ALMA observations of the η Corvi debris disc: inward scattering of CO-rich exocomets by a chain of 3–30 M⊕ planets?

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DOI	Resolve DOI: https://doi.org/10.1093/mnras/stw2867
Author	Search for: Marino, S.; Search for: Wyatt, M. C.; Search for: Panić, O.; Search for: Matrà, L.; Search for: Kennedy, G. M.; Search for: Bonsor, A.; Search for: Kral, Q.; Search for: Dent, W. R. F; Search for: Duchene, G.; Search for: Wilner, D.; Search for: Lisse, C. M.; Search for: Lestrade, J.-F.; Search for: Matthews, B.¹
Name affiliation	National Research Council of Canada. Herzberg Astronomy and Astrophysics
Format	Text, Article
Journal title	Monthly Notices of the Royal Astronomical Society
ISSN	0035-8711 1365-2966
Volume	465
Issue	3
Pages	2595–2615
Subject	circumstellar matter; stars: individual: HD 109085; planetary systems; radio continuum: planetary systems
Abstract	While most of the known debris discs present cold dust at tens of astronomical unit (au), a few young systems exhibit hot dust analogous to the Zodiacal dust. η Corvi is particularly interesting as it is old and it has both, with its hot dust significantly exceeding the maximum luminosity of an in situ collisional cascade. Previous work suggested that this system could be undergoing an event similar to the Late Heavy Bombardment (LHB) soon after or during a dynamical instability. Here, we present ALMA observations of η Corvi with a resolution of 1.2 arcsec (∼22 au) to study its outer belt. The continuum emission is consistent with an axisymmetric belt, with a mean radius of 152 au and radial full width at half-maximum of 46 au, which is too narrow compared to models of inward scattering of an LHB-like scenario. Instead, the hot dust could be explained as material passed inwards in a rather stable planetary configuration. We also report a 4σ detection of CO at ∼20 au. CO could be released in situ from icy planetesimals being passed in when crossing the H2O or CO2 ice lines. Finally, we place constraints on hidden planets in the disc. If a planet is sculpting the disc's inner edge, this should be orbiting at 75–100 au, with a mass of 3–30 M⊕ and an eccentricity <0.08. Such a planet would be able to clear its chaotic zone on a time-scale shorter than the age of the system and scatter material inwards from the outer belt to the inner regions, thus feeding the hot dust.
Publication date	2016-11-05
Publisher	Oxford University Press
Language	English
Peer reviewed	Yes
NPARC number	23002590
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Record identifier	28090fa9-706c-4933-a202-cdf99ef540ce
Record created	2017-12-04
Record modified	2020-05-30

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