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High S/N Na I D Line Profiles in Late-Type MS Stars and their Importance for Stellar Modellingl

Published online by Cambridge University Press:  12 April 2016

E. Covino ,
M.T. Gomez ,
G. Severino  and
M. Franchini
E. Covino
Affiliation:
Osservatorio Astronomico di Capodimonte, Via Moiariello 16, Napoli
M.T. Gomez
Affiliation:
Osservatorio Astronomico di Capodimonte, Via Moiariello 16, Napoli
G. Severino
Affiliation:
Osservatorio Astronomico di Capodimonte, Via Moiariello 16, Napoli
M. Franchini
Affiliation:
Osservatorio Astronomico di Trieste Via Tiepolo 11, Trieste

Extract

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Progress in observational techniques (i.e. high S/N spectroscopy) and modelling (e.g. RE models including convection, nonLTE codes, accurate atomic data) make significant to carry to extremes the numerical fit of a portion of the stellar spectrum and try to interpret the residual differences between calculations and observations in terms of stellar characteristics new respect to the employed model.

We have started to apply this synthesis method to a set of high resolution, high S/N spectra of late-type dwarfs in the region of the Na I D lines, obtained at ESO with the 1.4m CAT on May 1989 (Franchini et al. 1992). The dwarf stars are modelled in radiative equilibrium (RE), and the Na I D line synthesis accounts for nonLTE and blend effects.

Type
II. Atmospheres, a window to the interior
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 190 - 192
Copyright
Copyright © Astronomical Society of the Pacific 1993

Footnotes

1

Based on observations collected at the European Southern Observatory, La Silla, Chile

References

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