Abundances in Przybylski's star

  1. C. R. Cowley1,
  2. T. Ryabchikova2,3,
  3. F. Kupka4,*,
  4. D. J. Bord5,
  5. G. Mathys6,
  6. W. P. Bidelman7

Article first published online: 4 APR 2002

DOI: 10.1046/j.1365-8711.2000.03578.x

Issue

Monthly Notices of the Royal Astronomical Society

Monthly Notices of the Royal Astronomical Society

Volume 317, Issue 2, pages 299–309, September 2000

Additional Information

How to Cite

Cowley, C. R., Ryabchikova, T., Kupka, F., Bord, D. J., Mathys, G. and Bidelman, W. P. (2000), Abundances in Przybylski's star. Monthly Notices of the Royal Astronomical Society, 317: 299–309. doi: 10.1046/j.1365-8711.2000.03578.x

Author Information

  1. 1

    Department of Astronomy, University of Michigan, David M. Dennison Building, Ann Arbor, MI 48109, USA

  2. 2

    Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya str. 48, 109017 Moscow, Russia

  3. 3

    Visiting Scientist, Institute of Astronomy, University of Vienna, Türkenschanzstraße 17, A-1180 Vienna, Austria

  4. 4

    Institute for Astronomy, University of Vienna, Türkenschanzstraße 17, A-1180 Vienna, Austria

  5. 5

    Department of Natural Sciences, The University of Michigan-Dearborn, 4901 Evergreen Rd., Dearborn, MI 48128-1491, USA

  6. 6

    European Southern Observatory, Casilla 19001, Santiago 19, Chile

  7. 7

    Case Western Reserve University, Department of Astronomy, Cleveland, OH 44106-7215, USA

*★ E-mail: kupka@astro.univie.ac.at

Publication History

  1. Issue published online: 4 APR 2002
  2. Article first published online: 4 APR 2002
  3. Accepted 2000 February 26. Received 2000 February 25; in original form 1999 December 15

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Keywords:

  • stars: abundances;
  • stars: chemically peculiar;
  • stars: individual: HD 101065

We have derived abundances for 54 elements in the extreme roAp star HD 101065. ESO spectra with a resolution of about 80 000, and S/N of 200 or more were employed. The adopted model has Teff=6600 K, and log(g)=4.2. Because of the increased line opacity and consequent low gas pressure, convection plays no significant role in the temperature structure. Lighter elemental abundances through the iron group scatter about standard abundance distribution (SAD) (solar) values. Iron and nickel are about one order of magnitude deficient while cobalt is enhanced by 1.5 dex. Heavier elements, including the lanthanides, generally follow the solar pattern but enhanced by 3 to 4 dex. Odd-Z elements are generally less abundant than their even-Z neighbours. With a few exceptions (e.g. Yb), the abundance pattern among the heavy elements is remarkably coherent, and resembles a displaced solar distribution.

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