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The vertical structure of the magnetic field of the CP star $\alpha^{2}$ CVn

Published online by Cambridge University Press:  02 March 2005

I. Romanyuk  and
D. Kudryavtsev
I. Romanyuk
Affiliation:
Special Astrophysical Observatory of the RAS, Nizhny Arkhyz, Russia email: [email protected], [email protected]
D. Kudryavtsev
Affiliation:
Special Astrophysical Observatory of the RAS, Nizhny Arkhyz, Russia email: [email protected], [email protected]
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Abstract

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We observed the magnetic field of the CP star $\alpha^2$ CVn with the 6-m telescope and the echelle-spectrometer (spectral resolution $R=50000$, spectral range $\lambda\lambda 3400--4100$) using a CCD device and Zeeman analyzer. The longitudinal magnetic field $B_{\rm e}$ measured using lines with wavelengths shorter than the Balmer jump ($\lambda 3646$) are systematically 25% smaller at all rotational phases compared with measurements made in the region $\lambda > 3646$. Because in general lines with $\lambda > 3646$ form at deeper levels than lines with $\lambda < 3646$ we get additional evidence for the increase of $B_{\rm e}$ with depth in the atmosphere of $\alpha^2$ CVn.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

Stars: chemically peculiarstars: magnetic fieldsstars: atmospherestars: individual ($\alpha^{2}$ CVn)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS224 , July 2004 , pp. 602 - 604
Copyright
© 2004 International Astronomical Union