Fe II Emission from the Orion Nebula

Details Fe II Emission from the Orion Nebula Fe II Emission from the Orion Nebula

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...188.0712v&link_type=abstract

American Astronomical Society, 188th AAS Meeting, #07.12; Bulletin of the American Astronomical Society, Vol. 28, p.W833

Astronomy and Astrophysics

Astronomy

Scientific paper

We have incorporated a complete radiative-collisional model of the 371 lowest levels of Fe II into the radiative equilibrium code Cloudy. This simulation predicts transitions producing 68,635 lines. The atomic data were taken from the results of the "Iron Project" and recent laboratory spectroscopy; for unknown lines, we use interpolations and /line g-approximation. A variety of processes affects the Fe II spectrum, including collisional excitation, pumping by the attenuated incident continuum and all ~ 10(4) emission lines included in the calculation, and fluorescence due to overlapping Fe II lines. This allows us to determine local level populations for the Fe II model self-consistently with electron temperature and density within each zone. The Orion Nebula model presented by Baldwin et al. (1991, ApJ, 374, 580; depleted elements, grains, ionization by the central star, and a hydrostatic blister) was recomputed with the large Fe II model. This H II region model, proposed some time ago to reproduce higher ionization optical lines, reproduces the observed Fe II spectrum quite well.

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