Ultraviolet excitation of H2 emission in starburst galaxies?

Details Ultraviolet excitation of H2 emission in starburst galaxies? Ultraviolet excitation of H2 emission in starburst galaxies?

Aug 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.257..433m&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 257, no. 3, Aug. 1, 1992, p. 433-437.

Astronomy and Astrophysics

Astronomy

5

Emission Spectra, Hydrogen, Infrared Astronomy, Interstellar Matter, Massive Stars, Starburst Galaxies, Luminosity, Molecular Clouds, Photons, Ultraviolet Radiation

Scientific paper

The generation of H2 line emission by UV photons from massive stars is modeled. The models are used to reconsider the H2 properties of starburst galaxies, previously explained by shock excitation of H2. It is shown that UV excitation of H2 can explain the correlation between H2 2.12-microns and forbidden Fe II 1.64-micron emission lines, which has been cited as evidence for shock excitation. Moreover, in the case of M82, the amount of molecular material heated by UV radiation is found to be sufficient to account for the observed H2 luminosity. Hence UV heating of molecular clouds is one of the most plausible excitation mechanisms of H2 emission in starburst galaxies.

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