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The Calibration of Photometric Determinations of Abundance

Published online by Cambridge University Press:  04 August 2017

V. Straižys
V. Straižys*
Affiliation:
Vilnius Astronomical Observatory

Abstract

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Photometric abundance determinations using blanketing in the ultraviolet and violet spectral regions as well as the intensity of strong lines and bands is the most important tool in the study of chemical composition of faint and distant stars. However, this method requires the calibration of different photometric quantities in terms of abundance at given temperatures and luminosities. Two principal methods of calibration are in use. One of them uses stars with abundances determined from high dispersion spectra by curve of growth or model atmosphere analysis of the spectral lines. The other one uses synthetic spectra based on model atmospheres which are integrated to imitate the narrow band photometric indices. This paper will summarize the results of the application of both of these methods to calibrate a number of the important photometric systems. Most attention will be given to the late-type stars, which demonstrate the strongest photometric abundance effects.

Type
1. Review Papers
Information
Symposium - International Astronomical Union , Volume 111: Calibration of Fundamental Stellar Quantities , 1985 , pp. 285 - 301
Copyright
Copyright © Reidel 1985 

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