The frequency of planetary debris around young white dwarfs
D. KoesterInstitut fr Theoretische Physik und Astrophysik, Universitt Kiel, 24098 Kiel, GermanyB. T. GänsickeDepartment of Physics, University of Warwick, Coventry CV4 7AL, UKJay FarihiUniversity College London, Department of Physics & Astronomy, Gower Street, London WC1E 6BT, UK
2014en
ABI
Annotatsiya
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 rely primarily on the detection of the Ca ii K line become insensitive at T eff > 15 000 K because this ionization state depopulates.
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