Ploonets: Formation, evolution, and detectability of tidally detached exomoons

Autores
Sucerquia, Mario; Alvarado-Montes, Jaime A.; Zuluaga, Jorge I.; Cuello, Nicolas; Giuppone, Cristian Andrés
Año de publicación
2019
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Close-in giant planets represent the most significant evidence of planetary migration. If large exomoons form around migrating giant planets which are more stable (e.g. those in the Solar system), what happens to these moons after migration is still under intense research. This paper explores the scenario where large regular exomoons escape after tidal interchange of angular momentum with its parent planet, becoming small planets by themselves. We name this hypothetical type of object a ploonet. By performing semi-analytical simulations of tidal interactions between a large moon with a close-in giant, and integrating numerically their orbits for several Myr, we found that in ∼50 per cent of the cases a young ploonet may survive ejection from the planetary system, or collision with its parent planet and host star, being in principle detectable. Volatile-rich ploonets are dramatically affected by stellar radiation during both planetocentric and siderocentric orbital evolution, and their radius and mass change significantly due to the sublimation of most of their material during time-scales of hundreds of Myr. We estimate the photometric signatures that ploonets may produce if they transit the star during the phase of evaporation, and compare them with noisy light curves of known objects (Kronian stars and non-periodical dips in dusty light curves). Additionally, the typical transit timing variations (TTV) induced by the interaction of a ploonet with its planet are computed. We find that present and future photometric surveys' capabilities can detect these effects and distinguish them from those produced by other nearby planetary encounters.
Fil: Sucerquia, Mario. Universidad de Antioquia. Facultad de Física; Colombia. Pontificia Universidad Católica de Chile; Chile
Fil: Alvarado-Montes, Jaime A.. Macquarie University. Faculty Of Science And Engineering. Department Of Earth And Planetary Sciences.; Australia. Universidad de Antioquia. Facultad de Física; Colombia
Fil: Zuluaga, Jorge I.. Universidad de Antioquia; Colombia
Fil: Cuello, Nicolas. Pontificia Universidad Católica de Chile; Chile. Universidad de Buenos Aires. Facultad de Ciencias Sociales. Instituto de Investigaciones "Gino Germani"; Argentina
Fil: Giuppone, Cristian Andrés. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Materia
PLANETS AND SATELLITES: ATMOSPHERES
PLANETS AND SATELLITES: DYNAMICAL EVOLUTION AND STABILITY
TECHNIQUES: PHOTOMETRIC
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/120850
Acceder
id CONICETDig_c8bd099c55ecb243142a26f6c9c9fb31
oai_identifier_str oai:ri.conicet.gov.ar:11336/120850
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Ploonets: Formation, evolution, and detectability of tidally detached exomoonsSucerquia, MarioAlvarado-Montes, Jaime A.Zuluaga, Jorge I.Cuello, NicolasGiuppone, Cristian AndrésPLANETS AND SATELLITES: ATMOSPHERESPLANETS AND SATELLITES: DYNAMICAL EVOLUTION AND STABILITYTECHNIQUES: PHOTOMETRIChttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Close-in giant planets represent the most significant evidence of planetary migration. If large exomoons form around migrating giant planets which are more stable (e.g. those in the Solar system), what happens to these moons after migration is still under intense research. This paper explores the scenario where large regular exomoons escape after tidal interchange of angular momentum with its parent planet, becoming small planets by themselves. We name this hypothetical type of object a ploonet. By performing semi-analytical simulations of tidal interactions between a large moon with a close-in giant, and integrating numerically their orbits for several Myr, we found that in ∼50 per cent of the cases a young ploonet may survive ejection from the planetary system, or collision with its parent planet and host star, being in principle detectable. Volatile-rich ploonets are dramatically affected by stellar radiation during both planetocentric and siderocentric orbital evolution, and their radius and mass change significantly due to the sublimation of most of their material during time-scales of hundreds of Myr. We estimate the photometric signatures that ploonets may produce if they transit the star during the phase of evaporation, and compare them with noisy light curves of known objects (Kronian stars and non-periodical dips in dusty light curves). Additionally, the typical transit timing variations (TTV) induced by the interaction of a ploonet with its planet are computed. We find that present and future photometric surveys' capabilities can detect these effects and distinguish them from those produced by other nearby planetary encounters.Fil: Sucerquia, Mario. Universidad de Antioquia. Facultad de Física; Colombia. Pontificia Universidad Católica de Chile; ChileFil: Alvarado-Montes, Jaime A.. Macquarie University. Faculty Of Science And Engineering. Department Of Earth And Planetary Sciences.; Australia. Universidad de Antioquia. Facultad de Física; ColombiaFil: Zuluaga, Jorge I.. Universidad de Antioquia; ColombiaFil: Cuello, Nicolas. Pontificia Universidad Católica de Chile; Chile. Universidad de Buenos Aires. Facultad de Ciencias Sociales. Instituto de Investigaciones "Gino Germani"; ArgentinaFil: Giuppone, Cristian Andrés. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaWiley Blackwell Publishing, Inc2019-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/120850Sucerquia, Mario; Alvarado-Montes, Jaime A.; Zuluaga, Jorge I.; Cuello, Nicolas; Giuppone, Cristian Andrés; Ploonets: Formation, evolution, and detectability of tidally detached exomoons; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 489; 2; 7-2019; 2313-23220035-87111365-2966CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1906.11400info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stz2110info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:01:34Zoai:ri.conicet.gov.ar:11336/120850instacron: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:34982025-09-29 10:01:35.218CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Ploonets: Formation, evolution, and detectability of tidally detached exomoons
title Ploonets: Formation, evolution, and detectability of tidally detached exomoons
spellingShingle Ploonets: Formation, evolution, and detectability of tidally detached exomoons
Sucerquia, Mario
PLANETS AND SATELLITES: ATMOSPHERES
PLANETS AND SATELLITES: DYNAMICAL EVOLUTION AND STABILITY
TECHNIQUES: PHOTOMETRIC
title_short Ploonets: Formation, evolution, and detectability of tidally detached exomoons
title_full Ploonets: Formation, evolution, and detectability of tidally detached exomoons
title_fullStr Ploonets: Formation, evolution, and detectability of tidally detached exomoons
title_full_unstemmed Ploonets: Formation, evolution, and detectability of tidally detached exomoons
title_sort Ploonets: Formation, evolution, and detectability of tidally detached exomoons
dc.creator.none.fl_str_mv Sucerquia, Mario
Alvarado-Montes, Jaime A.
Zuluaga, Jorge I.
Cuello, Nicolas
Giuppone, Cristian Andrés
author Sucerquia, Mario
author_facet Sucerquia, Mario
Alvarado-Montes, Jaime A.
Zuluaga, Jorge I.
Cuello, Nicolas
Giuppone, Cristian Andrés
author_role author
author2 Alvarado-Montes, Jaime A.
Zuluaga, Jorge I.
Cuello, Nicolas
Giuppone, Cristian Andrés
author2_role author
author
author
author
dc.subject.none.fl_str_mv PLANETS AND SATELLITES: ATMOSPHERES
PLANETS AND SATELLITES: DYNAMICAL EVOLUTION AND STABILITY
TECHNIQUES: PHOTOMETRIC
topic PLANETS AND SATELLITES: ATMOSPHERES
PLANETS AND SATELLITES: DYNAMICAL EVOLUTION AND STABILITY
TECHNIQUES: PHOTOMETRIC
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Close-in giant planets represent the most significant evidence of planetary migration. If large exomoons form around migrating giant planets which are more stable (e.g. those in the Solar system), what happens to these moons after migration is still under intense research. This paper explores the scenario where large regular exomoons escape after tidal interchange of angular momentum with its parent planet, becoming small planets by themselves. We name this hypothetical type of object a ploonet. By performing semi-analytical simulations of tidal interactions between a large moon with a close-in giant, and integrating numerically their orbits for several Myr, we found that in ∼50 per cent of the cases a young ploonet may survive ejection from the planetary system, or collision with its parent planet and host star, being in principle detectable. Volatile-rich ploonets are dramatically affected by stellar radiation during both planetocentric and siderocentric orbital evolution, and their radius and mass change significantly due to the sublimation of most of their material during time-scales of hundreds of Myr. We estimate the photometric signatures that ploonets may produce if they transit the star during the phase of evaporation, and compare them with noisy light curves of known objects (Kronian stars and non-periodical dips in dusty light curves). Additionally, the typical transit timing variations (TTV) induced by the interaction of a ploonet with its planet are computed. We find that present and future photometric surveys' capabilities can detect these effects and distinguish them from those produced by other nearby planetary encounters.
Fil: Sucerquia, Mario. Universidad de Antioquia. Facultad de Física; Colombia. Pontificia Universidad Católica de Chile; Chile
Fil: Alvarado-Montes, Jaime A.. Macquarie University. Faculty Of Science And Engineering. Department Of Earth And Planetary Sciences.; Australia. Universidad de Antioquia. Facultad de Física; Colombia
Fil: Zuluaga, Jorge I.. Universidad de Antioquia; Colombia
Fil: Cuello, Nicolas. Pontificia Universidad Católica de Chile; Chile. Universidad de Buenos Aires. Facultad de Ciencias Sociales. Instituto de Investigaciones "Gino Germani"; Argentina
Fil: Giuppone, Cristian Andrés. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
description Close-in giant planets represent the most significant evidence of planetary migration. If large exomoons form around migrating giant planets which are more stable (e.g. those in the Solar system), what happens to these moons after migration is still under intense research. This paper explores the scenario where large regular exomoons escape after tidal interchange of angular momentum with its parent planet, becoming small planets by themselves. We name this hypothetical type of object a ploonet. By performing semi-analytical simulations of tidal interactions between a large moon with a close-in giant, and integrating numerically their orbits for several Myr, we found that in ∼50 per cent of the cases a young ploonet may survive ejection from the planetary system, or collision with its parent planet and host star, being in principle detectable. Volatile-rich ploonets are dramatically affected by stellar radiation during both planetocentric and siderocentric orbital evolution, and their radius and mass change significantly due to the sublimation of most of their material during time-scales of hundreds of Myr. We estimate the photometric signatures that ploonets may produce if they transit the star during the phase of evaporation, and compare them with noisy light curves of known objects (Kronian stars and non-periodical dips in dusty light curves). Additionally, the typical transit timing variations (TTV) induced by the interaction of a ploonet with its planet are computed. We find that present and future photometric surveys' capabilities can detect these effects and distinguish them from those produced by other nearby planetary encounters.
publishDate 2019
dc.date.none.fl_str_mv 2019-07
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
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/120850
Sucerquia, Mario; Alvarado-Montes, Jaime A.; Zuluaga, Jorge I.; Cuello, Nicolas; Giuppone, Cristian Andrés; Ploonets: Formation, evolution, and detectability of tidally detached exomoons; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 489; 2; 7-2019; 2313-2322
0035-8711
1365-2966
CONICET Digital
CONICET
url http://hdl.handle.net/11336/120850
identifier_str_mv Sucerquia, Mario; Alvarado-Montes, Jaime A.; Zuluaga, Jorge I.; Cuello, Nicolas; Giuppone, Cristian Andrés; Ploonets: Formation, evolution, and detectability of tidally detached exomoons; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 489; 2; 7-2019; 2313-2322
0035-8711
1365-2966
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1906.11400
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stz2110
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
_version_ 1844613810981175296
score 13.070432

Publicaciones similares