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Activity, Colour Anomalies and Temperature Determination in Solar-type Stars

Published online by Cambridge University Press:  12 April 2016

J. Fabregat ,
V. Reglero ,
J. Suso  and
J.E. Armentia
J. Fabregat
Affiliation:
Departamento de Matemática Aplicada y Astronomía, Universidad de Valencia, 46100 Burjassot (Valencia), Spain Physics Department, The University, Southampton S09 5NH, U.K.
V. Reglero
Affiliation:
Departamento de Matemática Aplicada y Astronomía, Universidad de Valencia, 46100 Burjassot (Valencia), Spain
J. Suso
Affiliation:
Departamento de Matemática Aplicada y Astronomía, Universidad de Valencia, 46100 Burjassot (Valencia), Spain
J.E. Armentia
Affiliation:
Departamento de Astrofísica, Universidad Complutense de Madrid, 28040 Madrid, Spain

Extract

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The presence of photometric anomalies in broad band colours produced by chromospheric activity was first suggested by Campbell (1984). He defined the colour anomaly δ(B–V)V–K as the deviation from the mean relation (B–V)–(V–K) for Hyades dwarfs, and found this anomaly correlated well with several activity indicators.

Since the work of Campbell, several authors have discussed the relation between activity and colour anomalies, obtaining diverging results. This discussion is relevant because long baseline photometric colours are the most reliable temperature indicators, and the presence of such anomalies implies that no consistent temperature scales can be obtained for stars with different activity levels. These topics have been recently reviewed by Soderblom (1989).

Type
Part IV Stellar activity
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 333 - 335
Copyright
Copyright © Springer-Verlag 1991

References

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