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A study of the Mg II 2796.34 angstrom emission line in late-type normal and RS CVn stars

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Cardini, D. and Cassatella, A. and Badiali, M. and Altamore, A. and Fernández Figueroa, María José (2003) A study of the Mg II 2796.34 angstrom emission line in late-type normal and RS CVn stars. Astronomy & Astrophysics, 408 (1). pp. 337-345. ISSN 0004-6361

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Official URL: http://dx.doi.org/10.1051/0004-6361:20030913


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Abstract

We carry out an analysis of the Mg II 2796.34 Å emission line in RS CVn stars and make a comparison with the normal stars studied in a previous paper ( Paper I). The sample of RS CVn stars consists of 34 objects with known HIPPARCOS parallaxes and observed at high resolution with IUE. We confirm that RS CVn stars tend to possess wider Mg II. lines than normal stars having the same absolute visual magnitude. However, we could not find any correlation between the logarithmic line width log W_o and the absolute visual magnitude M_v (the Wilson-Bappu relationship) for these active stars, contrary to the case of normal stars addressed in Paper I. On the contrary, we find that a strong correlation exists in the (M_v, log L_MgII) plane (L_MgII is the absolute flux in the line). In this plane, normal and RS CVn stars are distributed along two nearly parallel straight lines with RS CVn stars being systematically brighter by ≈1 dex. Such a diagram provides an interesting tool to discriminate active from normal stars. We finally analyse the distribution of RS CVn and of normal stars in the (log L_MgII, log W_o) plane, and find a strong linear correlation for normal stars, which can be used for distance determinations.


Item Type:Article
Additional Information:

© ESO 2003. The authors are grateful to Prof. J. Linsky for
stimulating suggestions and to Dr. D. Marinucci for useful comments.

Uncontrolled Keywords:Chromospherically active binaries; CA-II-H; Multiwavelength optical observations; High-resolution spectra; Wilson-Bappu relation; K-line; Stellar activity; Ines system; Alpha; Parameters
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
ID Code:31484
Deposited On:03 Aug 2015 12:32
Last Modified:10 Dec 2018 15:05

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