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- W4313263106 abstract "The persistence of planetary systems after their host stars evolve into their post-main sequence phase is poorly constrained by observations. Many young white dwarf systems exhibit infrared excess emission and/or spectral absorption lines associated with a reservoir of dust (or planetesimals) and its accretion. However, most white dwarfs are too cool to sufficiently heat any circumstellar dust to detectable levels of emission. The Helix Nebula (NGC 7293) is a young, nearby planetary nebula; observations at mid- and far-infrared wavelengths revealed excess emission associated with its central white dwarf (WD 2226-210). The origin of this excess is ambiguous. It could be a remnant planetesimal belt, a cloud of comets, or the remnants of material shed during the post-asymptotic giant branch phase. Here we combine infrared (SOFIA, Spitzer, Herschel ) and millimetre (ALMA) observations of the system to determine the origin of this excess using multi-wavelength imaging and radiative transfer modelling. We find the data are incompatible with a compact remnant planetesimal belt or post-asymptotic giant branch disc, and conclude the dust most likely originates from deposition by a cometary cloud. The measured dust mass, and lifetime of the constituent grains, implies disruption of several thousand Hale-Bopp equivalent comets per year to fuel the observed excess emission around the Helix Nebula's white dwarf." @default.
- W4313263106 created "2023-01-06" @default.
- W4313263106 creator A5000235602 @default.
- W4313263106 creator A5007484889 @default.
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- W4313263106 creator A5052844813 @default.
- W4313263106 creator A5071774310 @default.
- W4313263106 creator A5074560289 @default.
- W4313263106 creator A5074813346 @default.
- W4313263106 creator A5075738144 @default.
- W4313263106 date "2022-12-19" @default.
- W4313263106 modified "2023-10-14" @default.
- W4313263106 title "Evidence for the Disruption of a Planetary System During the Formation of the Helix Nebula" @default.
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