2014
DOI: 10.1051/0004-6361/201423691
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The frequency of planetary debris around young white dwarfs

Abstract: Context. Heavy metals in the atmospheres of white dwarfs are thought in many cases to be accreted from a circumstellar debris disk, which was formed by the tidal disruption of a rocky planetary body within the Roche radius of the star. The abundance analysis of photospheric elements and conclusions about the chemical composition of the accreted matter are a new and promising method of studying the composition of extrasolar planetary systems. However, ground-based searches for metal-polluted white dwarfs that r… Show more

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Cited by 439 publications
(557 citation statements)
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“…More specifically and importantly, the predictions of PR drag on white dwarf disks can account for the full range of instantaneous accretion rates (Rafikov, 2011a;, including all the DAZ stars with diffusion timescales less than 1000 yr. That is, the PR drag model successfully describes the subset of white dwarfs where ongoing, steady-state accretion is likely. Moreover, the disk lifetimes predicted by these models are a good match to those inferred from observations based on 1) the fraction of polluted white dwarfs over a given range of cooling ages Koester et al, 2014), 2) the mass of metals in the outer layers of convective stars divided by typical accretion rates , or 3) the steady-state accretion phase necessary for self-consistent oxygen chemistry (Klein et al, 2011). These combined theoretical and empirical data support a picture where the most prominent disks have m 10 20 g and hence parent bodies with d 40 km .…”
Section: Disk Accretion and Lifetimesupporting
confidence: 69%
“…More specifically and importantly, the predictions of PR drag on white dwarf disks can account for the full range of instantaneous accretion rates (Rafikov, 2011a;, including all the DAZ stars with diffusion timescales less than 1000 yr. That is, the PR drag model successfully describes the subset of white dwarfs where ongoing, steady-state accretion is likely. Moreover, the disk lifetimes predicted by these models are a good match to those inferred from observations based on 1) the fraction of polluted white dwarfs over a given range of cooling ages Koester et al, 2014), 2) the mass of metals in the outer layers of convective stars divided by typical accretion rates , or 3) the steady-state accretion phase necessary for self-consistent oxygen chemistry (Klein et al, 2011). These combined theoretical and empirical data support a picture where the most prominent disks have m 10 20 g and hence parent bodies with d 40 km .…”
Section: Disk Accretion and Lifetimesupporting
confidence: 69%
“…A literature search reveals that at least 39 stars in the sample have known pollution (7%). HST COS observations of a sub-set (85 stars) find a pollution rate of at least 27% (Koester et al 2014), suggesting a similar rate of pollution for the full sample. This compares well to typical pollution rates observed for other samples of white dwarfs.…”
Section: The Distribution Of Infrared Excessesmentioning
confidence: 75%
“…This expectation is corroborated by the detection of debris accreted into the photospheres of white dwarfs, resulting from the tidal disruption (Debes & Sigurdsson 2002;Jura 2003) of planetary bodies among ;25%-50% of all white dwarfs (Zuckerman et al 2003;Koester et al 2014). Little is known so far regarding the detailed nature of the disrupted objects, the exact origin within their planetary systems, and the processes resulting in their disintegration and subsequent circularization (Debes et al 2012;Veras et al 2014bVeras et al , 2015c) and leading to dusty debris disks with typical radii of ;1 R  , which have been detected as infrared excess to ;40 white dwarfs (Rocchetto et al 2015).…”
Section: Introductionmentioning
confidence: 78%