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dc.contributor.authorPaardekooper, SJen_US
dc.contributor.authorJohansen, Aen_US
dc.date.accessioned2018-02-20T11:42:43Z
dc.date.available2018-01-11en_US
dc.date.issued2018-01-24en_US
dc.date.submitted2018-02-10T20:19:21.278Z
dc.identifier.issn0038-6308en_US
dc.identifier.urihttp://qmro.qmul.ac.uk/xmlui/handle/123456789/32803
dc.description.abstract© 2018, The Author(s). Planets form in circumstellar discs around young stars. Starting with sub-micron sized dust particles, giant planet formation is all about growing 14 orders of magnitude in size. It has become increasingly clear over the past decades that during all stages of giant planet formation, the building blocks are extremely mobile and can change their semimajor axis by substantial amounts. In this chapter, we aim to give a basic overview of the physical processes thought to govern giant planet formation and migration, and to highlight possible links to water delivery.en_US
dc.description.sponsorshipS.-J. Paardekooper is supported by a Royal Society University Research Fellowship. A. Johansen is supported by the Knut and Alice Wallenberg Foundation, the Swedish Research Council (grant 2014-5775) and the European Research Council (ERC Starting Grant 278675-PEBBLE2PLANET).en_US
dc.relation.ispartofSpace Science Reviewsen_US
dc.rightsThis article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made.
dc.titleGiant Planet Formation and Migrationen_US
dc.typeArticle
dc.rights.holder© The Author(s) 2018
dc.identifier.doi10.1007/s11214-018-0472-yen_US
pubs.issue1en_US
pubs.notesNo embargoen_US
pubs.publication-statusPublisheden_US
pubs.volume214en_US
dcterms.dateAccepted2018-01-11en_US


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