KNOW YOUR NEIGHBORHOOD: A DETAILED MODEL ATMOSPHERE ANALYSIS OF NEARBY WHITE DWARFS
By N. Giammichele, Pierre Bergeron, Patrick Dufour. 2012
173 citations recorded by the source corpus.
We present improved atmospheric parameters of nearby white dwarfs lying within 20 pc of the Sun. The aim of the current study is to obtain the best statistical model of the least-biased sample of the white dwarf population. A homogeneous analysis of the local population is performed combining detailed spectroscopic and photometric analyses based on improved model atmosphere calculations for various spectral types including DA, DB, DC, DQ, and DZ stars. The spectroscopic technique is applied to all stars in our sample for which optical spectra are available. Photometric energy distributions, when available, are also combined to trigonometric parallax measurements to derive effective temperatures, stellar radii, as well as atmospheric compositions. A revised catalog of white dwarfs in the solar neighborhood is presented. We provide, for the first time, a comprehensive analysis of the mass distribution and the chemical distribution of white dwarf stars in a volume-limited sample.
Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics
View Paper: https://www.semanticscholar.org/paper/7518075175c8d9874ceed6346d8f2874055baaed
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Citations in the corpus
- AGaiaData Release 2 catalogue of white dwarfs and a comparison with SDSS (2018, background): “…(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; Rebassa-Mansergas et al. 2015; Kilic et al. 2017).”
- Stellar and substellar companions of nearby stars from Gaia DR2 (2018, methodology): “When not available for a given star, the (K,V−K) surface brightness-color relation by Kervella et al. (2004) was employed to estimate the radius, and a fixed mass of 0.6 ± 0.2 M was assumed (from the mass distribution by Finley et al. 1997; see also Giammichele et al. 2012).”
- The frequency of planetary debris around young white dwarfs (2014, background): “1 resembles closely that of larger well-studied samples (Finley et al. 1997; Liebert et al. 2005; Giammichele et al. 2012), displaying besid s the dominant population around a mean mass of 0.6M⊙ two additional peaks near≈0.4 M⊙ and≈0.8 M⊙.”
- Magnetic White Dwarfs (2015, background): “3.4 Beyond hydrogen The bulk of all WDs have hydrogen-dominated atmospheres, both in magnitudelimited (Kleinman et al. 2013) and volume-limited samples (Giammichele et al. 2012), and the same is true for MWDs.”