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Constraining the evolution of ZZ Ceti

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Constraining the evolution of ZZ Ceti

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Título Constraining the evolution of ZZ Ceti
Autor Mukadam, Anjum Shagufta
Kepler, Souza Oliveira
Winget, Donald Earl
Nather, R. Edward
Kilic, Mukremin
Mullally, Fergal
Von Hippel, Theodore A.
Kleinman, Scot James
Nitta, Atsuko
Guzik, Joyce Ann
Bradley, Paul A.
Matthews, Jaymie M.
Sekiguchi, Kazuhiro
Sullivan, Denis J.
Sullivan, Terry
Shobbrook, Robert R.
Birch, P.
Jiang, Xiaojun
Xu, D.W.
Joshi, Santosh
Ashoka, B.N.
Ibbetson, Peter A.
Leibowitz, Elia M.
Ofek, Eran O.
Meistas, Edmundas G.
Janulis, Rimvydas
Alisauskas, Darius
Kalytis, Romualdas
Handler, Gerald
Kilkenny, Dave
O'Donoghue, Darragh
Kurtz, Donald W.
Muller, M.
Moskalik, Pawel
Ogloza, Waldemar
Zola, Staszek
Krzesinski, Jerzy
Johannessen, F.
Gonzalez Perez, Jose Miguel
Solheim, Jan-Eric
Silvotti, Roberto
Bernabei, S.
Vauclair, Gérard
Dolez, Noël
Fu, Jianning Ning
Chevreton, Michel
Manteiga, Minia
Suarez, Olga
Ulla, Ana
Cunha, Margarida S.
Metcalfe, Travis S.
Kanaan Neto, Antonio Nemer
Fraga, Luciano
Costa, Alex Fabiano Murillo da
Giovannini Junior, Odilon
Fontaine, Gilles
Bergeron, Pierre
O'Brien, M. Sean
Sanwal, Divas
Wood, Matthew A.
Ahrens, T.J.
Silvestri, Nicole M.
Klumpe, Eric W.
Kawaler, Steven D.
Riddle, Reed L.
Reed, M. D.
Watson, Todd K.
Abstract We report our analysis of the stability of pulsation periods in the DAV star (pulsating hydrogen atmosphere white dwarf ) ZZ Ceti, also called R548. On the basis of observations that span 31 years, we conclude that the period 213.13 s observed in ZZ Ceti drifts at a rate dP/dt ≤ (5:5 ± 1:9) x 10 15 s s-ˡ, after correcting for proper motion. Our results are consistent with previous _PP values for this mode and an improvement over them because of the larger time base. The characteristic stability timescale implied for the pulsation period is |P/PP| ≥ 1.2 Gyr, comparable to the theoretical cooling timescale for the star. Our current stability limit for the period 213.13 s is only slightly less than the present measurement for another DAV, G117-B15A, for the period 215.2 s, establishing this mode in ZZ Ceti as the second most stable optical clock known, comparable to atomic clocks and more stable than most pulsars. Constraining the cooling rate of ZZ Ceti aids theoretical evolutionary models and white dwarf cosmochronology. The drift rate of this clock is small enough that we can set interesting limits on reflex motion due to planetary companions.
Contido em The astrophysical journal. Chicago. Vol. 594, no. 2 pt. 1 (Sept. 2003), p. 961-970
Assunto Anãs brancas
Espectros estelares
Estrelas variaveis
Modelos estelares
Movimento estelar
Pulsacoes estelares
[en] Stars: evolution
[en] Stars: individual (ZZ Ceti, R548)
[en] Stars: oscillations
[en] Stars: variables: other
[en] White dwarfs
Origem Estrangeiro
Tipo Artigo de periódico
URI http://hdl.handle.net/10183/108912
Arquivos Descrição Formato
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