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

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dc.contributor.authorSucerquia, Mario
dc.contributor.authorAlvarado-Montes, Jaime A.
dc.contributor.authorZuluaga, Jorge, I
dc.contributor.authorCuello, Nicolas
dc.contributor.authorGiuppone, Cristian
dc.date.accessioned2025-01-23T21:10:46Z
dc.date.available2025-01-23T21:10:46Z
dc.date.issued2019
dc.description.abstractClose-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 similar to 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.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stz2110
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stz2110
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/100858
dc.identifier.wosidWOS:000489298100065
dc.issue.numero2
dc.language.isoen
dc.pagina.final2322
dc.pagina.inicio2313
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectTechniques: photometric
dc.subjectPlanets and satellites: atmospheres
dc.subjectPlanets and satellites: dynamical evolution and stability
dc.subject.ods13 Climate Action
dc.subject.odspa13 Acción por el clima
dc.titlePloonets: formation, evolution, and detectability of tidally detached exomoons
dc.typeartículo
dc.volumen489
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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