Estimating the mass of the debris disc in HD 69830

Abstract

We present a method to estimate the mass of the debris disc in the HD 69830 system, which also hosts three exoplanets with Neptune-like minimum masses. By considering the range of published stellar ages, we interpret the infrared emission from the debris disc as originating from a steady state, collisional cascade of dust grains. Using dynamical survival models subjected to observational constraints, we estimate the allowed range of disc masses. If the disc has an age of about 1 Gyr, then its mass is several times that of our asteroid belt. The maximum allowed age for the disc and the number of planetesimals it contains are determined by the assumed value for the binding energy of the planetesimals. If one insists on interpreting the disc as being transient, then this mass estimate becomes an upper limit.

Accepted by MNRAS. 4 pages, 2 figures. No changes from previous version, except for corrections of typographical errors and to British English (e.g., "disc")

References in corpus (7)

• Transience of hot dust around sun-like stars
• On the Nature of the Dust in the Debris Disk Around HD69830
• Formation and structure of the three Neptune-mass planets system around HD69830
• Resolving the hot dust around HD69830 and eta Corvi with MIDI and VISIR
• Long-lived planetesimal discs
• The Secular Evolution and Dynamical Architecture of the Neptunian Triplet Planetary System HD 69830
• Dynamical Simulations of the Planetary System HD69830

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• Multi-Epoch Observations of HD69830: High Resolution Spectroscopy and Limits to Variability
• Investigation of the asteroid-neutron star collision model for the repeating fast radio bursts
• How dusty is alpha Centauri? Excess or non-excess over the infrared photospheres of main-sequence stars
• Planetary system architectures with low-mass inner planets: Direct imaging exploration of mature systems beyond 1 au