An intensive study of the planetary debris disks around the single white dwarfs SDSS1228+1040 and SDSS1043+0855

Details An intensive study of the planetary debris disks around the single white dwarfs SDSS1228+1040 and SDSS1043+0855 An intensive study of the planetary debris disks around the single white dwarfs SDSS1228+1040 and SDSS1043+0855

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007sptz.prop40048b&link_type=abstract

Spitzer Proposal ID #40048

Computer Science

Scientific paper

While > 200 extrasolar planets orbiting main sequence stars have been discovered, the destiny of planetary systems through the late stages of evolution of their host stars is very uncertain, and no planet has been found around a white dwarf. We have identified metal-rich gas disks around two relatively young white dwarfs, SDSS 1228+1040 and SDSS 1043+0855. A dynamical model of the double-peaked emission lines constrains the outer disk radius in SDSS 1228+1040 to just 1.2 solar radii. The likely origin of such a disk is a tidally distrupted asteroid, which has been destabilised from its initial orbit of more than 1000 solar radii by the interaction with a relatively massive planetessimal object or a planet. Here we propose a Spitzer study to test for a cooler, dusty extension to the gaseous disks around both white dwarfs. In particular we will model the mass of material in the disks, thereby placing tighter constraints on their origin and evolution. In the unlikely event that we fail to detect a cooler extension to the gaseous disks, we will have an even more exciting problem on our hands, with the possibility that the disks are either extraordinarily young and are still in the process of spreading, or they are somehow prevented from spreading by as-yet undetected, extremely low-mass companions to the white dwarfs.

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