Non-LTE Analysis of Gaseous Planetary Debris Disks around White Dwarfs

Details Non-LTE Analysis of Gaseous Planetary Debris Disks around White Dwarfs Non-LTE Analysis of Gaseous Planetary Debris Disks around White Dwarfs

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.3003h&link_type=abstract

American Astronomical Society, ESS meeting #2, #30.03

Astronomy and Astrophysics

Astronomy

Scientific paper

About two dozen white dwarfs (WD) exhibit an IR excess that most likely originates from a circumstellar debris disk formed from ground planetary material. Some of these objects also have gaseous disk components which were discovered by CaII IR triplet emission. Potentially, a quantitative spectral analysis of the gas disk reveals the chemical composition of extrasolar planetary material around WDs directly. This method is in contrast to the hitherto employed method that uses the WD atmosphere as a "detector" of accreted material. The latter method may suffer from uncertainties in our knowledge of gravitational settling of heavy elements in WD atmospheres. We have constructed models for metallic gas disks with detailed non-LTE radiation transfer and successfully apply them to fit optical and UV spectra of a particular object.

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