Host-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways

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dc.contributor.authorBanerjee, Bihan
dc.contributor.authorNarang, Mayank
dc.contributor.authorManoj, P.
dc.contributor.authorHenning, Thomas
dc.contributor.authorTyagi, Himanshu
dc.contributor.authorSurya, Arun
dc.contributor.authorNayak, Prasanta K.
dc.contributor.authorTripathi, Mihir
dc.date.accessioned2025-01-20T16:15:35Z
dc.date.available2025-01-20T16:15:35Z
dc.date.issued2024
dc.description.abstractGiant planets exhibit diverse orbital properties, hinting at their distinct formation and dynamic histories. In this paper, using Gaia Data Release 3 (DR3), we investigate if and how the orbital properties of Jupiters are linked to their host star properties, particularly their metallicity and age. We obtain metallicities for main-sequence stars of spectral type F, G, and K, hosting hot, warm, and cold Jupiters with varying eccentricities. We compute the velocity dispersions of the host stars of these three groups using kinematic information from Gaia DR3 and obtain average ages using a velocity dispersion-age relation. We find that the host stars of hot Jupiters are relatively metal rich ([Fe/H] = 0.18 +/- 0.13) and young (median age of 3.97 +/- 0.51 Gyr) compared to the host stars of cold Jupiters in nearly circular orbits, which are relatively metal poor (0.03 +/- 0.18) and older (median age of 6.07 +/- 0.79 Gyr). The host stars of cold Jupiters in high-eccentricity orbits, on the other hand, show metallicities similar to those of the hosts of hot Jupiters, but are older, on average (median age of 6.25 +/- 0.92 Gyr). The similarity in metallicity between the hosts of hot Jupiters and the hosts of cold Jupiters in high-eccentricity orbits supports high-eccentricity migration as the potential origin of hot Jupiters, with the latter serving as the progenitors of hot Jupiters. However, the average age difference between them suggests that the older hot Jupiters may have been engulfed by their host star over timescales similar to 6 Gyr. This allows us to estimate the value of stellar tidal quality factor, Q * ' similar to 10 6 +/- 1 .
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-3881/ad429f
dc.identifier.eissn1538-3881
dc.identifier.issn0004-6256
dc.identifier.urihttps://doi.org/10.3847/1538-3881/ad429f
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/90502
dc.identifier.wosidWOS:001248923400001
dc.issue.numero1
dc.language.isoen
dc.revistaAstronomical journal
dc.rightsacceso restringido
dc.subject.ods13 Climate Action
dc.subject.odspa13 Acción por el clima
dc.titleHost-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways
dc.typeartículo
dc.volumen168
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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