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Dong, Jiayin; Wang, Songhu; Rice, Malena; Zhou, George; Huang, Chelsea X.; Dawson, Rebekah I.; Stefánsson, Gudmundur K.; Halverson, Samuel; Kanodia, Shubham; Mahadevan, Suvrath; McElwain, Michael W.; Alvarado-Montes, Jaime A.; Ninan, Joe P.; Robertson, Paul; Roy, Arpita; Schwab, Christian; Logsdon, Sarah E.; Terrien, Ryan C.; Collins, Karen A.; Srdoc, Gregor; Sefako, Ramotholo; Laloum, Didier; Latham, David W.; Bieryla, Allyson; Dalba, Paul A.; Dragomir, Diana; Villanueva, Steven; Howell, Steve B.; Ricker, George R.; Seager, S.; Winn, Joshua N.; Jenkins, Jon M.; Shporer, Avi; Rapetti, David
Astrophysical journal. Letters, 07/2023, Letnik: 951, Številka: 2Journal Article
Abstract Warm Jupiters are close-in giant planets with relatively large planet–star separations (i.e., 10 < a / R ⋆ < 100). Given their weak tidal interactions with their host stars, measurements of stellar obliquity may be used to probe the initial obliquity distribution and dynamical history for close-in gas giants. Using spectroscopic observations, we confirm the planetary nature of TOI-1859b and determine the stellar obliquity of TOI-1859 to be λ = 38.9 − 2.7 + 2.8 ° relative to its planetary companion using the Rossiter–McLaughlin effect. TOI-1859b is a 64 day warm Jupiter orbiting around a late F dwarf and has an orbital eccentricity of 0.57 − 0.16 + 0.12 inferred purely from transit light curves. The eccentric and misaligned orbit of TOI-1859b is likely an outcome of dynamical interactions, such as planet–planet scattering and planet–disk resonance crossing.
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in: SICRIS
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