Authors:Gurri et alAbstract:Being the first of its kind, the white dwarf WD 1145+017 exhibits a complex system of disintegrating debris which offers a unique opportunity to study its disruption process in real time. Even with plenty of transit observations there are no clear constraints on the masses or eccentricities of such debris. Using N-body simulations we show that masses greater than approximately 1020 kg (a tenth of the mass of Ceres) or orbits that are not nearly circular (eccentricity>10−3) dramatically increase the chances of the system becoming unstable within two years, which would contrast with the observational data over this timespan. We also provide a direct comparison between transit phase shifts detected in the observations and by our numerical simulations.
Tuesday, December 20, 2016
Mass and eccentricity constraints on the planetary debris orbiting the white dwarf WD 1145+017
Posted by Will Baird at 12:00 PM
Labels: debris disk, WD 1145+017, white dwarf
Subscribe to: Post Comments (Atom)
Post a Comment
Note: Only a member of this blog may post a comment.