The variable 6307A emission line in the spectrum of Eta Carinae: blueshifted [S III] 6313A from the interacting winds

Details The variable 6307A emission line in the spectrum of Eta Carinae: blueshifted [S III] 6313A from the interacting winds The variable 6307A emission line in the spectrum of Eta Carinae: blueshifted [S III] 6313A from the interacting winds

2009-10-07

arxiv.org/abs/0910.1286v2

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

15 pages. accepted, PASP

Scientific paper

The 6307A emission line in the spectrum of Eta Car (Martin et al. 2006) is blue-shifted [S III] 6313A emission originating from the outer wind structures of the massive binary system. We realized the identification while analyzing multiple forbidden emission lines not normally seen in the spectra of massive stars. The high spatial and moderate spectral resolutions of HST/STIS resolve forbidden lines of Fe+, N+, Fe++, S++, Ne++ and Ar++ into spatially and velocity-resolved rope-like features originating from collisionally-excited ions photo-ionized by UV photons or collisions. While the [Fe II] emission extends across a velocity range of +/-500 km/s out to 0."7, more highly ionized forbidden emissions are systematically blue-shifted (-500 to +200 km/s) and extend only to 0."4. The [Fe II] defines the outer regions of the massive primary wind. The [N II], [Fe III] emission define the the outer wind interaction regions directly photo-ionized by far-UV radiation. Variations in emission of [S III] 9533A, 9071A and 6313A suggest density ranges of 10^6 to 10^10 cm^-3 for electron temperatures ranging from 8,000 to 13,000K. Mapping the temporal changes of the emission structure at critical phases of the 5.54-year period will provide important diagnostics of the interacting winds.

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