Institut für Astronomie und Astrophysik
Abteilung AstronomieSand 1, D-72076 Tübingen, Germany
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Stephan Hartmann (1), Thorsten Nagel (1), Thomas Rauch (1), and Klaus Werner (1)
(1) Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, D-72076 Tübingen, Germany
To be published in: Proceedings of the 17th European White Dwarf Workshop, AIP Conference Series
Abstract. Around several single DAZ and DBZ white dwarfs metal-rich disks have been observed, which are mostly believed to originate from disruption of smaller rocky planetesimals. In some cases the material does not (only) form a dusty but gaseous disk. In the case of SDSS J122859.93+104032.9 the double peaked infrared Ca II triplet λλ 8498, 8542, 8662 Å, one of only two emission features of the spectra, exhibits a strong red/violet asymmetry. Assuming a composition similar to a chondrite-like asteroid, being the most prominent type in our own solar system, we calculated the spectrum and vertical structure of the disk using the Tübingen non-LTE accretion disk code AcDc. Modified to simulate different non axis-symmetrical disk geometries, the first preliminary results are in good agreement with the observed asymmetric line profile.
Key words: stars: individual (SDSS J122859.93+104032.9), white dwarfs, circumstellar matter, planetary systems
Preprint (1,03 Mb PDF file including figures)
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Last modified 05 Oct 2010