The FeII Spectra of Eta Carinae: Implications for Atomic and Plasma Astrophysics

Details The FeII Spectra of Eta Carinae: Implications for Atomic and Plasma Astrophysics The FeII Spectra of Eta Carinae: Implications for Atomic and Plasma Astrophysics

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8387v&link_type=abstract

HST Proposal ID #8387

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Hst Proposal Id #8387 Stellar Ejecta

Scientific paper

The FeII emission spectrum is a ubiquitous one, appearing in such objects as stars, protostellar disks, HII regions, novae, supernova remnants, active galaxies and quasars. Its interpretation is painfully difficult because of the great complexity of the Fe^+ energy level structure. We have embarked on a long term program to fully simulate the physical conditions within FeII-emitting gas and then predict the resulting spectrum. The first steps, the generation of the initial data base and its incorporation into the radiative- collisional code Cloudy, are complete. Now we request archive HST observations of the massive star Eta Carinae. Although Eta Carinae is one of the most studied stellar objects, its spectrum of FeII emission lines is still poorly understood. We plan to attack the FeII spectrum from two directions: {1} by detailed self-consistent quantitative modelling of all excitation mechanisms of the FeII atom interacting with its environment, {2} and by validating existing and calculating new atomic data for FeII. The rich FeII spectra of Eta Carinae will allow us to check the reliability and completeness of the atomic data and processes considered, to investigate the sensitivity of emission lines to temperature and density variations, to assess the importance of blending, and hence to quantify what FeII emission tells us about iron abundances in other objects.

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