Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b

Simple item page
dc.contributor.authorCarleo, Ilaria
dc.contributor.authorBarragan, Oscar
dc.contributor.authorPersson, Carina M.
dc.contributor.authorFridlund, Malcolm
dc.contributor.authorLam, Kristine W. F.
dc.contributor.authorMessina, Sergio
dc.contributor.authorGandolfi, Davide
dc.contributor.authorSmith, Alexis M. S.
dc.contributor.authorJohnson, Marshall C.
dc.contributor.authorCochran, William
dc.contributor.authorOsborne, Hannah L. M.
dc.contributor.authorBrahm, Rafael
dc.contributor.authorCiardi, David R.
dc.contributor.authorCollins, Karen A.
dc.contributor.authorEverett, Mark E.
dc.contributor.authorGiacalone, Steven
dc.contributor.authorGuenther, Eike W.
dc.contributor.authorHatzes, Artie
dc.contributor.authorHellier, Coel
dc.contributor.authorHorner, Jonathan
dc.contributor.authorKabath, Petr
dc.contributor.authorKorth, Judith
dc.contributor.authorMacQueen, Phillip
dc.contributor.authorMasseron, Thomas
dc.contributor.authorMurgas, Felipe
dc.contributor.authorNowak, Grzegorz
dc.contributor.authorRodriguez, Joseph E.
dc.contributor.authorWatkins, Cristilyn N.
dc.contributor.authorWittenmyer, Rob
dc.contributor.authorZhou, George
dc.contributor.authorZiegler, Carl
dc.contributor.authorBieryla, Allyson
dc.contributor.authorBoyd, Patricia T.
dc.contributor.authorClark, Catherine A.
dc.contributor.authorDressing, Courtney D.
dc.contributor.authorEastman, Jason D.
dc.contributor.authorEberhardt, Jan
dc.contributor.authorEndl, Michael
dc.contributor.authorEspinoza, Nestor
dc.contributor.authorFausnaugh, Michael
dc.contributor.authorGuerrero, Natalia M.
dc.contributor.authorHenning, Thomas
dc.contributor.authorHesse, Katharine
dc.contributor.authorHobson, Melissa J.
dc.contributor.authorHowell, Steve B.
dc.contributor.authorJordan, Andres
dc.contributor.authorLatham, David W.
dc.contributor.authorLund, Michael B.
dc.contributor.authorMireles, Ismael
dc.contributor.authorNarita, Norio
dc.contributor.authorTala Pinto, Marcelo
dc.contributor.authorPugh, Teznie
dc.contributor.authorQuinn, Samuel N.
dc.contributor.authorRicker, George
dc.contributor.authorRodriguez, David R.
dc.contributor.authorRojas, Felipe I.
dc.contributor.authorRose, Mark E.
dc.contributor.authorRudat, Alexander
dc.contributor.authorSarkis, Paula
dc.contributor.authorSavel, Arjun B.
dc.contributor.authorSchlecker, Martin
dc.contributor.authorSchwarz, Richard P.
dc.contributor.authorSeager, Sara
dc.contributor.authorShporer, Avi
dc.contributor.authorSmith, Jeffrey C.
dc.contributor.authorStassun, Keivan G.
dc.contributor.authorStockdale, Chris
dc.contributor.authorTrifonov, Trifon
dc.contributor.authorVanderspek, Roland
dc.contributor.authorWinn, Joshua N.
dc.contributor.authorWright, Duncan
dc.date.accessioned2025-01-20T16:07:34Z
dc.date.available2025-01-20T16:07:34Z
dc.date.issued2024
dc.description.abstractContext. Hot and warm Jupiters might have undergone the same formation and evolution path, but the two populations exhibit different distributions of orbital parameters. This challenges our understanding of their actual origin. Aims. We report the results of our warm Jupiters survey, which was carried out with the CHIRON spectrograph within the KESPRINT collaboration. We addressed the question of the population origin by studying two planets that might help to bridge the gap between the two populations. Methods. We confirm two planets and determine their mass. One is a hot Jupiter (with an orbital period shorter than 10 days), TOI-2420 b, and the other is a warm Jupiter, TOI-2485 b. We analyzed them using a wide variety of spectral and photometric data in order to characterize these planetary systems. Results. We found that TOI-2420 b has an orbital period of P-b=5.8 days, a mass of M-b=0.9 M-J, and a radius of R-b=1.3 R-J, with a planetary density of 0.477 g cm(-3). TOI-2485 b has an orbital period of P-b=11.2 days, a mass of M-b=2.4 M-J, and a radius of R-b=1.1 R-J with a density of 2.36 g cm(-3). Conclusions. With the current parameters, the migration history for TOI-2420 b and TOI-2485 b is unclear: Scenarios of a high-eccentricity migration cannot be ruled out, and the characteristics of TOI-2485 b even support this scenario.
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/202451313
dc.identifier.eissn1432-0746
dc.identifier.issn0004-6361
dc.identifier.urihttps://doi.org/10.1051/0004-6361/202451313
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/90005
dc.identifier.wosidWOS:001321174100002
dc.language.isoen
dc.revistaAstronomy & astrophysics
dc.rightsacceso restringido
dc.subjectplanets and satellites: detection
dc.subjectplanets and satellites: gaseous planets
dc.subject.ods13 Climate Action
dc.subject.odspa13 Acción por el clima
dc.titleMass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b
dc.typeartículo
dc.volumen690
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
Files
Collections
Artículos de revistas