Dusty Disks Around PG1159 Stars

Details Dusty Disks Around PG1159 Stars Dusty Disks Around PG1159 Stars

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop50168d&link_type=abstract

Spitzer Proposal ID #50168

Computer Science

Scientific paper

The recent detection of old dusty white dwarfs (WDs) has been interpreted as signaling the presence of debris disks around these objects. Alternatively, this WD dust could be a remnant from the asymptotic giant branch phase. In any case, this old circumstellar dust is of great interest because it has survived for long periods around very hot stars. The dusty environments of the hydrogen-deficient central stars of planetary nebula (PN) have, since the days of ISO, raised similar questions about dust lifetimes, processing, and how different types of dust can be used as markers for different evolutionary channels. The PG1159 central stars are the last phase of the evolution of the hydrogen-deficient central stars of PN, just before the PN disperses and the star becomes a non-DA WD. Half of these stars are bright IRAS sources indicating that, like their progenitors, they are dusty. We seek to obtain IRS spectra of these IRAS-detected PG1159 stars, to determine dust composition and spatial distribution, which can help to answer: (i) how dust evolves with age and how it can survive so that it is still present around older WDs, and (ii) how dust evolution can be coupled to stellar evolution to aid in the determination of evolutionary channels.

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