Estimating the chromospheric magnetic field from a revised NLTE modeling: the case of HR 7428. Issue Volume 12:Issue S328(2016) (12th September 2017)

• Record Type: Journal Article
• Authors: Busá, Innocenza
• Editors: Nandy, D.; Valio, A.; Petit, P.
• Is Part Of: Proceedings of the International Astronomical Union. Volume 12:Issue S328(2016)
• Page Start: 38
• Page End: 45
• Publication Date: 2017-09-12
• Subjects: magnetic field, -- stars: chromospheres, -- stars: modeling atmosphere, -- stars: activity; Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S1743921317003684
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract: 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.