A gaseous metal disk around a white dwarf.
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.
Gänsicke
B T
BT
Department of Physics, University of Warwick, Coventry CV4 7AL, UK. boris.gaensicke@warwick.ac.uk
Marsh
T R
TR
Southworth
J
J
Rebassa-Mansergas
A
A