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Some Constraints on Chromospheric Modelling for Solar-Type Stars with High S:N Spectra

Published online by Cambridge University Press:  19 July 2016

B. H. Foing ,
F. Castelli ,
G. Vladilo  and
J. Beckman
B. H. Foing
Affiliation:
LPSD/IAS Verrierres, France.
F. Castelli
Affiliation:
Osservatorio Astronomico di Trieste, Trieste, Italy.
G. Vladilo
Affiliation:
Osservatorio Astronomico di Trieste, Trieste, Italy.
J. Beckman
Affiliation:
Instituto de Astrofisica de Canarias, Tenerife, Spain.

Abstract

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High signal to noise spectra are required in chromospheric modelling because chromospheric emission lines are formed in a boundary layer under conditions of NLTE and in non-hydrostatic equilibrium, as well as in multiple magnetically-controlled streams, with horizontal structure on several scales, and vertical velocity fields. To obtain useable estimates of energy dissipation with height we have obtained sequences of spectra from F8 to K5 and for stars of different activity levels. These comprise Call H and K, the IR triplet, and MgII h and k obtained with the ESO CAT+CES or IUE. We outline the constraints such observations place on models and indicate theoretical and observational difficulties.

Type
III. Stars
Information
Symposium - International Astronomical Union , Volume 132: The Impact of Veryhigh S/N Spectroscopy on Stellar Physics , 1988 , pp. 149 - 151
Copyright
Copyright © Kluwer 1988 

References

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