The Mg i b triplet and the 4571 Å line as diagnostics of stellar chromospheric activity

Context. The Mg i 4571 Å line and the b triplet are denoted in the literature as diagnostics of solar and stellar activity since their formation is in the low chromosphere. Aims. We aim to investigate the potential of these four spectral lines as diagnostics of chromospheric activity in solar-like s...

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Bibliographic Details
Published in:Astronomy and astrophysics (Berlin) 2017-08, Vol.604, p.A50
Main Authors: Sasso, C., Andretta, V., Terranegra, L., Gomez, M. T.
Format: Article
Language:English
Subjects:
Astronomical models
Atmospheric models
Chromosphere
Dependence
Line spectra
Metallicity
Photosphere
Radiative transfer
stars: activity
stars: chromospheres
stars: solar-type
Stellar activity
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Summary:Context. The Mg i 4571 Å line and the b triplet are denoted in the literature as diagnostics of solar and stellar activity since their formation is in the low chromosphere. Aims. We aim to investigate the potential of these four spectral lines as diagnostics of chromospheric activity in solar-like stars, studying the dependence of the intensity of these lines from local atmospheric changes by varying atmospheric models and stellar parameters. Methods. Starting with Next-Gen photospheric models, we build a grid of atmospheric models including photosphere, chromosphere and transition region and solve the radiative transfer to obtain synthetic profiles to compare with observed spectra of main-sequence, solar like stars with effective temperatures in the range 4800–6400 K, solar gravity and solar metallicity. Results. We find that the Mg i 4571 Å line is significantly sensitive to local changes in the atmospheric model around the minimum temperature. Conversely, the lines of the b triplet do not show significant responses to changes on the local atmospheric structure.
ISSN:0004-6361
1432-0746
DOI:10.1051/0004-6361/201730676