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Spectroscopy of Rapidly Oscillating Ap Stars

Published online by Cambridge University Press:  12 April 2016

W.W. Weiss
Affiliation:
Institute for Astronomy, Univ. Vienna, Türkenschanzstrasse 17, A-1180 Vienna, Austria (last-name@astro.univie.ac.at)
T.A. Ryabchikova
Affiliation:
Institute for Astronomy, Univ. Vienna, Türkenschanzstrasse 17, A-1180 Vienna, Austria (last-name@astro.univie.ac.at) Institute of Astronomy, Russ. Acad. Sciences, Moscow, Russia (ryabchik@inasan.rssi.ru)
I. Savanov
Affiliation:
Crimean Astrophysical Observatory, c/o 334413 Nauchny, Crimea, Ukraine (savanov@crao.crimea.ua)
N. Piskunov
Affiliation:
Uppsala Astronomical Observatory, S-751 20 Uppsala, Sweden (last-name@astro.uu.se)
V. Tsymbal
Affiliation:
Tavrian National University, Physics Dept., 950000 Crimea, Ukraine (vad@ccssu.Crimea.ua)
P. Mittermayer
Affiliation:
Institute for Astronomy, Univ. Vienna, Türkenschanzstrasse 17, A-1180 Vienna, Austria (last-name@astro.univie.ac.at)
P. Martinez
Affiliation:
South African Astronomical Observatory, P.O. Box 9, Observatory 7935, South Africa (peter@saao.ac.za)
O. Kochukhov
Affiliation:
Uppsala Astronomical Observatory, S-751 20 Uppsala, Sweden (last-name@astro.uu.se)
N. Nesvacil
Affiliation:
Institute for Astronomy, Univ. Vienna, Türkenschanzstrasse 17, A-1180 Vienna, Austria (last-name@astro.univie.ac.at)

Abstract

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We identify Spectroscopic differences between roAp stars and Ap stars with no observational evidence for pulsation, but with otherwise similar Teff and log g values. These differences concern the abundance pattern, Hydrogen line profile anomalies, evidence for stratification, and effects of pulsation on spectral lines.

Type
Part 2.3. Chemically Peculiar Stars
Copyright
Copyright © Astronomical Society of the Pacific 2002

References

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