Rocky super-Earths or waterworlds: The interplay of planet migration, pebble accretion, and disc evolution
Autor(a) principal: | |
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Data de Publicação: | 2019 |
Outros Autores: | , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1051/0004-6361/201935007 http://hdl.handle.net/11449/187608 |
Resumo: | Recent observations have found a valley in the size distribution of close-in super-Earths that is interpreted as a signpost that close-in super-Earths are mostly rocky in composition. However, new models predict that planetesimals should first form at the water ice line such that close-in planets are expected to have a significant water ice component. Here we investigate the water contents of super-Earths by studying the interplay between pebble accretion, planet migration and disc evolution. Planets' compositions are determined by their position relative to different condensation fronts (ice lines) throughout their growth. Migration plays a key role. Assuming that planetesimals start at or exterior to the water ice line (r > rH2O), inward migration causes planets to leave the source region of icy pebbles and therefore to have lower final water contents than in discs with either outward migration or no migration. The water ice line itself moves inward as the disc evolves, and delivers water as it sweeps across planets that formed dry. The relative speed and direction of planet migration and inward drift of the water ice line is thus central in determining planets' water contents. If planet formation starts at the water ice line, this implies that hot close-in super-Earths (r < 0.3 AU) with water contents of a few percent are a signpost of inward planet migration during the early gas phase. Hot super-Earths with larger water ice contents on the other hand, experienced outward migration at the water ice line and only migrated inwards after their formation was complete either because they become too massive to be contained in the region of outward migration or in chains of resonant planets. Measuring the water ice content of hot super-Earths may thus constrain their migration history. |
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Rocky super-Earths or waterworlds: The interplay of planet migration, pebble accretion, and disc evolutionAccretion, accretion disksPlanet-disk interactionsPlanets and satellites: compositionPlanets and satellites: formationRecent observations have found a valley in the size distribution of close-in super-Earths that is interpreted as a signpost that close-in super-Earths are mostly rocky in composition. However, new models predict that planetesimals should first form at the water ice line such that close-in planets are expected to have a significant water ice component. Here we investigate the water contents of super-Earths by studying the interplay between pebble accretion, planet migration and disc evolution. Planets' compositions are determined by their position relative to different condensation fronts (ice lines) throughout their growth. Migration plays a key role. Assuming that planetesimals start at or exterior to the water ice line (r > rH2O), inward migration causes planets to leave the source region of icy pebbles and therefore to have lower final water contents than in discs with either outward migration or no migration. The water ice line itself moves inward as the disc evolves, and delivers water as it sweeps across planets that formed dry. The relative speed and direction of planet migration and inward drift of the water ice line is thus central in determining planets' water contents. If planet formation starts at the water ice line, this implies that hot close-in super-Earths (r < 0.3 AU) with water contents of a few percent are a signpost of inward planet migration during the early gas phase. Hot super-Earths with larger water ice contents on the other hand, experienced outward migration at the water ice line and only migrated inwards after their formation was complete either because they become too massive to be contained in the region of outward migration or in chains of resonant planets. Measuring the water ice content of hot super-Earths may thus constrain their migration history.European Research CouncilMax-Planck-Institut für Astronomie, Königstuhl 17Laboratoire d'Astrophysique de Bordeaux CNRS and Université de Bordeaux, Allée Geoffroy St. HilaireUNESP Universidade Estadual Paulista - Grupo de Dinàmica Orbital Planetologia, Guaratinguetà, CEP 12.516-410UNESP Universidade Estadual Paulista - Grupo de Dinàmica Orbital Planetologia, Guaratinguetà, CEP 12.516-410European Research Council: 757448-PAMDORAMax-Planck-Institut für AstronomieCNRS and Université de BordeauxUniversidade Estadual Paulista (Unesp)Bitsch, BertramRaymond, Sean N.Izidoro, Andre [UNESP]2019-10-06T15:41:41Z2019-10-06T15:41:41Z2019-04-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttp://dx.doi.org/10.1051/0004-6361/201935007Astronomy and Astrophysics, v. 624.1432-07460004-6361http://hdl.handle.net/11449/18760810.1051/0004-6361/2019350072-s2.0-85065019033Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengAstronomy and Astrophysicsinfo:eu-repo/semantics/openAccess2021-10-23T12:39:42Zoai:repositorio.unesp.br:11449/187608Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462021-10-23T12:39:42Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
Rocky super-Earths or waterworlds: The interplay of planet migration, pebble accretion, and disc evolution |
title |
Rocky super-Earths or waterworlds: The interplay of planet migration, pebble accretion, and disc evolution |
spellingShingle |
Rocky super-Earths or waterworlds: The interplay of planet migration, pebble accretion, and disc evolution Bitsch, Bertram Accretion, accretion disks Planet-disk interactions Planets and satellites: composition Planets and satellites: formation |
title_short |
Rocky super-Earths or waterworlds: The interplay of planet migration, pebble accretion, and disc evolution |
title_full |
Rocky super-Earths or waterworlds: The interplay of planet migration, pebble accretion, and disc evolution |
title_fullStr |
Rocky super-Earths or waterworlds: The interplay of planet migration, pebble accretion, and disc evolution |
title_full_unstemmed |
Rocky super-Earths or waterworlds: The interplay of planet migration, pebble accretion, and disc evolution |
title_sort |
Rocky super-Earths or waterworlds: The interplay of planet migration, pebble accretion, and disc evolution |
author |
Bitsch, Bertram |
author_facet |
Bitsch, Bertram Raymond, Sean N. Izidoro, Andre [UNESP] |
author_role |
author |
author2 |
Raymond, Sean N. Izidoro, Andre [UNESP] |
author2_role |
author author |
dc.contributor.none.fl_str_mv |
Max-Planck-Institut für Astronomie CNRS and Université de Bordeaux Universidade Estadual Paulista (Unesp) |
dc.contributor.author.fl_str_mv |
Bitsch, Bertram Raymond, Sean N. Izidoro, Andre [UNESP] |
dc.subject.por.fl_str_mv |
Accretion, accretion disks Planet-disk interactions Planets and satellites: composition Planets and satellites: formation |
topic |
Accretion, accretion disks Planet-disk interactions Planets and satellites: composition Planets and satellites: formation |
description |
Recent observations have found a valley in the size distribution of close-in super-Earths that is interpreted as a signpost that close-in super-Earths are mostly rocky in composition. However, new models predict that planetesimals should first form at the water ice line such that close-in planets are expected to have a significant water ice component. Here we investigate the water contents of super-Earths by studying the interplay between pebble accretion, planet migration and disc evolution. Planets' compositions are determined by their position relative to different condensation fronts (ice lines) throughout their growth. Migration plays a key role. Assuming that planetesimals start at or exterior to the water ice line (r > rH2O), inward migration causes planets to leave the source region of icy pebbles and therefore to have lower final water contents than in discs with either outward migration or no migration. The water ice line itself moves inward as the disc evolves, and delivers water as it sweeps across planets that formed dry. The relative speed and direction of planet migration and inward drift of the water ice line is thus central in determining planets' water contents. If planet formation starts at the water ice line, this implies that hot close-in super-Earths (r < 0.3 AU) with water contents of a few percent are a signpost of inward planet migration during the early gas phase. Hot super-Earths with larger water ice contents on the other hand, experienced outward migration at the water ice line and only migrated inwards after their formation was complete either because they become too massive to be contained in the region of outward migration or in chains of resonant planets. Measuring the water ice content of hot super-Earths may thus constrain their migration history. |
publishDate |
2019 |
dc.date.none.fl_str_mv |
2019-10-06T15:41:41Z 2019-10-06T15:41:41Z 2019-04-01 |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/article |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://dx.doi.org/10.1051/0004-6361/201935007 Astronomy and Astrophysics, v. 624. 1432-0746 0004-6361 http://hdl.handle.net/11449/187608 10.1051/0004-6361/201935007 2-s2.0-85065019033 |
url |
http://dx.doi.org/10.1051/0004-6361/201935007 http://hdl.handle.net/11449/187608 |
identifier_str_mv |
Astronomy and Astrophysics, v. 624. 1432-0746 0004-6361 10.1051/0004-6361/201935007 2-s2.0-85065019033 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
Astronomy and Astrophysics |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.source.none.fl_str_mv |
Scopus reponame:Repositório Institucional da UNESP instname:Universidade Estadual Paulista (UNESP) instacron:UNESP |
instname_str |
Universidade Estadual Paulista (UNESP) |
instacron_str |
UNESP |
institution |
UNESP |
reponame_str |
Repositório Institucional da UNESP |
collection |
Repositório Institucional da UNESP |
repository.name.fl_str_mv |
Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP) |
repository.mail.fl_str_mv |
|
_version_ |
1803047140526653440 |