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Understanding the cool DA white dwarf pulsator G29-38

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Understanding the cool DA white dwarf pulsator G29-38

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Título Understanding the cool DA white dwarf pulsator G29-38
Autor Kleinman, Scot James
Nather, R. Edward
Winget, Donald Earl
Clemens, J. Christopher
Bradley, Paul A.
Kanaan Neto, Antonio Nemer
Provencal, Judith L.
Claver, C.F.
Watson, Todd K.
Yanagida, K.
Nitta, Atsuko
Dixson, James S.
Wood, Matthew A.
Grauer, Albert D.
Hine, B.P.
Fontaine, Gilles
Liebert, James
Sullivan, Denis J.
Wickramasinghe, D.T.
Achilleos, Nicholas
Marar, T.M. Krishnan
Seetha, S.
Ashoka, B.N.
Meistas, Edmundas G.
Leibowitz, Elia M.
Moskalik, Pawel
Krzesinski, Jerzy
Solheim, Jan-Eric
Bruvold, A.
O'Donoghue, Darragh
Kurtz, Donald W.
Warner, B.
Martinez, Peter
Vauclair, Gérard
Dolez, Noël
Chevreton, Michel
Barstow, Martin A.
Kepler, Souza Oliveira
Giovannini Junior, Odilon
Augusteijn, T.
Hansen, Carl J.
Kawaler, Steven D.
Abstract The white dwarfs are promising laboratories for the study of cosmochronology and stellar evolution. Through observations of the pulsating white dwarfs, we can measure their internal structures and compositions, critical to understanding post-main-sequence evolution, along with their cooling rates, which will allow us to calibrate their ages directly. The most important set of white dwarf variables to measure are the oldest of the pulsators, the cool DA variables (DAVs), which have not been explored previously through asteroseismology due to their complexity and instability. Through a time-series photometry data set spanning 10 yr, we explore the pulsation spectrum of the cool DAV, G29-38 and find an underlying structure of 19 (not including multiplet components) normal-mode, probably l=1 pulsations amidst an abundance of time variability and linear combination modes. Modeling results are incomplete, but we suggest possible starting directions and discuss probable values for the stellar mass and hydrogen layer size. For the first time, we have made sense out of the complicated power spectra of a large-amplitude DA pulsator. We have shown that its seemingly erratic set of observed frequencies can be understood in terms of a recurring set of normal-mode pulsations and their linear combinations. With this result, we have opened the interior secrets of the DAVs to future asteroseismological modeling, thereby joining the rest of the known white dwarf pulsators.
Contido em The astrophysical journal. Chicago. Vol. 495, no. 1, pt. 1 (Mar. 1998), p. 424-434
Assunto Anãs brancas
Estrutura estelar
Fotometria estelar
Massa estelar
Pulsacoes estelares
[en] Stars : individual (G29-38)
[en] Stars : oscillations
[en] Stars : white dwarfs
Origem Estrangeiro
Tipo Artigo de periódico
URI http://hdl.handle.net/10183/108875
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