Spectroscopic analysis of DA white dwarfs with 3D model atmospheres

By P.-E. Tremblay, H. Ludwig, M. Steffen, Bernd Freytag. 2013

161 citations recorded by the source corpus.

We present the first grid of mean three-dimensional (3D) spectra for pure-hydrogen (DA) white dwarfs based on 3D model atmospheres. We use CO 5 BOLD radiation-hydrodynamics 3D simulations instead of the mixing-length theory for the treatment of convection. The simulations cover the effective temperature range of 6000 < Teff (K) < 15 000 and the surface gravity range of 7 < log g< 9 where the large majority of DAs with a convective atmosphere are located. We rely on horizontally averaged 3D structures (over ... ... ... ... ... ...

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/947ae1fa886a467ea17cecb780dd46b4ff074703

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Citations in the corpus

Magnetic White Dwarfs (2015, background): “The most recent estimate for the mean mass of non-magnetic DA WDs is 0.663 ± 0.136M⊙ (Tremblay et al. 2013).”
White Dwarf Rotation as a Function of Mass and a Dichotomy of Mode Line Widths: Kepler Observations of 27 Pulsating DA White Dwarfs through K2 Campaign 8 (2017, methodology): “We use the analytic functions based on the three-dimensional (3D) convection simulations of Tremblay et al. (2013) to correct these 1D values to 3D atmospheric parameters, which we list in Table 3 as T 3Deff - and glog 3D- .”
AGaiaData Release 2 catalogue of white dwarfs and a comparison with SDSS (2018, background): “…Hollands et al. 2018), kinematic properties (Wegg & Phinney 2012), mass distribution (Bergeron et al. 1992; Liebert et al. 2005; Falcon et al. 2010; Tremblay et al. 2013, 2016), and age or luminosity distributions (Catalán et al. 2008; Giammichele et al. 2012; Tremblay et al. 2014;…”
New white dwarf stars in the Sloan Digital Sky Survey Data Release 10 (2014, methodology): “…but now closer to the results of other determinations methods, as gravitational redshift (Falcon et al. 2010) and seismology (Romero et al. 2012), and especially with the Gianninas, Bergeron, & Ruiz (2011) sample of bright DAs corrected to 3D by Tremblay et al. (2013) which is centred at 0.637 M⊙.”
Formation of planetary debris discs around white dwarfs – I. Tidal disruption of an extremely eccentric asteroid (2014, background): “The value of 0.6 M may be considered as a fiducial WD mass given the mass distribution of all observed WDs (Liebert, Bergeron & Holberg 2005; Camenzind 2007; Falcon et al. 2010; Tremblay et al. 2013).”
The White Dwarf Initial–Final Mass Relation for Progenitor Stars from 0.85 to 7.5 M⊙ (2018, methodology): “Using the 3D models including convection from Tremblay et al. (2013) would not affect the results.”
Pulsating white dwarfs: new insights (2019, methodology): “On the other hand, the 3D convection studies of Tremblay et al. (2013a, 2015) have converged the determination of temperatures and gravities using different mixing length models, which had plagued prior studies of the location of the ZZ Ceti instability strip.”
New white dwarf and subdwarf stars in the Sloan Digital Sky Survey Data Release 12 (2015, methodology): “We include corrections to Teff and log g based on three–dimensional convection calculations from Tremblay et al. (2013).”