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      ALMA observations of the \(\eta\) Corvi debris disc: inward scattering of CO-rich exocomets by a chain of 3-30 M\(_\oplus\) planets?

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          Abstract

          While most of the known debris discs present cold dust at tens of AU, a few young systems exhibit hot dust analogous to the Zodiacal dust. \(\eta\) 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 \(\eta\) Corvi with a resolution of 1."2 (~22au) to study its outer belt. The continuum emission is consistent with an axisymmetric belt, with a mean radius of 152au and radial FWHM of 46au, 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 4sigma detection of CO at ~ 20au. CO could be released in situ from icy planetesimals being passed in when crossing the H\(_2\)O or CO\(_2\) 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 75-100au, with a mass of 3-30 M\(_\oplus\) and an eccentricity < 0.08. Such a planet would be able to clear its chaotic zone on a timescale shorter than the age of the system and scatter material inwards from the outer belt to the inner regions, thus feeding the hot dust.

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          The Joker A Custom Monte Carlo Sampler for Binary-star and Exoplanet Radial Velocity Data

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            Pluto and Charon: Formation, Seasons, Composition

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              Author and article information

              Journal
              2016-11-03
              Article
              1611.01168

              http://arxiv.org/licenses/nonexclusive-distrib/1.0/

              Custom metadata
              22 pages, 16 figures. Accepted for publication in MNRAS
              astro-ph.EP

              Planetary astrophysics

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