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 destabilised 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 masses implies that planetary systems may form around high-mass stars.
@article{arxiv.astro-ph/0612697,
title = {A gaseous metal disk around a white dwarf},
author = {B. T. Gaensicke and T. R. Marsh and J. Southworth and A. Rebassa-Mansergas},
journal= {arXiv preprint arXiv:astro-ph/0612697},
year = {2007}
}
Comments
Published 22 December in Science, added journal ref