Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...128...74f&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 128, no. 1, Nov. 1983, p. 74-83.
Astronomy and Astrophysics
Astrophysics
32
Absorption Spectra, Chromosphere, Emission Spectra, Stellar Spectra, Variable Stars, Calcium, Helium, Hydrogen, Line Spectra, Sodium, Stellar Color
Scientific paper
The H-alpha, He I 5876 A, Na I 5890 A, Ca II IR triplet, and P14-P16 Paschen lines of AB Aur are all brighter than the nearby continuum. The emission lines are examined with regard to their origin as either recombination or chromospheric emission. While He I and H-alpha could be formed simultaneously by recombination under certain circumstances, a deep chromosphere would account for He I 5876, for the Paschen lines in emission, and perhaps even for the Ca II IR triplet in emission. A deep chromosphere would also explain why higher Balmer lines are in absorption and why the Ca II resonance lines have only an autoreversed emission core, despite not being fully in emission.
Felenbok Paul
Praderie Francoise
Talavera Antonio
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