Abundances in Przybylski's star |
| |
| Authors: | C R Cowley T Ryabchikova F Kupka D J Bord G Mathys W P Bidelman |
| |
| Institution: | Department of Astronomy, University of Michigan, David M. Dennison Building, Ann Arbor, MI 48109, USA;Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya str. 48, 109017 Moscow, Russia;Visiting Scientist, Institute of Astronomy, University of Vienna, Türkenschanzstraße 17, A-1180 Vienna, Austria;Institute for Astronomy, University of Vienna, Türkenschanzstraße 17, A-1180 Vienna, Austria;Department of Natural Sciences, The University of Michigan-Dearborn, 4901 Evergreen Rd., Dearborn, MI 48128-1491, USA;European Southern Observatory, Casilla 19001, Santiago 19, Chile;Case Western Reserve University, Department of Astronomy, Cleveland, OH 44106-7215, USA |
| |
| Abstract: | 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 T eff=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. |
| |
| Keywords: | stars: abundances stars: chemically peculiar stars: individual: HD 101065 |
|
|
