1. The pulsations of PG 1351+489
- Author
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Redaelli, Maurício, Kepler, Souza Oliveira, Costa, Jose Eduardo da Silveira, Winget, Donald Earl, Handler, Gerald, Castanheira, Bárbara Garcia, Kanaan Neto, Antonio Nemer, Fraga, Luciano, Henrique, P., Giovannini Junior, Odilon, Provencal, Judith L., Shipman, Harry L., Dalessio, J., Thompson, S. E., Mullally, Fergal, Brewer, M. M., Childers, D., Oksala, M. E., Rosen, Rachel, Wood, Matthew A., Reed, M. D., Walter, B., Strickland, Willie, Chandler, Dean W., Watson, Todd K., Nather, R. Edward, Montgomery, Michael Houston, Bischoff-Kim, Agnès, Hansen, Carl J., Nitta, Atsuko, Kleinman, Scot James, Claver, C.F., Brown, Tim, Sullivan, Denis J., Kim, Seung-Lee, Chen, Wen-Ping, Yang, M., Shih, Chia-You, Zhang, X, Jiang, Xiaojun, Fu, Jianning Ning, Seetha, S., Ashoka, B.N., Marar, T.M. Krishnan, Baliyan, Kiran S., Vats, Hari Om, Chernyshev, A.V., Ibbetson, Peter A., Leibowitz, Elia M., Hemar, Shirley, Sergeev, A., Andreev, M., Janulis, Rimvydas, Meistas, Edmundas G., Moskalik, Pawel, Pajdosz, Gabriel, Baran, Andrzej, Winiarski, M., Zola, Staszek, Ogloza, Waldemar, Siwak, Michal, Bognár, Zsófia, Solheim, Jan-Eric, Sefako, R., Buckley, David A.H., O'Donoghue, Darragh, Nagel, Thorsten, Silvotti, Roberto, Bruni, I., Fremy, J. R., Vauclair, Gérard, Chevreton, Michel, Dolez, Noël, Pfeiffer, Ben, Barstow, Martin A., Creevey, o, Kawaler, Steven D., and Clemens, J. Christopher
- Subjects
Anãs brancas ,Oscilacoes ,individual: PG 1351+489 [Stars] ,oscillations [Stars] ,Evolucao estelar ,evolution [Stars] ,White dwarfs - Abstract
PG 1351+489 is one of the 20DBVs – pulsating helium-atmospherewhite dwarf stars – known and has the simplest power spectrum for this class of star, making it a good candidate to study cooling rates. We report accurate period determinations for the main peak at 489.334 48 s and two other normal modes using data from the Whole Earth Telescope (WET) observations of 1995 and 2009. In 2009, we detected a new pulsation mode and the main pulsation mode exhibited substantial change in its amplitude compared to all previous observations. We were able to estimate the star’s rotation period, of 8.9 h, and discuss a possible determination of the rate of period change of (2.0 ± 0.9) × 10−13 s s-ˡ, the first such estimate for a DBV.
- Published
- 2011