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.
Original language | English (US) |
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Article number | L29 |
Journal | Astrophysical Journal Letters |
Volume | 951 |
Issue number | 2 |
DOIs | |
State | Published - Jul 1 2023 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science