Discovery of an ultramassive pulsating white dwarf

• Autor(a) principal: Hermes, James J.
• Data de Publicação: 2013
• Outros Autores: Kepler, Souza Oliveira, Castanheira, Bárbara Garcia, Gianninas, Alexandros, Winget, Donald Earl, Montgomery, Michael Houston, Brown, Warren R., Harrold, Samuel T.
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Institucional da UFRGS
• Texto Completo: http://hdl.handle.net/10183/109061
• topic: Evolucao estelar; Pulsacoes estelares; Espectros estelares; Anãs brancas; Stars: evolution; Stars: individual (GD 518); Stars: oscillations; Stars: variables: general; Supernovae: general; White dwarfs

We announce the discovery of themostmassive pulsating hydrogen-atmosphere white dwarf (WD) ever discovered, GD 518. Model atmosphere fits to the optical spectrum of this star show it is a 12,030 ± 210 K WD with a log g = 9.08 ± 0.06, which corresponds to a mass of 1.20 ± 0.03M . Stellar evolution models indicate that the progenitor of such a high-mass WD endured a stable carbon-burning phase, producing an oxygen–neon-core WD. The discovery of pulsations in GD 518 thus offers the first opportunity to probe the interior of a WD with a possible oxygen–neon core. Such amassiveWDshould also be significantly crystallized at this temperature. The star exhibits multi-periodic luminosity variations at timescales ranging from roughly 425 to 595 s and amplitudes up to 0.7%, consistent in period and amplitude with the observed variability of typical ZZ Ceti stars, which exhibit non-radial g-mode pulsations driven by a hydrogen partial ionization zone. Successfully unraveling both the total mass and core composition of GD 518 provides a unique opportunity to investigate intermediate-mass stellar evolution, and can possibly place an upper limit to the mass of a carbon–oxygen-core WD, which in turn constrains Type Ia supernovae progenitor systems.