The vertical structure of the magnetic field of the CP star α2 CVn

Details The vertical structure of the magnetic field of the CP star α2 CVn The vertical structure of the magnetic field of the CP star α2 CVn

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004iaus..224..602r&link_type=abstract

The A-Star Puzzle, held in Poprad, Slovakia, July 8-13, 2004. Edited by J. Zverko, J. Ziznovsky, S.J. Adelman, and W.W. Weiss,

Computer Science

1

Stars: Chemically Peculiar, Stars: Magnetic Fields, Stars: Atmosphere, Stars: Individual (Α2 Cvn).

Scientific paper

We observed the magnetic field of the CP star α2 CVn with the 6-m telescope and the echelle-spectrometer (spectral resolution R=50000, spectral range λλ 3400--4100) using a CCD device and Zeeman analyzer. The longitudinal magnetic field Be measured using lines with wavelengths shorter than the Balmer jump (λ 3646) are systematically 25% smaller at all rotational phases compared with measurements made in the region λ > 3646. Because in general lines with λ > 3646 form at deeper levels than lines with λ < 3646 we get additional evidence for the increase of Be with depth in the atmosphere of α2 CVn.

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