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dc.contributor.authorMoriarty, John C
dc.contributor.authorBallard, Sarah A
dc.date.accessioned2017-05-02T16:06:40Z
dc.date.available2017-05-02T16:06:40Z
dc.date.issued2016-11
dc.date.submitted2016-08
dc.identifier.issn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/1721.1/108584
dc.description.abstractNASA's Kepler Mission uncovered a wealth of planetary systems, many with planets on short-period orbits. These short-period systems reside around 50% of Sun-like stars and are similarly prevalent around M dwarfs. Their formation and subsequent evolution is the subject of active debate. In this paper, we simulate late-stage, in situ planet formation across a grid of planetesimal disks with varying surface density profiles and total mass. We compare simulation results with observable characteristics of the Kepler sample. We identify mixture models with different primordial planetesimal disk properties that self-consistently recover the multiplicity, radius, period and period ratio, and duration ratio distributions of the Kepler planets. We draw three main conclusions. (1) We favor a "frozen-in" narrative for systems of short-period planets, in which they are stable over long timescales, as opposed to metastable. (2) The "Kepler dichotomy," an observed phenomenon of the Kepler sample wherein the architectures of planetary systems appear to either vary significantly or have multiple modes, can naturally be explained by formation within planetesimal disks with varying surface density profiles. Finally, (3) we quantify the nature of the "Kepler dichotomy" for both GK stars and M dwarfs, and find that it varies with stellar type. While the mode of planet formation that accounts for high multiplicity systems occurs in 24% ± 7% of planetary systems orbiting GK stars, it occurs in 63% ± 16% of planetary systems orbiting M dwarfs.en_US
dc.description.sponsorshipUnited States. National Aeronautics and Space Administration (NASA grant NNX12AC01G)en_US
dc.description.sponsorshipMassachusetts Institute of Technology (Torres Fellowship for Exoplanet Research))en_US
dc.language.isoen_US
dc.publisherInstitute of Physics Publishing (IOP)en_US
dc.relation.isversionofhttp://dx.doi.org/10.3847/0004-637x/832/1/34en_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.sourceAmerican Astronomical Societyen_US
dc.titleTHE KEPLER DICHOTOMY IN PLANETARY DISKS: LINKING KEPLER OBSERVABLES TO SIMULATIONS OF LATE-STAGE PLANET FORMATIONen_US
dc.typeArticleen_US
dc.identifier.citationMoriarty, John, and Sarah Ballard. “THE KEPLER DICHOTOMY IN PLANETARY DISKS: LINKING KEPLER OBSERVABLES TO SIMULATIONS OF LATE-STAGE PLANET FORMATION.” The Astrophysical Journal 832, no. 1 (November 14, 2016): 34. © Copyright 2016 IOP Publishing.en_US
dc.contributor.departmentKavli Institute for Astrophysics and Space Researchen_US
dc.contributor.mitauthorMoriarty, John C
dc.contributor.mitauthorBallard, Sarah A
dc.relation.journalAstrophysical Journalen_US
dc.eprint.versionFinal published versionen_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dspace.orderedauthorsMoriarty, John; Ballard, Sarahen_US
dspace.embargo.termsNen_US
mit.licensePUBLISHER_POLICYen_US


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