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dc.contributor.authorBooth, Richarden
dc.contributor.authorClarke, Catherineen
dc.contributor.authorNikku, Madhusudhanen
dc.contributor.authorIlee, Johnen
dc.date.accessioned2017-08-02T07:26:59Z
dc.date.available2017-08-02T07:26:59Z
dc.date.issued2017-05-06en
dc.identifier.issn0035-8711
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/265837
dc.description.abstractChemical compositions of giant planets provide a means to constrain how and where they form. Traditionally, super-stellar elemental abundances in giant planets were thought to be possible due to accretion of metal-rich solids. Such enrichments are accompanied by oxygen-rich compositions (i.e. C/O below the disc’s value, assumed to be solar, C/O = 0.54). Without solid accretion, the planets are expected to have sub-solar metallicity, but high C/O ratios. This arises because the solids are dominated by oxygen-rich species, e.g. H$_2$O and CO$_2$, which freeze out in the disc earlier than CO, leaving the gas metal poor but carbon rich. Here we demonstrate that super-solar metallicities can be achieved by gas accretion alone when growth and radial drift of pebbles are considered in protoplanetary discs. Through this mechanism, planets may simultaneously acquire super-solar metallicities and super-solar C/O ratios. This happens because the pebbles transport volatile species inwards as they migrate through the disc, enriching the gas at snow lines where the volatiles sublimate. Furthermore, the planet’s composition can be used to constrain where it formed. Since high C/H and C/O ratios cannot be created by accreting solids, it may be possible to distinguish between formation via pebble accretion and planetesimal accretion by the level of solid enrichment. Finally, we expect that Jupiter’s C/O ratio should be near or above solar if its enhanced carbon abundance came through accreting metal-rich gas. Thus, $\textit{Juno}$’s measurement of Jupiter’s C/O ratio should determine whether Jupiter accreted its metals from carbon-rich gas or oxygen-rich solids.
dc.description.sponsorshipThis work has been supported by the DISCSIM project, grant agreement 341137 funded by the European Research Council under ERC-2013-ADG.
dc.language.isoenen
dc.publisherOxford University Press
dc.subjectplanets and satellites: atmospheresen
dc.subjectplanets and satellites: compositionen
dc.subjectplanets and satellites: formationen
dc.subjectplanets and satellites: individual: Jupiteren
dc.subjectprotoplanetary discsen
dc.titleChemical enrichment of giant planets and discs due to pebble driften
dc.typeArticle
prism.endingPage4011
prism.issueIdentifier4en
prism.publicationDate2017en
prism.publicationNameMonthly Notices of the Royal Astronomical Societyen
prism.startingPage3994
prism.volume469en
dc.identifier.doi10.17863/CAM.9962
dcterms.dateAccepted2017-05-04en
rioxxterms.versionofrecord10.1093/mnras/stx1103en
rioxxterms.versionVoRen
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserveden
rioxxterms.licenseref.startdate2017-05-06en
dc.contributor.orcidBooth, Richard [0000-0002-0364-937X]
dc.contributor.orcidClarke, Catherine [0000-0003-4288-0248]
dc.contributor.orcidNikku, Madhusudhan [0000-0002-4869-000X]
dc.identifier.eissn1365-2966
dc.publisher.urlhttp://dx.doi.org/10.1093/mnras/stx1103en
rioxxterms.typeJournal Article/Reviewen
pubs.funder-project-idEuropean Research Council (341137)
pubs.funder-project-idSCIENCE & TECHNOLOGY FACILITIES COUNCIL (ST/N000927/1)
cam.orpheus.successThu Jan 30 13:04:53 GMT 2020 - The item has an open VoR version.*
rioxxterms.freetoread.startdate2100-01-01


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