The presence of Si(3+) and C(3+) in the wind of AB AUR

Details The presence of Si(3+) and C(3+) in the wind of AB AUR The presence of Si(3+) and C(3+) in the wind of AB AUR

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...140..421c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 140, no. 2, Nov. 1984, p. 421-426.

Astronomy and Astrophysics

Astrophysics

19

Chromosphere, Pre-Main Sequence Stars, Stellar Composition, Stellar Spectra, Stellar Winds, Ultraviolet Spectra, Variable Stars, A Stars, Carbon Stars, Ionization, Resonance Lines, Silicon, Stellar Models, Stellar Temperature

Scientific paper

The Herbig Ae variable AB Aur (spectral type A0) exhibits a line spectrum characteristic of a stellar wind. IUE observations of the Si IV and C IV resonance lines in AB Aur are reported. These lines are strong and in absorption. Two models can explain the presence of Si3+ and C3+ in the wind of AB Aur: a "remote chromosphere" model, with a temperature rise up to 105K, occurring beyond the point where the ionizing radiation begins to depart from the local Planck function, and a "deep chromosphere" model, with a temperature rise up to 15,000 - 18,000K, located just above the stellar photosphere. Several additional observational arguments are in favor of the "deep chromosphere" model.

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