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Title:
Magnetic activity in HD 111456, a young F5-6 main-sequence star
Authors:
Freire Ferrero, R.; Frasca, A.; Marilli, E.; Catalano, S.
Affiliation:
AA(Observatoire Astronomique, 11 rue de l'Université, 67000 Strasbourg, France), AB(INAF - Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy), AC(INAF - Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy), AD(INAF - Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy)
Publication:
Astronomy and Astrophysics, v.413, p.657-667 (2004) (A&A Homepage)
Publication Date:
01/2004
Origin:
A&A
Astronomy Keywords:
stars: activity, stars: individual: HD 111456
DOI:
10.1051/0004-6361:20031565
Bibliographic Code:
2004A&A...413..657F

Abstract

We present spectroscopic and photometric observations of the young F5-6 V field star HD 111456 which exhibits emission cores in the Ca Ii H and K lines and a filling in the H\alpha line. Absorption lines of He I D_3 and Li I are clearly detected and we give a new value of v\sin i=41.5 km s-1. Although the limit of magnetic activity detectability at optical wavelengths occurs around F5-6 spectral types, HD 111456 shows unusual chromospheric activity. High UV fluxes in the C Ii, C Iv, Si Ii and Si Iv lines and a strong X-ray emission confirm that HD 111456 is one of the most active F5-6 V star. The Ca Ii and H\alpha chromospheric emission fluxes do not show any detectable variation on time scales of few days, as well as uvby photometry. A possible explanation in terms of a very high level of magnetic activity and a homogeneous distribution of active regions, both at chromospheric and photospheric level, or a very low inclination of the rotation axis with respect to the line of sight is proposed. From 1998 to 2001 the radial velocity varies indicating a possible binary system, but the spectral distribution of HD 111456 is better reproduced by a single normal F5 V star, and composite spectra simulations (Ca Ii, H\alpha) with a normal inactive F star and a very active low-mass K-M star are not able to reproduce the observed emissions.

Based on observations collected at the Observatoire de Haute Provence (CNRS), France, and at the Osservatorio Astrofisico di Catania, Italy.

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