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hal.structure.identifierLund Observatory
dc.contributor.authorBITSCH, Bertram
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorRAYMOND, Sean N.
hal.structure.identifierNational Space Institute [Lyngby] [DTU Space]
dc.contributor.authorBUCHHAVE, Lars
hal.structure.identifierNational Space Institute [Lyngby] [DTU Space]
dc.contributor.authorBELLO-ARUFE, Aaron
hal.structure.identifierNational Space Institute [Lyngby] [DTU Space]
dc.contributor.authorRATHCKE, Alexander
dc.contributor.authorDAVID SCHNEIDER, Aaron
dc.date.issued2021-05
dc.identifier.issn0004-6361
dc.description.abstractEnIn the pebble accretion scenario, the pebbles that form planets drift inward from the outer disk regions, carrying water ice with them. At the water ice line, the water ice on the inward drifting pebbles evaporates and is released into the gas phase, resulting in water-rich gas and dry pebbles that move into the inner disk regions. Large planetary cores can block the inward drifting pebbles by forming a pressure bump outside their orbit in the protoplanetary disk. Depending on the relative position of a growing planetary core relative to the water ice line, water-rich pebbles might be blocked outside or inside the water ice line. Pebbles blocked outside the water ice line do not evaporate and thus do not release their water vapor into the gas phase, resulting in a dry inner disk, while pebbles blocked inside the water ice line release their water vapor into the gas phase, resulting in water vapor diffusing into the inner disk. As a consequence, close-in sub-Neptunes that accrete some gas from the disk should be dry or wet, respectively, if outer gas giants are outside or inside the water ice line, assuming that giant planets form fast, as has been suggested for Jupiter in our Solar System. Alternatively, a sub-Neptune could form outside the water ice line, accreting a large amount of icy pebbles and then migrating inward as a very wet sub-Neptune. We suggest that the water content of inner sub-Neptunes in systems with giant planets that can efficiently block the inward drifting pebbles could constrain the formation conditions of these systems, thus making these sub-Neptunes exciting targets for detailed characterization (e.g., with JWST, ELT, or ARIEL). In addition, the search for giant planets in systems with already characterized sub-Neptunes can be used to constrain the formation conditions of giant planets as well.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enaccretion discs -planets and satellites
dc.subject.enformation -protoplanetary discs -planets and satellites
dc.subject.encomposition
dc.title.enDry or water world? How the water contents of inner sub-Neptunes constrain giant planet formation and the location of the water ice line
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/202140793
dc.subject.halPlanète et Univers [physics]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageL5
bordeaux.volume649
bordeaux.peerReviewedoui
hal.identifierhal-03378833
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-03378833v1
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