NEW COOLING SEQUENCES FOR OLD WHITE DWARFS

By I. Renedo, L. Althaus, M. M. Bertolami, A. Romero, A. Córsico, R. Rohrmann, E. García–Berro. 2010

171 citations recorded by the source corpus.

We present full evolutionary calculations appropriate for the study of hydrogen-rich DA white dwarfs. This is done by evolving white dwarf progenitors from the zero-age main sequence, through the core hydrogen-burning phase, the helium-burning phase, and the thermally pulsing asymptotic giant branch phase to the white dwarf stage. Complete evolutionary sequences are computed for a wide range of stellar masses and for two different metallicities, Z = 0.01, which is representative of the solar neighborhood, and Z = 0.001, which is appropriate for the study of old stellar systems, like globular clusters. During the white dwarf cooling stage, we self-consistently compute the phase in which nuclear reactions are still important, the diffusive evolution of the elements in the outer layers and, finally, we also take into account all the relevant energy sources in the deep interior of the white dwarf, such as the release of latent heat and the release of gravitational energy due to carbon–oxygen phase separation upon crystallization. We also provide colors and magnitudes for these sequences, based on a new set of improved non-gray white dwarf model atmospheres, which include the most up-to-date physical inputs like the Lyα quasi-molecular opacity. The calculations are extended down to an effective temperature of 2500 K. Our calculations provide a homogeneous set of evolutionary cooling tracks appropriate for mass and age determinations of old DA white dwarfs and for white dwarf cosmochronology of the different Galactic populations.

Subfields: Astronomy and Astrophysics, Education, Instrumentation

View Paper: https://www.semanticscholar.org/paper/88dcfb02971c1942fe6c7d264e1219d438bd9bbb

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Citations in the corpus

New white dwarf stars in the Sloan Digital Sky Survey Data Release 10 (2014, methodology): “We use the mass–radius relations of Renedo et al. (2010) and Romero, Campos & Kepler (2014) carbon– oxygen DA white dwarfs, for solar metallicities, to calculate the mass of our identified clean DA stars from the Teff and log g values obtained from our fits, corrected to 3D convection.”
Evolutionary and pulsational properties of white dwarf stars (2010, background): “These values strongly depend on the stellar mass of the white dwarf (Renedo et al. 2010), and on the occurrenceof LTP episodes, which may reduce the mass of the remnant H and He buffer considerably, see Sect.”
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, background): “Our overall mass estimates do not change by more than the adopted uncertainties (0.04Me for all white dwarfs here) if we instead use the models of Renedo et al. (2010), which have more realistic carbon–oxygen profiles resulting from full evolutionary sequences.”
SDSS DR7 WHITE DWARF CATALOG (2012, methodology): “To calculate the mass of our identiﬁed clean DA and DB stars from the T eff and log g values obtained from our ﬁts, we used the mass–radius relations of Renedo et al. (2010) for carbon–oxygen DA white dwarfs.”
On the Spectral Evolution of Hot White Dwarf Stars. I. A Detailed Model Atmosphere Analysis of Hot White Dwarfs from SDSS DR12 (2020, background): “Nevertheless, we verified that these extrapolated sequences behave similarly to existing evolutionary calculations, such as those of Althaus et al. (2009) and Renedo et al. (2010).”
Spectroscopic analysis of DA white dwarfs with 3D model atmospheres (2013, background): “In the latter case, a theoretical sequence (Fontaine et al. 2001; Renedo et al. 2010) with a given internal composition is usually assumed, although the relation varies by 3−5% whether a thick or thin hydrogen layer is chosen.”
New white dwarf and subdwarf stars in the Sloan Digital Sky Survey Data Release 12 (2015, methodology): “We use the mass–radius relations of Renedo et al. (2010) and Romero, Campos, & Kepler (2015) for carbon– oxygen DA white dwarfs with solar metallicities to calculate the mass of our identified DA stars from the Teff and log g values obtained from our fits, after correcting to 3D convec- tion.”
Revisiting the axion bounds from the Galactic white dwarf luminosity function (2014, methodology): “A detailed description of the code is available in [27] and references therein, here we only mention those which are most relevant for the present work.”
SUB-CHANDRASEKHAR MASS MODELS FOR SUPERNOVAE (2010, background): “Cooling to 0.01 L takes about 200 Myr, while cooling to 1 L , in the absence of accretion only takes about 10 Myr (Renedo et al. 2010), comparable to the accretion time.”