The Effects of Thermal Heating via the Dissipation of Turbulence on Physical Conditions in the Galactic Diffuse Ionized Gas

Details The Effects of Thermal Heating via the Dissipation of Turbulence on Physical Conditions in the Galactic Diffuse Ionized Gas The Effects of Thermal Heating via the Dissipation of Turbulence on Physical Conditions in the Galactic Diffuse Ionized Gas

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...484l.133m&link_type=abstract

Astrophysical Journal Letters v.484, p.L133

Astronomy and Astrophysics

Astronomy

21

Ism: General, Ism: Kinematics And Dynamics, Turbulence

Scientific paper

The observed properties of the diffuse ionized gas (DIG) in our Galaxy are not easily reconcilable with simple photoionization models. Photoionization models, however, can reproduce the observed properties of H II regions. 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] lambda 6583/H alpha ratio, [S II] lambda 6716/H alpha ratio, and He I lambda 5876/H alpha ratio as observed in the DIG. The model suggests that the observed [O III] emission from the diffuse interstellar medium (ISM) does not originate from the oxygen 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.

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