Resonant sub-Neptunes are puffier

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dc.citation.articleNumberL1en_US
dc.citation.journalTitleAstronomy & Astrophysicsen_US
dc.citation.volumeNumber687en_US
dc.contributor.authorLeleu, Adrienen_US
dc.contributor.authorDelisle, Jean-Baptisteen_US
dc.contributor.authorBurn, Remoen_US
dc.contributor.authorIzidoro, Andréen_US
dc.contributor.authorUdry, Stéphaneen_US
dc.contributor.authorDumusque, Xavieren_US
dc.contributor.authorLovis, Christopheen_US
dc.contributor.authorMillholland, Sarahen_US
dc.contributor.authorParc, Lénaen_US
dc.contributor.authorBouchy, Françoisen_US
dc.contributor.authorBourrier, Vincenten_US
dc.contributor.authorAlibert, Yannen_US
dc.contributor.authorFaria, Joãoen_US
dc.contributor.authorMordasini, Christophen_US
dc.contributor.authorSégransan, Damienen_US
dc.date.accessioned2024-10-08T13:28:37Zen_US
dc.date.available2024-10-08T13:28:37Zen_US
dc.date.issued2024en_US
dc.description.abstractA systematic, population-level discrepancy exists between the densities of exoplanets whose masses have been measured with transit timing variations (TTVs) versus those measured with radial velocities (RVs). Since the TTV planets are predominantly nearly resonant, it is still unclear whether the discrepancy is attributed to detection biases or to astrophysical differences between the nearly resonant and non resonant planet populations. We defined a controlled, unbiased sample of 36 sub-Neptunes characterised by <i>Kepler<i/>, TESS, HARPS, and ESPRESSO. We found that their density depends mostly on the resonant state of the system, with a low probability (of ) that the mass of (nearly) resonant planets is drawn from the same underlying population as the bulk of sub-Neptunes. Increasing the sample to 133 sub-Neptunes reveals finer details: the densities of resonant planets are similar and lower than non-resonant planets, and both the mean and spread in density increase for planets that are away from resonance. This trend is also present in RV-characterised planets alone. In addition, TTVs and RVs have consistent density distributions for a given distance to resonance. We also show that systems closer to resonances tend to be more co-planar than their spread-out counterparts. These observational trends are also found in synthetic populations, where planets that survived in their original resonant configuration retain a lower density; whereas less compact systems have undergone post-disc giant collisions that increased the planet’s density, while expanding their orbits. Our findings reinforce the claim that resonant systems are archetypes of planetary systems at their birth.en_US
dc.identifier.citationLeleu, A., Delisle, J.-B., Burn, R., Izidoro, A., Udry, S., Dumusque, X., Lovis, C., Millholland, S., Parc, L., Bouchy, F., Bourrier, V., Alibert, Y., Faria, J., Mordasini, C., & Ségransan, D. (2024). Resonant sub-Neptunes are puffier. Astronomy & Astrophysics, 687, L1. https://doi.org/10.1051/0004-6361/202450587en_US
dc.identifier.digitalaa50587-24en_US
dc.identifier.doihttps://doi.org/10.1051/0004-6361/202450587en_US
dc.identifier.urihttps://hdl.handle.net/1911/117935en_US
dc.language.isoengen_US
dc.publisheredp Sciencesen_US
dc.rightsExcept where otherwise noted, this work is licensed under a Creative Commons Attribution (CC BY) license. Permission to reuse, publish, or reproduce the work beyond the terms of the license or beyond the bounds of fair use or other exemptions to copyright law must be obtained from the copyright holder.en_US
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/en_US
dc.titleResonant sub-Neptunes are puffieren_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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