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  • stu1641

    Final published version, 2.7 MB, PDF document

  • S. M. Lawler
  • J. Di Francesco
  • G. M. Kennedy
  • B. Sibthorpe
  • M. Booth
  • B. Vandenbussche
  • B. C. Matthews
  • W. S. Holland
  • J. Greaves
  • D. J. Wilner
  • Mikko Tuomi
  • J. A D L Blommaert
  • B. L. De Vries
  • C. Dominik
  • M. Fridlund
  • W. Gear
  • A. M. Heras
  • R. Ivison
  • G. Olofsson
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Original languageEnglish
Pages (from-to)2665-2675
Number of pages11
JournalMonthly Notices of the Royal Astronomical Society
Volume444
Issue3
Early online date11 Sep 2014
DOIs
Publication statusPublished - 1 Nov 2014

Abstract

Τ Ceti is a nearby, mature G-type star very similar to our Sun, with a massive Kuiper Belt analogue and possible multiplanet system that has been compared to our Solar system. We present Herschel Space Observatory images of the debris disc, finding the disc is resolved at 70 μm and 160 μm, and marginally resolved at 250 μm. The Herschel images and infrared photometry from the literature are best modelled using a wide dust annulus with an inner edge between 1 and 10 au and an outer edge at~55 au, inclined from face-on by 35° ±10°, and with no significant azimuthal structure. We model the proposed tightly packed planetary system of five super-Earths and find that the innermost dynamically stable disc orbits are consistent with the inner edge found by the observations. The photometric modelling, however, cannot rule out a disc inner edge as close to the star as 1 au, though larger distances produce a better fit to the data. Dynamical modelling shows that the five-planet system is stable with the addition of a Neptune or smaller mass planet on an orbit outside 5 au, where the radial velocity data analysis would not have detected a planet of this mass.

Notes

S. M. Lawler, et al, 'The debris disk of solar analogue τ Ceti: Herschel observations and dynamical simulations of the proposed multiplanet system', Monthly Notices of the Royal Astronomical Society, Vol. 444 (3): 2665-2675, first published online 11 September 2014. The version of record is available online at doi: 10.1093/mnras/stu1641 © 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.

ID: 11128947