Mass and eccentricity constraints on the planetary debris orbiting the white dwarf WD 1145+017

Abstract

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 a tenth of the mass of Ceres or orbits that are not nearly circular 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.

Siendo la primera de su tipo, la enana blanca WD 1145+017 muestra un complejo sistema de planetas orbitándola. Este trabajo usa simulaciones numéricas para determinar restricciones en masa y excentricidad para los cuerpos orbitando WD 1145+017.

Sent la primera de la seva classe, la nana blanca WD 1145+017 llueix un complex sistema de planetes orbitant-la. Aquest treball utilitza simulacions numèriques per determinar restriccions en massa i excentricitat pels objectes orbitant WD 1145+017.