Volume 537, January 2012
|Number of page(s)||10|
|Published online||26 January 2012|
Multi-element Doppler imaging of the CP2 star HD 3980⋆
1 Universität Wien, Institut für Astronomie, Türkenschanzstraße 17, 1180 Wien, Austria
2 Institute of Astrophysics, Georg-August University, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany
3 Sobolev Astronomical Institute, St. Petersburg State University, Universitetski pr. 28, St. Petersburg 198504, Russia
4 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
5 Institute of Astronomy, Russian Academy of Science, Pyatnitskaya 48, 119017 Moscow, Russia
6 Department of Physics and Astronomy, Uppsala University, Box 515, 75120 Uppsala, Sweden
7 Department of Radiotherapy, Medical University of Vienna, Währinger Gürtel 18-20, 1090 Wien, Austria
8 Crimean Astrophysical Observatory, Nauchnyi, Crimea, Ukraine
9 Observatório Nacional/MCT, Rua Gen. José Cristino 77, 20921-400 Rio de Janeiro, Brazil
Received: 18 April 2011
Accepted: 18 October 2011
Context. In atmospheres of magnetic main-sequence stars, the diffusion of chemical elements leads to a number of observed anomalies, such as abundance spots across the stellar surface.
Aims. The aim of this study was to derive a detailed picture of the surface abundance distribution of the magnetic chemically peculiar star HD 3980.
Methods. Based on high-resolution, phase-resolved spectroscopic observations of the magnetic A-type star HD 3980, the inhomogeneous surface distribution of 13 chemical elements (Li, O, Si, Ca, Cr, Mn, Fe, La, Ce, Pr, Nd, Eu, and Gd) has been reconstructed. The INVERS12 code was used to invert the rotational variability in line profiles to elemental surface distributions.
Results. Assuming a centered, dominantly dipolar magnetic field configuration, we find that Li, O, Mg, Pr, and Nd are mainly concentrated in the area of the magnetic poles and depleted in the regions around the magnetic equator. The high abundance spots of Si, La, Ce, Eu, and Gd are located between the magnetic poles and the magnetic equator. Except for La, which is clearly depleted in the area of the magnetic poles, no obvious correlation with the magnetic field has been found for these elements otherwise. Ca, Cr, and Fe appear enhanced along the rotational equator and the area around the magnetic poles. The intersection between the magnetic and the rotational equator constitutes an exception, especially for Ca and Cr, which are depleted in that region.
Conclusions. No obvious correlation between the theoretically predicted abundance patterns and those determined in this study could be found. This can be attributed to a lack of up-to-date theoretical models, especially for rare earth elements.
Key words: stars: abundances / techniques: spectroscopic / stars: chemically peculiar / stars: magnetic field / diffusion / stars: individual: HD 3980
Table 1 is available in electronic form at http://www.aanda.org
© ESO, 2012
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