A Gaseous Metal Disk Around a White Dwarf
Abstract
The destiny of planetary systems through the late evolution of their host stars is very uncertain. We report a metal-rich gas disk around a moderately hot and young white dwarf. A dynamical model of the double-peaked emission lines constrains the outer disk radius to just 1.2 solar radii. The likely origin of the disk is a tidally disrupted asteroid, which has been destabilized from its initial orbit at a distance of more than 1000 solar radii by the interaction with a relatively massive planetesimal object or a planet. The white dwarf mass of 0.77 solar mass implies that planetary systems may form around high-mass stars.
- Publication:
-
Science
- Pub Date:
- December 2006
- DOI:
- 10.1126/science.1135033
- arXiv:
- arXiv:astro-ph/0612697
- Bibcode:
- 2006Sci...314.1908G
- Keywords:
-
- ASTRONOMY;
- Astrophysics
- E-Print:
- Published 22 December in Science, added journal ref