The Potential of White Dwarf Cosmochronology

By G. Fontaine, P. Brassard, Pierre Bergeron. 2001

596 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/35ec54f997c1ade6864c0feb0902d9dfa5691b53

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In Astronomy and Astrophysics

1. Pierre Bergeron
2. J. Farihi
3. P.-E. Tremblay
4. B. Gänsicke
5. A. Gianninas
6. D. Koester
7. Patrick Dufour
8. M. Ruiz

In Instrumentation

1. Pierre Bergeron
2. J. Farihi
3. P.-E. Tremblay
4. A. Gianninas
5. B. Gänsicke
6. M. Ruiz
7. D. Koester
8. Patrick Dufour

Citations in the corpus

• On the Spectral Evolution of Cool, Helium-Atmosphere White Dwarfs: Detailed Spectroscopic and Photometric Analysis of DZ Stars (2007, methodology): “…obtained from trigonometric parallax measurements, we can obtain the radius of the star from the solid angle from our modeling, which in turn can be converted into log g (or mass) using evolutionary models similar to those described in Fontaine et al. (2001) but with C/O cores, q(He) log (MHe /M?)”
• The White Dwarf Luminosity Function from Sloan Digital Sky Survey Imaging Data (2005, unknown): “No feature is predicted (Fontaine et al. 2001) from a pause in WD cooling and dimming.”
• A SPECTROSCOPIC SURVEY AND ANALYSIS OF BRIGHT, HYDROGEN-RICH WHITE DWARFS (2011, methodology): “Although the Montréal group has computed evolutionary models of their own (Fontaine et al. 2001), these are better suited for the cooler end of the white dwarf cooling sequence.”
• KNOW YOUR NEIGHBORHOOD: A DETAILED MODEL ATMOSPHERE ANALYSIS OF NEARBY WHITE DWARFS (2012, methodology): “The radius is then converted into mass using evolutionary models similar to those described in Fontaine et al. (2001) but with C/O cores, q(He) ≡ logMHe/M⋆ = 10−2 and q(H) = 10−4, which are representative of hydrogen-atmosphere white dwarfs, and q(He) = 10−2 and q(H) = 10−10, which are…”
• Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars (2016, background): “According to evolutionary tracks, a WD cools to TWD ≈ 15,000 K in tcool ≈ 0.15 - 0.60 Gyr, depending on its mass and composition (Fontaine et al. 2001).”
• Evolutionary and pulsational properties of white dwarf stars (2010, background): “The second reason is more subtle and has been largely overlooked until recently (Fontaine et al. 2001).”
• A COMPREHENSIVE SPECTROSCOPIC ANALYSIS OF DB WHITE DWARFS (2011, methodology): “The stellar mass (M) and white dwarf cooling age (log τ) of each star are obtained from evolutionary models similar to those described in Fontaine et al. (2001) but with C/O cores, q(He) ≡ logMHe/M⋆ = 10 −2 and q(H) = 10−10, which are representative of helium-atmosphere white dwarfs.”
• Spectroscopic analysis of DA white dwarfs with 3D model atmospheres (2013, methodology): “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.”
• Calibration of Synthetic Photometry Using DA White Dwarfs (2005, background): “…dwarf fluxes predicted at the top of the Earth’s atmosphere fobs (k) as follows: fobs(k)¼ 4 R2 D2 Hk; ð4Þ where Hk is the white dwarf Eddington flux, R is the radius of the white dwarf defined by the Wood (1995) and Fontaine et al. (2001) mass-radius relations, and D is a stellar distance of 10 pc.”
• 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 used the C/O-core models of Fontaine et al. (2001) to determine the mass of SDSS J0358+1324, but this DAV is very near the boundary for He-core white dwarfs.”
• AN IMPROVED SPECTROSCOPIC ANALYSIS OF DA WHITE DWARFS FROM THE SLOAN DIGITAL SKY SURVEY DATA RELEASE 4 (2011, methodology): “We convert log g values into stellar masses using the evolutionary models with thick hydrogen layers of Fontaine et al. (2001) below Teff < 30, 000 K and of Wood (1995) above this temperature; we also provide in Table 1 the corresponding white dwarf cooling time (log τ).”
• The age, life expectancy, and space density of Post Common Envelope Binaries (2003, background): “Some uncertainties in the theoretical models remain at the low-temperature end of the white dwarf luminosity function, and are relevant primarily for the cosmo-chronological interpretation of the coldest (halo) white dwarfs (see the reviews by Fontaine et al. 2001; Koester 2002).”
• Experimental astrophysics with high power lasers and Z pinches (2004, background): “White dwarfs are interesting in their own right, but also serve as “cosmochronometer” Fontaine et al., 2001 , and when accreting from a binary partner, form the initial conditions for a type-I SN. Extended duration radiation sources will be available, which will be ideal for experimental studies of…”
• The Progenitors of Type Ia Supernovae (2012, background): “Some other processes, such as carbon and oxygen separation or crystallization, may occur and dominate the properties of the CO WD (Fontaine et al., 2001).”
• The Detailed Star Formation History in the Spheroid, Outer Disk, and Tidal Stream of the Andromeda Galaxy (2006, background): “…Italy; arenzini@pd.astro.it 7 Code 667, NASA Goddard Space Flight Center, Greenbelt, MD 20771; allen.v.sweigart@nasa.gov, randy.a.kimble@nasa.gov et al. 2003 ; McWilliam & Rich 1994), and a disk hosting a wide range of ages and metallicities (e.g., Fontaine et al. 2001; Ibukiyama & Arimoto 2002).”
• NEW COOLING SEQUENCES FOR OLD WHITE DWARFS (2010, background): “Second, we corroborate the importance of convective coupling at low luminosity in the cooling of white dwarfs, as originally suggested by Fontaine et al. (2001).”