Evolution of BD-14 3065b (TOI-4987b) from giant planet to brown dwarf as possible evidence of deuterium burning at old stellar ages

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dc.contributor.authorSubjak, Jan
dc.contributor.authorLatham, David W.
dc.contributor.authorQuinn, Samuel N.
dc.contributor.authorBerlind, Perry
dc.contributor.authorCalkins, Michael L.
dc.contributor.authorEsquerdo, Gilbert A.
dc.contributor.authorBrahm, Rafael
dc.contributor.authorCaballero, Jose A.
dc.contributor.authorCollins, Karen A.
dc.contributor.authorGuenther, Eike
dc.contributor.authorJanik, Jan
dc.contributor.authorKabath, Petr
dc.contributor.authorSchwarz, Richard P.
dc.contributor.authorTan, Thiam-Guan
dc.contributor.authorVanzi, Leonardo
dc.contributor.authorZambelli, Roberto
dc.contributor.authorZiegler, Carl
dc.contributor.authorJenkins, Jon M.
dc.contributor.authorMireles, Ismael
dc.contributor.authorSeager, Sara
dc.contributor.authorShporer, Avi
dc.contributor.authorStriegel, Stephanie
dc.contributor.authorWinn, Joshua N.
dc.date.accessioned2025-01-20T16:09:33Z
dc.date.available2025-01-20T16:09:33Z
dc.date.issued2024
dc.description.abstractThe present study confirms BD-14 3065b as a transiting planet-brown dwarf in a triple-star system, with a mass near the deuterium-burning boundary. BD-14 3065b has the largest radius observed within the sample of giant planets and brown dwarfs around post-main sequence stars. Its orbital period is 4.3 days and it transits a subgiant F-type star with a mass of M-* = 1.41 +/- 0.05 M-circle dot, a radius of R-* = 2.35 +/- 0.08 R-circle dot, an effective temperature of T-eff = 6935 +/- 90 K, and a metallicity of -0.34 +/- 0.05 dex. By combining TESS photometry with high-resolution spectra acquired with the TRES and Pucheros+ spectrographs, we measured a mass of M-p = 12.37 +/- 0.92 M-Jup and a radius of R-p = 1.926 +/- 0.094 R-Jup. Our discussion of potential processes that could be responsible for the inflated radius led us to conclude that deuterium burning is a plausible explanation for the heating taking place in BD-14 3065b's interior. Detections of the secondary eclipse with TESS photometry enabled a precise determination of the eccentricity, e(p) = 0.066 +/- 0.011, and reveal that BD-14 3065b has a brightness temperature of 3520 +/- 130 K. With its unique characteristics, BD-14 3065b presents an excellent opportunity to study its atmosphere via thermal emission spectroscopy.
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/202349028
dc.identifier.eissn1432-0746
dc.identifier.issn0004-6361
dc.identifier.urihttps://doi.org/10.1051/0004-6361/202349028
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/90156
dc.identifier.wosidWOS:001289291100017
dc.language.isoen
dc.revistaAstronomy & astrophysics
dc.rightsacceso restringido
dc.subjecttechniques: photometric
dc.subjecttechniques: radial velocities
dc.subjecttechniques: spectroscopic
dc.subjectplanets and satellites: gaseous planets
dc.subjectbrown dwarfs
dc.subject.ods13 Climate Action
dc.subject.odspa13 Acción por el clima
dc.titleEvolution of BD-14 3065b (TOI-4987b) from giant planet to brown dwarf as possible evidence of deuterium burning at old stellar ages
dc.typeartículo
dc.volumen688
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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