Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...581.1154v&link_type=abstract
The Astrophysical Journal, Volume 581, Issue 2, pp. 1154-1167.
Astronomy and Astrophysics
Astronomy
35
Ism: H Ii Regions, Ism: Individual: Name: Η Carinae, Line: Formation, Line: Identification
Scientific paper
We present numerical simulations that reproduce the salient features of the amazingly strong [Fe II] and Fe II emission spectra in the B and D Weigelt blobs of η Carinae. For our studies we have used spectra obtained during the 1998 epoch observations with the Hubble Space Telescope (HST). The spectrum of the B and D Weigelt blobs dominates in [Fe II] and Fe II emission lines. The same observations show no Fe I or Fe III. We have compared our measurements of the strongest (>=200) [Fe II] and Fe II lines and blends in the spectrum with theoretical predictions. Our predictions are based on non-LTE modeling of the Fe II atom, which includes the lowest 371 energy levels (all levels up to 11.6 eV). We have investigated the dependence of the spectrum on electron density, pumping by the blackbody-like stellar continuum, and intense Lyα emission. We find that radiative pumping is essential in explaining the observed spectrum. We have identified the main pumping routes responsible for the observed Fe II emission. Comparison between the model and observations reveals details of the radiation field. Pumping by the blackbody-like stellar radiation field from η Carinae explains the numerous strong [Fe II] and Fe II lines in the range of 4000-6500 Å. The strongest Fe II lines in a range of 8000-10000 Å are pumped by intense Lyα radiation. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.
Bruhweiler Fred
Davidson Kris
Gull Ted R.
Ishibashi Kazunori
Johansson Sara
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