A remnant planetary core in the hot-Neptune desert
- Autores
- Armstrong, David J.; Lopez, Théo A.; Adibekyan, Vardan; Booth, Richard A.; Bryant, Edward M.; Collins, Karen A.; Emsenhuber, Alexandre; Huang, Chelsea X.; King, George W.; Lillo Box, Jorge; Lissauer, Jack J.; Matthews, Elisabeth; Mousis, Olivier; Nielsen, Louise D.; Osborn, Hugh; Otegi, Jon; Santos, Nuno C.; Sousa, Sérgio G.; Stassun, Keivan G.; Veras, Dimitri; Ziegler, Carl; Acton, Jack S.; Almenara, Jose M.; Anderson, David R.; Barrado, David; Barros, Susana C. C.; Bayliss, Daniel; Belardi, Claudia; Diaz, Rodrigo Fernando
- Año de publicación
- 2020
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- The interiors of giant planets remain poorly understood. Even for the planets in the Solar System, difficulties in observation lead to major uncertainties in the properties of planetary cores. Exoplanets that have undergone rare evolutionary pathways provide a new route to understanding planetary interiors. We present the discovery of TOI-849b, the remnant core of a giant planet, with a radius smaller than Neptune but an anomalously high mass Mp =40.8+2.4 −2.5 M⊕ and density of 5.5±0.8 gcm−3 , similar to the Earth. Interior structure models suggest that any gaseous envelope of pure hydrogen and helium consists of no more than 3.9 +0.8 −0.9% of the total mass of the planet. TOI-849b transits a late G type star (Tmag = 11.5) with an orbital period of 18.4 hours, leading to an equilibrium temperature of 1800K. The planet’s mass is larger than the theoretical threshold mass for runaway gas accretion. As such, the planet could have been a gas giant before undergoing extreme mass loss via thermal self-disruption or giant planet collisions, or it avoided substantial gas accretion, perhaps through gap opening or late formation. Photoevaporation rates cannot provide the mass loss required to reduce a Jupiter-like gas giant, but can remove a few M⊕ hydrogen and helium envelope on timescales of several Gyr, implying that any remaining atmosphere is likely to be enriched by water or other volatiles from the planetary interior. TOI-849b represents a unique case where material from the primordial core is left over from formation and available to study.
Fil: Armstrong, David J.. University of Warwick; Reino Unido
Fil: Lopez, Théo A.. Centre National D Etudes Spatiales.; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Adibekyan, Vardan. Universidad de Porto; Portugal
Fil: Booth, Richard A.. Institute of Astronomy; Reino Unido
Fil: Bryant, Edward M.. University of Warwick; Reino Unido
Fil: Collins, Karen A.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Emsenhuber, Alexandre. University of Arizona; Estados Unidos. University of Bern; Suiza
Fil: Huang, Chelsea X.. Massachusetts Institute of Technology; Estados Unidos
Fil: King, George W.. University of Warwick; Reino Unido
Fil: Lillo Box, Jorge. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; España
Fil: Lissauer, Jack J.. National Aeronautics and Space Administration; Estados Unidos
Fil: Matthews, Elisabeth. Massachusetts Institute of Technology; Estados Unidos
Fil: Mousis, Olivier. Centre National de la Recherche Scientifique; Francia. Centre National D Etudes Spatiales.; Francia
Fil: Nielsen, Louise D.. Universidad de Ginebra; Suiza
Fil: Osborn, Hugh. Centre National de la Recherche Scientifique; Francia. Centre National D Etudes Spatiales.; Francia
Fil: Otegi, Jon. Universitat Zurich; Suiza. Universidad de Ginebra; Suiza
Fil: Santos, Nuno C.. Universidad de Porto; Portugal
Fil: Sousa, Sérgio G.. Universidad de Porto; Portugal
Fil: Stassun, Keivan G.. Vanderbilt University; Estados Unidos. Fisk University; Estados Unidos
Fil: Veras, Dimitri. University of Warwick; Reino Unido
Fil: Ziegler, Carl. University of Toronto; Canadá
Fil: Acton, Jack S.. University of Leicester; Reino Unido
Fil: Almenara, Jose M.. Universite Grenoble Alpes; Francia
Fil: Anderson, David R.. University of Warwick; Reino Unido
Fil: Barrado, David. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; España
Fil: Barros, Susana C. C.. Universidad de Porto; Portugal
Fil: Bayliss, Daniel. University of Warwick; Reino Unido
Fil: Belardi, Claudia. University of Leicester; Reino Unido
Fil: Diaz, Rodrigo Fernando. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina - Materia
-
Astrophysics - Earth and Planetary Astrophysics
Astrophysics - Solar and Stellar Astrophysics - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/161440
Ver los metadatos del registro completo
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A remnant planetary core in the hot-Neptune desertArmstrong, David J.Lopez, Théo A.Adibekyan, VardanBooth, Richard A.Bryant, Edward M.Collins, Karen A.Emsenhuber, AlexandreHuang, Chelsea X.King, George W.Lillo Box, JorgeLissauer, Jack J.Matthews, ElisabethMousis, OlivierNielsen, Louise D.Osborn, HughOtegi, JonSantos, Nuno C.Sousa, Sérgio G.Stassun, Keivan G.Veras, DimitriZiegler, CarlActon, Jack S.Almenara, Jose M.Anderson, David R.Barrado, DavidBarros, Susana C. C.Bayliss, DanielBelardi, ClaudiaDiaz, Rodrigo FernandoAstrophysics - Earth and Planetary AstrophysicsAstrophysics - Solar and Stellar Astrophysicshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The interiors of giant planets remain poorly understood. Even for the planets in the Solar System, difficulties in observation lead to major uncertainties in the properties of planetary cores. Exoplanets that have undergone rare evolutionary pathways provide a new route to understanding planetary interiors. We present the discovery of TOI-849b, the remnant core of a giant planet, with a radius smaller than Neptune but an anomalously high mass Mp =40.8+2.4 −2.5 M⊕ and density of 5.5±0.8 gcm−3 , similar to the Earth. Interior structure models suggest that any gaseous envelope of pure hydrogen and helium consists of no more than 3.9 +0.8 −0.9% of the total mass of the planet. TOI-849b transits a late G type star (Tmag = 11.5) with an orbital period of 18.4 hours, leading to an equilibrium temperature of 1800K. The planet’s mass is larger than the theoretical threshold mass for runaway gas accretion. As such, the planet could have been a gas giant before undergoing extreme mass loss via thermal self-disruption or giant planet collisions, or it avoided substantial gas accretion, perhaps through gap opening or late formation. Photoevaporation rates cannot provide the mass loss required to reduce a Jupiter-like gas giant, but can remove a few M⊕ hydrogen and helium envelope on timescales of several Gyr, implying that any remaining atmosphere is likely to be enriched by water or other volatiles from the planetary interior. TOI-849b represents a unique case where material from the primordial core is left over from formation and available to study.Fil: Armstrong, David J.. University of Warwick; Reino UnidoFil: Lopez, Théo A.. Centre National D Etudes Spatiales.; Francia. Centre National de la Recherche Scientifique; FranciaFil: Adibekyan, Vardan. Universidad de Porto; PortugalFil: Booth, Richard A.. Institute of Astronomy; Reino UnidoFil: Bryant, Edward M.. University of Warwick; Reino UnidoFil: Collins, Karen A.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Emsenhuber, Alexandre. University of Arizona; Estados Unidos. University of Bern; SuizaFil: Huang, Chelsea X.. Massachusetts Institute of Technology; Estados UnidosFil: King, George W.. University of Warwick; Reino UnidoFil: Lillo Box, Jorge. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; EspañaFil: Lissauer, Jack J.. National Aeronautics and Space Administration; Estados UnidosFil: Matthews, Elisabeth. Massachusetts Institute of Technology; Estados UnidosFil: Mousis, Olivier. Centre National de la Recherche Scientifique; Francia. Centre National D Etudes Spatiales.; FranciaFil: Nielsen, Louise D.. Universidad de Ginebra; SuizaFil: Osborn, Hugh. Centre National de la Recherche Scientifique; Francia. Centre National D Etudes Spatiales.; FranciaFil: Otegi, Jon. Universitat Zurich; Suiza. Universidad de Ginebra; SuizaFil: Santos, Nuno C.. Universidad de Porto; PortugalFil: Sousa, Sérgio G.. Universidad de Porto; PortugalFil: Stassun, Keivan G.. Vanderbilt University; Estados Unidos. Fisk University; Estados UnidosFil: Veras, Dimitri. University of Warwick; Reino UnidoFil: Ziegler, Carl. University of Toronto; CanadáFil: Acton, Jack S.. University of Leicester; Reino UnidoFil: Almenara, Jose M.. Universite Grenoble Alpes; FranciaFil: Anderson, David R.. University of Warwick; Reino UnidoFil: Barrado, David. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; EspañaFil: Barros, Susana C. C.. Universidad de Porto; PortugalFil: Bayliss, Daniel. University of Warwick; Reino UnidoFil: Belardi, Claudia. University of Leicester; Reino UnidoFil: Diaz, Rodrigo Fernando. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaNature Publishing Group2020-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/161440Armstrong, David J.; Lopez, Théo A.; Adibekyan, Vardan; Booth, Richard A.; Bryant, Edward M.; et al.; A remnant planetary core in the hot-Neptune desert; Nature Publishing Group; Nature; 583; 7814; 7-2020; 39-420028-08361476-4687CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.nature.com/articles/s41586-020-2421-7info:eu-repo/semantics/altIdentifier/doi/10.1038/s41586-020-2421-7info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2003.10314#:~:text=The%20interiors%20of%20giant%20planets,the%20properties%20of%20planetary%20cores.info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-10T13:11:46Zoai:ri.conicet.gov.ar:11336/161440instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-10 13:11:46.495CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
A remnant planetary core in the hot-Neptune desert |
| title |
A remnant planetary core in the hot-Neptune desert |
| spellingShingle |
A remnant planetary core in the hot-Neptune desert Armstrong, David J. Astrophysics - Earth and Planetary Astrophysics Astrophysics - Solar and Stellar Astrophysics |
| title_short |
A remnant planetary core in the hot-Neptune desert |
| title_full |
A remnant planetary core in the hot-Neptune desert |
| title_fullStr |
A remnant planetary core in the hot-Neptune desert |
| title_full_unstemmed |
A remnant planetary core in the hot-Neptune desert |
| title_sort |
A remnant planetary core in the hot-Neptune desert |
| dc.creator.none.fl_str_mv |
Armstrong, David J. Lopez, Théo A. Adibekyan, Vardan Booth, Richard A. Bryant, Edward M. Collins, Karen A. Emsenhuber, Alexandre Huang, Chelsea X. King, George W. Lillo Box, Jorge Lissauer, Jack J. Matthews, Elisabeth Mousis, Olivier Nielsen, Louise D. Osborn, Hugh Otegi, Jon Santos, Nuno C. Sousa, Sérgio G. Stassun, Keivan G. Veras, Dimitri Ziegler, Carl Acton, Jack S. Almenara, Jose M. Anderson, David R. Barrado, David Barros, Susana C. C. Bayliss, Daniel Belardi, Claudia Diaz, Rodrigo Fernando |
| author |
Armstrong, David J. |
| author_facet |
Armstrong, David J. Lopez, Théo A. Adibekyan, Vardan Booth, Richard A. Bryant, Edward M. Collins, Karen A. Emsenhuber, Alexandre Huang, Chelsea X. King, George W. Lillo Box, Jorge Lissauer, Jack J. Matthews, Elisabeth Mousis, Olivier Nielsen, Louise D. Osborn, Hugh Otegi, Jon Santos, Nuno C. Sousa, Sérgio G. Stassun, Keivan G. Veras, Dimitri Ziegler, Carl Acton, Jack S. Almenara, Jose M. Anderson, David R. Barrado, David Barros, Susana C. C. Bayliss, Daniel Belardi, Claudia Diaz, Rodrigo Fernando |
| author_role |
author |
| author2 |
Lopez, Théo A. Adibekyan, Vardan Booth, Richard A. Bryant, Edward M. Collins, Karen A. Emsenhuber, Alexandre Huang, Chelsea X. King, George W. Lillo Box, Jorge Lissauer, Jack J. Matthews, Elisabeth Mousis, Olivier Nielsen, Louise D. Osborn, Hugh Otegi, Jon Santos, Nuno C. Sousa, Sérgio G. Stassun, Keivan G. Veras, Dimitri Ziegler, Carl Acton, Jack S. Almenara, Jose M. Anderson, David R. Barrado, David Barros, Susana C. C. Bayliss, Daniel Belardi, Claudia Diaz, Rodrigo Fernando |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
Astrophysics - Earth and Planetary Astrophysics Astrophysics - Solar and Stellar Astrophysics |
| topic |
Astrophysics - Earth and Planetary Astrophysics Astrophysics - Solar and Stellar Astrophysics |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
The interiors of giant planets remain poorly understood. Even for the planets in the Solar System, difficulties in observation lead to major uncertainties in the properties of planetary cores. Exoplanets that have undergone rare evolutionary pathways provide a new route to understanding planetary interiors. We present the discovery of TOI-849b, the remnant core of a giant planet, with a radius smaller than Neptune but an anomalously high mass Mp =40.8+2.4 −2.5 M⊕ and density of 5.5±0.8 gcm−3 , similar to the Earth. Interior structure models suggest that any gaseous envelope of pure hydrogen and helium consists of no more than 3.9 +0.8 −0.9% of the total mass of the planet. TOI-849b transits a late G type star (Tmag = 11.5) with an orbital period of 18.4 hours, leading to an equilibrium temperature of 1800K. The planet’s mass is larger than the theoretical threshold mass for runaway gas accretion. As such, the planet could have been a gas giant before undergoing extreme mass loss via thermal self-disruption or giant planet collisions, or it avoided substantial gas accretion, perhaps through gap opening or late formation. Photoevaporation rates cannot provide the mass loss required to reduce a Jupiter-like gas giant, but can remove a few M⊕ hydrogen and helium envelope on timescales of several Gyr, implying that any remaining atmosphere is likely to be enriched by water or other volatiles from the planetary interior. TOI-849b represents a unique case where material from the primordial core is left over from formation and available to study. Fil: Armstrong, David J.. University of Warwick; Reino Unido Fil: Lopez, Théo A.. Centre National D Etudes Spatiales.; Francia. Centre National de la Recherche Scientifique; Francia Fil: Adibekyan, Vardan. Universidad de Porto; Portugal Fil: Booth, Richard A.. Institute of Astronomy; Reino Unido Fil: Bryant, Edward M.. University of Warwick; Reino Unido Fil: Collins, Karen A.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Emsenhuber, Alexandre. University of Arizona; Estados Unidos. University of Bern; Suiza Fil: Huang, Chelsea X.. Massachusetts Institute of Technology; Estados Unidos Fil: King, George W.. University of Warwick; Reino Unido Fil: Lillo Box, Jorge. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; España Fil: Lissauer, Jack J.. National Aeronautics and Space Administration; Estados Unidos Fil: Matthews, Elisabeth. Massachusetts Institute of Technology; Estados Unidos Fil: Mousis, Olivier. Centre National de la Recherche Scientifique; Francia. Centre National D Etudes Spatiales.; Francia Fil: Nielsen, Louise D.. Universidad de Ginebra; Suiza Fil: Osborn, Hugh. Centre National de la Recherche Scientifique; Francia. Centre National D Etudes Spatiales.; Francia Fil: Otegi, Jon. Universitat Zurich; Suiza. Universidad de Ginebra; Suiza Fil: Santos, Nuno C.. Universidad de Porto; Portugal Fil: Sousa, Sérgio G.. Universidad de Porto; Portugal Fil: Stassun, Keivan G.. Vanderbilt University; Estados Unidos. Fisk University; Estados Unidos Fil: Veras, Dimitri. University of Warwick; Reino Unido Fil: Ziegler, Carl. University of Toronto; Canadá Fil: Acton, Jack S.. University of Leicester; Reino Unido Fil: Almenara, Jose M.. Universite Grenoble Alpes; Francia Fil: Anderson, David R.. University of Warwick; Reino Unido Fil: Barrado, David. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; España Fil: Barros, Susana C. C.. Universidad de Porto; Portugal Fil: Bayliss, Daniel. University of Warwick; Reino Unido Fil: Belardi, Claudia. University of Leicester; Reino Unido Fil: Diaz, Rodrigo Fernando. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina |
| description |
The interiors of giant planets remain poorly understood. Even for the planets in the Solar System, difficulties in observation lead to major uncertainties in the properties of planetary cores. Exoplanets that have undergone rare evolutionary pathways provide a new route to understanding planetary interiors. We present the discovery of TOI-849b, the remnant core of a giant planet, with a radius smaller than Neptune but an anomalously high mass Mp =40.8+2.4 −2.5 M⊕ and density of 5.5±0.8 gcm−3 , similar to the Earth. Interior structure models suggest that any gaseous envelope of pure hydrogen and helium consists of no more than 3.9 +0.8 −0.9% of the total mass of the planet. TOI-849b transits a late G type star (Tmag = 11.5) with an orbital period of 18.4 hours, leading to an equilibrium temperature of 1800K. The planet’s mass is larger than the theoretical threshold mass for runaway gas accretion. As such, the planet could have been a gas giant before undergoing extreme mass loss via thermal self-disruption or giant planet collisions, or it avoided substantial gas accretion, perhaps through gap opening or late formation. Photoevaporation rates cannot provide the mass loss required to reduce a Jupiter-like gas giant, but can remove a few M⊕ hydrogen and helium envelope on timescales of several Gyr, implying that any remaining atmosphere is likely to be enriched by water or other volatiles from the planetary interior. TOI-849b represents a unique case where material from the primordial core is left over from formation and available to study. |
| publishDate |
2020 |
| dc.date.none.fl_str_mv |
2020-07 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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article |
| status_str |
publishedVersion |
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http://hdl.handle.net/11336/161440 Armstrong, David J.; Lopez, Théo A.; Adibekyan, Vardan; Booth, Richard A.; Bryant, Edward M.; et al.; A remnant planetary core in the hot-Neptune desert; Nature Publishing Group; Nature; 583; 7814; 7-2020; 39-42 0028-0836 1476-4687 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/161440 |
| identifier_str_mv |
Armstrong, David J.; Lopez, Théo A.; Adibekyan, Vardan; Booth, Richard A.; Bryant, Edward M.; et al.; A remnant planetary core in the hot-Neptune desert; Nature Publishing Group; Nature; 583; 7814; 7-2020; 39-42 0028-0836 1476-4687 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
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eng |
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info:eu-repo/semantics/altIdentifier/url/https://www.nature.com/articles/s41586-020-2421-7 info:eu-repo/semantics/altIdentifier/doi/10.1038/s41586-020-2421-7 info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2003.10314#:~:text=The%20interiors%20of%20giant%20planets,the%20properties%20of%20planetary%20cores. |
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info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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openAccess |
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Nature Publishing Group |
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Nature Publishing Group |
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