα ratio as observed in the DIG. Without the turbulent thermal heating term, this model will not reproduce the observed properties of the DIG. The dissipation of turbulence may also be important in other phases of the ISM.

Type
Part IX External Galaxies
Information
International Astronomical Union Colloquium , Volume 166: The Local Bubble and Beyond , 1997 , pp. 543 - 546
Copyright
Copyright © Springer-Verlag 1998

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