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Estimating the chromospheric magnetic field from a revised NLTE modeling: the case of HR 7428

Published online by Cambridge University Press:  12 September 2017

Innocenza Busá Open the ORCID record for Innocenza Busá [Opens in a new window]
Innocenza Busá*
Affiliation:
INAF - Catania Astrophysical Observatory, Via S. Sofia, 78, 95123 - Catania - Italy email: [email protected]
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Abstract

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Semi-empirical atmospheric modeling is here used to obtain the chromospheric magnetic field distribution versus height in the K2 primary component of the RS CVn binary system HR 7428. The chromospheric magnetic field estimation versus height comes from considering the possibility of not imposing hydrostatic equilibrium in the atmospheric modeling. The stability of the best Non-hydrostatic equilibrium model, implies the presence of and additive (toward the center of the star) pressure, that decrease in strength from the base of the chromosphere toward the outer layers. Interpreting the additive pressure as magnetic pressure and I derive a magnetic field intensity of about 500 Gauss at the base of the chromosphere.

Keywords

magnetic fieldstars: chromospheresstars: modeling atmospherestars: activity
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S328: Living Around Active Stars , October 2016 , pp. 38 - 45
Copyright
Copyright © International Astronomical Union 2017 

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