The Impact of White Dwarf Luminosity Profiles on Oscillation Frequencies

• Published in: Astrophysical journal. Letters Vol. 867; no. 2; p. L30
• Main Authors: Timmes, F. X., Townsend, Richard H. D., Bauer, Evan B., Thoul, Anne, Fields, C. E., Wolf, William M.
• Format: Journal Article Web Resource
• Language: English
• Published: Austin The American Astronomical Society 10.11.2018; IOP Publishing; Institute of Physics Publishing; Institute of Physics (IOP)
• Subjects: Accounting; ASTRONOMY AND ASTROPHYSICS; Aérospatiale, astronomie & astrophysique; Luminosity; Neutrinos; Oxygen; Physical, chemical, mathematical & earth Sciences; Physique, chimie, mathématiques & sciences de la terre; Random errors; Space science, astronomy & astrophysics; stars: evolution; stars: individual (KIC 08626021); stars: interiors; stars: oscillations; Stellar evolution; White dwarf stars; white dwarfs
• ISSN: 2041-8205; 2041-8213; 2041-8213
• DOI: 10.3847/2041-8213/aae70f

KIC 08626021 is a pulsating DB white dwarf (WD) of considerable recent interest, and the first of its class to be extensively monitored by Kepler for its pulsation properties. Fitting the observed oscillation frequencies of KIC 08626021 to a model can yield insights into its otherwise-hidden internal structure. Template-based WD models choose a luminosity profile where the luminosity is proportional to the enclosed mass, , independent of the effective temperature Teff. Evolutionary models of young WDs with Teff 25,000 K suggest that neutrino emission gives rise to luminosity profiles with Lr Mr. We explore this contrast by comparing the oscillation frequencies between two nearly identical WD models: one with an enforced luminosity profile, and the other with a luminosity profile determined by the star's previous evolution history. We find that the low-order g-mode frequencies differ by up to 70 Hz over the range of Kepler observations for KIC 08626021. This suggests that by neglecting the proper thermal structure of the star (e.g., accounting for the effect of plasmon neutrino losses), the model frequencies calculated by using an profile may have uncorrected, effectively random errors at the level of tens of Hz. A mean frequency difference of 30 Hz, based on linearly extrapolating published results, suggests a template model uncertainty in the fit precision of 12% in WD mass, 9% in the radius, and 3% in the central oxygen mass fraction.