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Title: Tidal Downsizing model - III. Planets from sub-Earths to brown dwarfs: structure and metallicity preferences
Authors: Nayakshin, Sergei
Fletcher, Mark
First Published: 15-Jul-2015
Publisher: Oxford University Press (OUP)
Citation: Monthly Notices of the Royal Astronomical Society, 2015, 452 (2), pp. 1654-1676 (23)
Abstract: We present population synthesis calculations of the Tidal Downsizing (TD) hypothesis for planet formation. Our models address the following observations: (i) most abundant planets being super-Earths; (ii) cores more massive than ∼5–15 M⊕ are enveloped by massive atmospheres; (iii) the frequency of occurrence of close-in gas-giant planets correlates strongly with metallicity of the host star; (iv) no such correlation is found for sub-Neptune planets; (v) presence of massive cores in giant planets; (vi) gas-giant planets are overabundant in metals compared to their host stars; (vii) this overabundance decreases with planet's mass; (viii) a deep valley in the planet mass function between masses of ∼10–20 M⊕ and ∼100 M⊕. A number of observational predictions distinguish the model from Core Accretion: (a) composition of the massive cores is always dominated by rocks not ices; (b) the core mass function is smooth with no minimum at ∼3 M⊕ and has no ice-dominated cores; (c) gas giants beyond 10 au are insensitive to the host-star metallicity; (d) objects more massive than ∼10 M[subscript: J] do not correlate or even anticorrelate with metallicity. The latter prediction is consistent with observations of low-mass stellar companions. TD can also explain formation of planets in close binary systems. TD model is a viable alternative to the Core Accretion scenario in explaining many features of the observed population of exoplanets.
DOI Link: 10.1093/mnras/stv1354
ISSN: 0035-8711
eISSN: 1365-2966
Version: Publisher Version
Status: Peer-reviewed
Type: Journal Article
Rights: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. Deposited with reference to the publisher’s archiving policy available on the SHERPA/RoMEO website.
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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