Whole Earth Telescope observations of the DAV white dwarf G226-29

We observed G226-29 for 121 hr in 1992 February and confirm the presence of the three previously identified frequencies close to 109 s. We find no evidence of other pulsation periods down to our noise level of about 0.35 millimodulation amplitudes. The presence of only one triplet pulsation mode in...

Descripción completa

Detalles Bibliográficos
Autores: Kepler, Souza Oliveira, Giovannini Junior, Odilon, Wood, Matthew A., Nather, R. Edward, Winget, Donald Earl, Kanaan Neto, Antonio Nemer, Kleinman, Scot James, Bradley, Paul A., Provencal, Judith L., Clemens, J. Christopher, Claver, C.F., Watson, Todd K., Yanagida, K., Krisciunas, K., Marar, T.M. Krishnan, Seetha, S., Ashoka, B.N., Leibowitz, Elia M., Mendelson, Haim, Mazeh, Tsevi, Moskalik, Pawel, Krzesinski, Jerzy, Pajdosz, Y., Zola, Staszek, Solheim, Jan-Eric, Emanuelsen, P.-I., Dolez, Noël, Vauclair, Gérard, Chevreton, Michel, Fremy, J. R., Barstow, Martin A., Sansom, A.E., Tweedy, R.W., Wickramasinghe, D.T., Ferrario, Lilia, Sullivan, Denis J., Peet, A.J. van der, Buckley, David A.H., Chen, A.-L.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:1995
País:Brasil
Institución:Universidade Federal do Rio Grande do Sul (UFRGS)
Repositorio:Repositório Institucional da UFRGS
Idioma:inglés
OAI Identifier:oai:www.lume.ufrgs.br:10183/108901
Acceso en línea:http://hdl.handle.net/10183/108901
Access Level:acceso abierto
Palabra clave:Astrofisica estelar
Estrelas variaveis
Pulsacoes estelares
Anãs brancas
Stars: individual (G226-29)
Stars: oscillations
Stars: rotation
White dwarfs
Descripción
Sumario:We observed G226-29 for 121 hr in 1992 February and confirm the presence of the three previously identified frequencies close to 109 s. We find no evidence of other pulsation periods down to our noise level of about 0.35 millimodulation amplitudes. The presence of only one triplet pulsation mode in G226-29 and its effective temperature near the blue edge of the instability strip identify the observed triplet of modes near 109 s as rotationally split components of the k = 1, l = 1 mode. With the mode identification, we derived a rotation period of 8.9 hr and an inclination of the pulsation axis of 70°-75° to our line of sight.

Similares en LA Referencia