Post-main sequence evolution of debris discs

Details Post-main sequence evolution of debris discs Post-main sequence evolution of debris discs

Nov 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1273..482b&link_type=abstract

17TH EUROPEAN WHITE DWARF WORKSHOP. AIP Conference Proceedings, Volume 1273, pp. 482-487 (2010).

Other

White Dwarfs, Circumstellar Matter, Stellar Photospheres, Planetary Nebulae, Faint Blue Stars, White Dwarfs, Degenerate Stars, Nuclei Of Planetary Nebulae, Physical Properties, Stellar Atmospheres, Radiative Transfer, Opacity And Line Formation, Planetary Nebulae

Scientific paper

Observations of dusty discs around white dwarfs suggest a link between white dwarfs and evolved planetary systems. The population of debris discs on the main sequence is well constrained. In this work we present models that evolve this population through to the white dwarf phase. Evolved main sequence debris discs are hard to detect around whtie dwarfs. The best chances are for hot young white dwarfs, fitting nicely with the observations for the example the infrared excess at the centre of the helix [1] and 9 other planetary nebula (Chu& Bilikova-this volume), although our baseline models do not predict such a high rate of detectable discs. Evolved main sequence debris discs potentially provide the reservoir of material required to replenish the hot dusty discs obsevred within the tidal radius.

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