TOI-1859b: A 64 Day Warm Jupiter on an Eccentric and Misaligned Orbit
Bieryla, Allyson; Latham, David W.; Mahadevan, Suvrath; Rice, Malena; Zhou, George; Howell, Steve B.; Dalba, Paul A.; Collins, Karen A.; Ricker, George R.; Winn, Joshua N.; Jenkins, Jon M.; Seager, S.; Shporer, Avi; Dragomir, Diana; Rapetti, David; Logsdon, Sarah E.; Huang, Chelsea X.; Wang, Songhu; Sefako, Ramotholo; McElwain, Michael W.; Kanodia, Shubham; Ninan, Joe P.; Halverson, Samuel; Robertson, Paul; Roy, Arpita; Schwab, Christian; Terrien, Ryan C.; Alvarado-Montes, Jaime A.; Dong, Jiayin; Srdoc, Gregor; Dawson, Rebekah I.; Stefánsson, Gudmundur K.; Laloum, Didier; Villanueva, Steven
United States, Australia, Switzerland, Croatia, South Africa
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.