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An Empirical T – τ Curve for the Roap Star HR 3831: Atmospheric Structure from Pulsation Amplitudes

Published online by Cambridge University Press:  12 April 2016

Jaymie M. Matthews ,
William H. Wehlau ,
John Rice  and
Gordon A. H. Walker
Jaymie M. Matthews*
Affiliation:
Dépt. de physique, Université de Montréal et Observatoire Astronomique du Mont Megantic, C.P. 6128, succ. A, Montréal, P.Q. H3C 3J7Canada
William H. Wehlau*
Affiliation:
Department of Astronomy, University of Western Ontario, London, Ontario N6A 3K7Canada
John Rice*
Affiliation:
Department of Physics, Brandon University, Brandon, Manitoba R7A 6A9Canada
Gordon A. H. Walker
Affiliation:
Department of Geophysics & Astronomy, University of British Columbia, Vancouver, British Columbia V6T 1W5Canada
*
1Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatories, operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation
1Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatories, operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation
1Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatories, operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation

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The atmospheric structures of magnetic CP2 (Ap) stars are notoriously difficult to model: line blanketing is severe, surface gravities are extremely uncertain, and the surface abundance inhomogeneities lead to different atmospheric properties as a function of position on the star. Seismology of the p-modes of rapidly oscillating Ap (roAp) stars (Kurtz 1990), which vary with periods of a few minutes and amplitudes below 0.01 mag and 1 km/s in light and velocity, has already helped constrain the luminosities – and hence, the logg values – of some cool CP2 stars (Kurtz 1992, these proceedings). We show here that the pulsations of an roAp star can also directly probe the temperature structure of a CP2 atmosphere.

Type
VII. Photometric Variability and Evolutionary Status
Information
International Astronomical Union Colloquium , Volume 138: Peculiar versus Normal Phenomena in A-Type and Related Stars , 1993 , pp. 617 - 622
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Kurtz, D.W. 1990, ARA&A, 28, 607 Google Scholar
Kurtz, D.W., Shibahashi, H. & Goode, P.R. 1990, MNRAS, 247, 558 Google Scholar
Kurtz, D.W., Kanaan, A. & Martinez, P. 1992, MNRAS, in pressGoogle Scholar
Matthews, J.M. 1991, PASP, 103, 5 Google Scholar
Matthews, J.M., Wehlau, W.H. & Walker, G.A.H. 1990, ApJ, 365, L81 CrossRefGoogle Scholar
Shibahashi, H. & Saio, H. 1985, PASJ, 37, 245 Google Scholar
Weiss, W.W. & Schneider, H. 1984, A&A, 135, 148 Google Scholar