Measuring the evolutionary rate of cooling of ZZ Ceti

• Autores: Mukadam, Anjum S.; Bischoff Kim, Agnes; Fraser, Oliver; Corsico, Alejandro Hugo; Montgomery, M. H.; Kepler, S. O.; Romero, A. D.; Winget, D. E.; Hermes, J. J.; Riecken, T. S.; Kronberg, M. E.; Winget, K. I.; Falcon, Ross E.; Chandler, D. W.; Kuehne, J. W.; Sullivan, D. J.; Reaves, D.; von Hippel, T.; Mullally, F.; Shipman,H.; Thompson, S. E.; Silvestri, N. M.; Hynes, R. I.
• Año de publicación: 2013
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: Evolution of stars; ZZ Ceti R548 (estrella); Pulsations; Variable stars; White dwarfs
• Institución: Consejo Nacional de Investigaciones Científicas y Técnicas

We have finally measured the evolutionary rate of cooling of the pulsating hydrogen atmosphere (DA) white dwarf ZZ Ceti (Ross 548), as reflected by the drift rate of the 213.13260694 s period. Using 41 yr of time-series photometry from 1970 November to 2012 January, we determine the rate of change of this period with time to be dP/dt = (5.2 ± 1.4) × 10–15 s s–1 employing the O – C method and (5.45 ± 0.79) × 10–15 s s–1 using a direct nonlinear least squares fit to the entire lightcurve. We adopt the dP/dt obtained from the nonlinear least squares program as our final determination, but augment the corresponding uncertainty to a more realistic value, ultimately arriving at the measurement of dP/dt = (5.5 ± 1.0) × 10–15 s s–1. After correcting for proper motion, the evolutionary rate of cooling of ZZ Ceti is computed to be (3.3 ± 1.1) × 10–15 s s–1. This value is consistent within uncertainties with the measurement of (4.19 ± 0.73) × 10–15 s s–1 for another similar pulsating DA white dwarf, G 117-B15A. Measuring the cooling rate of ZZ Ceti helps us refine our stellar structure and evolutionary models, as cooling depends mainly on the core composition and stellar mass. Calibrating white dwarf cooling curves with this measurement will reduce the theoretical uncertainties involved in white dwarf cosmochronometry. Should the 213.13 s period be trapped in the hydrogen envelope, then our determination of its drift rate compared to the expected evolutionary rate suggests an additional source of stellar cooling. Attributing the excess cooling to the emission of axions imposes a constraint on the mass of the hypothetical axion particle.
Fil: Mukadam, Anjum S. . University of Washington; Estados Unidos
Fil: Bischoff Kim, Agnes . Georgia State University; Estados Unidos
Fil: Fraser, Oliver. University of Washington; Estados Unidos
Fil: Corsico, Alejandro Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina
Fil: Montgomery, M. H. . University of Texas at Austin; Estados Unidos
Fil: Kepler, S. O. . Universidade Federal do Rio Grande do Sul; Brasil
Fil: Romero, A. D. . Universidade Federal do Rio Grande do Sul; Brasil
Fil: Winget, D. E. . University of Texas at Austin; Estados Unidos
Fil: Hermes, J. J. . University of Texas at Austin; Estados Unidos
Fil: Riecken, T. S. . Washington State University; Estados Unidos
Fil: Kronberg, M. E. . University of Washington; Estados Unidos
Fil: Winget, K. I. . University of Texas at Austin; Estados Unidos
Fil: Falcon, Ross E. . University of Texas at Austin; Estados Unidos
Fil: Chandler, D. W. . Central Texas Astronomical Society. Meyer Observatory; Estados Unidos
Fil: Kuehne, J. W. . McDonald Observatory; Estados Unidos
Fil: Sullivan, D. J. . Victoria University of Wellington; Nueva Zelanda
Fil: Reaves, D. . University of Texas at Austin; Estados Unidos
Fil: von Hippel, T. . Embry-Riddle Aeronautical University; Estados Unidos
Fil: Mullally, F. . National Aeronautics And Space Administration; Estados Unidos
Fil: Shipman,H. . Delaware Asteroseismic Research Center; Estados Unidos
Fil: Thompson, S. E. . National Aeronautics And Space Administration; Estados Unidos
Fil: Silvestri, N. M. . University of Washington; Estados Unidos
Fil: Hynes, R. I. . State University Of Louisiana; Estados Unidos