Metal Lines in DA White Dwarfs

By B. Zuckerman, D. Koester, I. Neill Reid, M. Hünsch. 2003

370 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/b804410d15b085eb2d8ed37e803558d31e17130b

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Dynamical effects of stellar mass-loss on a Kuiper-like belt (2011, background): “1 IN T RO D U C T I O N Keck observations of cool single DA white dwarfs find that ∼25 per cent of them contain elements heavier than helium in their spectra (Zuckerman et al. 2003).”
The frequency of planetary debris around young white dwarfs (2014, background): “The bottom panel shows log(Ca/H) abundances (open circles and stars) and upper limits (gray dots) from Koester & Wilken (2006) (compiled from Zuckerman et al. 2003; Berger et al. 2005).”
THE LINK BETWEEN PLANETARY SYSTEMS, DUSTY WHITE DWARFS, AND METAL-POLLUTED WHITE DWARFS (2012, background): “…feature, careful abundance analysis of narrow metal lines in the photosphere of the target white dwarf, or detection of gaseous emission lines (Zuckerman et al. 2003; Koester et al. 2005; Reach et al. 2005; Kilic et al. 2006; Gänsicke et al. 2006; von Hippel et al. 2007; Farihi et al. 2010;…”
Magnetic White Dwarfs (2015, background): “Yet, ∼ 25% of all WDs show traces of metals – most commonly Ca and Si, but also Mg, Fe, Na and other elements (Zuckerman et al. 2003; Koester et al. 2014).”
Circumstellar Debris and Pollution at White Dwarf Stars (2016, background): “These results strongly corroborate the pioneering studies based on optical, high-resolution spectroscopy, accounting for various differences in target properties and instrumentation (Zuckerman et al., 2003; Koester et al., 2005; Zuckerman et al., 2010).”
A SPECTROSCOPIC SURVEY AND ANALYSIS OF BRIGHT, HYDROGEN-RICH WHITE DWARFS (2011, background): “Indeed, Kilkenny et al. (1997) find Teff = 7000 K while Zuckerman et al. (2003) find Teff = 8000 K, in both cases the temperature is determined solely from a measurement of (B − V ).”
Debris Disks around White Dwarfs: The DAZ Connection (2006, background): “Yet Zuckerman et al. (2003) did not find any correlation between the locations and relatively large numbers of DAZs and the locations and amount of ISM present within the local bubble.”
The Dust Cloud around the White Dwarf G29-38 (2005, background): “As discussed by Zuckerman et al. (2003), the photospheric metals could be accreted from interstellar gas, but then the star would need to be within a dense cloud (because the lifetime of metals in the photosphere [!”
INFRARED SIGNATURES OF DISRUPTED MINOR PLANETS AT WHITE DWARFS (2009, background): “For DA white dwarfs, it is easier to detect metals in cooler stars and, in a survey that focused primarily on DA white dwarfs cooler than 10,000 K, Zuckerman et al. (2003) found that of order 25% displayed a calcium K line.”
ANCIENT PLANETARY SYSTEMS ARE ORBITING A LARGE FRACTION OF WHITE DWARF STARS (2010, background): “…at Mauna Kea Observatory revealed that ∼25% of cool DA (hydrogen atmosphere) white dwarf photospheres are polluted with elements heavier than helium (Zuckerman et al 2003; hereafter ZKRH03), notwithstanding the short photospheric residence time of such elements before they sink out of sight…”
The Chemical Composition of an Extrasolar Minor Planet (2007, background): “…of metals, notably calcium, in the spectra of numerous white dwarf helium atmospheres (Sion et al. 1990a, 1990b;Koester et al. 2005b;Dufour et al. 2007; and references therein) and hydrogen atmospheres (Zuckerman et al. 2003; Koester et al. 2005b), stimulated a suite of explanatory models.”
Externally Polluted White Dwarfs with Dust Disks (2007, background): “…in white dwarfs cooler than 20,000 K that their atmospheres are expected to be pure hydrogen or pure helium (Paquette et al. 1986), and the ∼20% of these stars which exhibit photospheric metals are thought to be externally polluted (Wolff et al. 2002, Zuckerman et al. 2003, Koester & Wilkin 2006).”
FORETELLINGS OF RAGNARÖK: WORLD-ENGULFING ASYMPTOTIC GIANTS AND THE INHERITANCE OF WHITE DWARFS (2012, background): “…metal-polluted atmospheres or with circumstellar discs strongly suggests that planets, feeding asteroidal or cometary material to locations close to the star, exist around these degenerate stellar remnants (Zuckerman et al. 2003; Gänsicke et al. 2006; Farihi et al. 2009; Gänsicke et al. 2012).”
KNOW YOUR NEIGHBORHOOD: A DETAILED MODEL ATMOSPHERE ANALYSIS OF NEARBY WHITE DWARFS (2012, background): “The objects displayed in red in Figure 19 are double degenerate binaries that have been confirmed through radial velocity measurements: G1-45 (0101+048; Maxted et al. 2000), L870-2 (0135−052; Saffer et al. 1988), and L587-77A (0326−073; Zuckerman et al. 2003).”
POLLUTION OF SINGLE WHITE DWARFS BY ACCRETION OF MANY SMALL ASTEROIDS (2008, methodology): “Furthermore, there is no correlation between metal contamination and the star’s space motion as would be expected from Bondi-Hoyle accretion theory (Zuckerman et al. 2003, Koester & Wilken 2006).”
Low-Luminosity Companions to White Dwarfs (2005, background): “Zuckerman et al. (2003) report Teff = 7660 K and log g = 7.80 from UBV RI photometry and parallax (which must be the same photometric parallax mentioned above).”
Simulations of two-planet systems through all phases of stellar evolution: implications for the instability boundary and white dwarf pollution (2013, background): “Heavier elements sink rapidly in such thin atmospheres and it is therefore puzzling that such a high fraction of WDs have evidence for metal pollutants in their spectra (25 per cent of single DA WDs; Zuckerman et al. 2003).”
Dawes Review 6: The Impact of Companions on Stellar Evolution (2016, background): “Between a quarter and half of all WDs exhibit some degree of pollution (Zuckerman et al., 2003, 2010; Barstow et al., 2014; Koester, Gänsicke, & Farihi, 2014).”