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Estimating the mass of the debris disc in HD 69830

Heng, Kevin

In: Monthly Notices of the Royal Astronomical Society, 2011, vol. 415, no. 4, p. 3365-3368

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    Titre
    • Estimating the mass of the debris disc in HD 69830
    Auteur
    • Heng, Kevin. Zwicky Fellow, ETH Zürich, Institute for Astronomy, Wolfgang-Pauli-Strasse 27, CH-8093 Zürich, Switzerland
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Monthly Notices of the Royal Astronomical Society, 2011, vol. 415, no. 4, p. 3365-3368. Blackwell Publishing Ltd
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:295802
    Summary
    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 t★≈ 1 Gyr, then its mass is Mdisc≈ 3-4 × 10−3 M⊕, several times more massive than 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