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dc.contributor.authorNayakshin, Sergei-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society , 2011, 413 (2), pp. 1462-1478-
dc.description.abstractGiant planet embryos are believed to be spawned by gravitational instability in massive extended (R∼ 100 au) protostellar discs. In a recent paper, we have shown that dust can sediment inside the embryos, as argued earlier by Boss in a slightly different model. Here we study numerically the next stage of this process – the formation of a solid core. If conditions are conducive to solid core formation, the centre of the gas cloud goes through the following sequence of phases: (i) becomes grain (and metal) rich; (ii) forms a terrestrial mass solid core via a rapid collapse driven by self-gravity of the grains; (iii) starts to accrete a gaseous atmosphere when the solid core reaches mass of a few to 10 M⊕. This sequence of events may build either terrestrial planet cores or metal-rich giant planets inside the larger gas reservoir of the giant planet embryo. In a companion letter we argue that tidal and irradiation effects from the parent star should disrupt the outer metal-poor layers of the embryo, releasing nearly ‘ready to use’ planets. We propose this as an alternative way to build planets.-
dc.publisherOxford University Press (OUP)-
dc.rightsThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2011 the 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.-
dc.titleFormation of terrestrial planet cores inside giant planet embryos-
dc.typeJournal Article-
dc.description.versionPublisher Version-
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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