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Abstract
Abstract HIP 67522 b is a 17 Myr old, close-in (P orb = 6.96 days), Jupiter-sized (R = 10 R ⊕) transiting planet orbiting a Sun-like star in the Sco–Cen OB association. We present our measurement of the system’s projected orbital obliquity via two spectroscopic transit observations using the CHIRON spectroscopic facility. We present a global model that accounts for large surface brightness features typical of such young stars during spectroscopic transit observations. With a value of ∣ λ ∣ = 5.8 − 5.7 + 2.8 ° it is unlikely that this well-aligned system is the result of a high-eccentricity-driven migration history. By being the youngest planet with a known obliquity, HIP 67522 b holds a special place in contributing to our understanding of giant planet formation and evolution. Our analysis shows the feasibility of such measurements for young and very active stars.
Highlights
One of the oldest puzzles in the field of exoplanets is the origin of short-orbit gas giants
We present our measurement of the system’s projected orbital obliquity via two spectroscopic transit observations using the CHIRON spectroscopic facility
We present a global model that accounts for large surface brightness features typical of such young stars during spectroscopic transit observations
Summary
One of the oldest puzzles in the field of exoplanets is the origin of short-orbit gas giants. Star-planet tidal interactions, resulting in angular momentum exchanges between a host star and its planet, have the ability to circularize and shrink planetary orbits and alter the star’s rotation axis alignment. It became possible to compare the obliquity distribution for very young stars (< 100 Myr) against that of more mature stars. These young planetary systems have yet been influenced by star-planet tidal effects, and provide a glimpse into the primordial orbits of planets post-formation. The recent efforts to characterize young planets discovered by the K2 and Transiting Exoplanet Survey Satellite (TESS, Ricker et al 2016) missions, such as AU Mic b, (Palle et al 2020; Addison et al 2020; Martioli et al 2020; Hirano et al 2020), V1298 Tau c, (David et al 2019; Feinstein et al 2021), DS Tuc Ab, (Zhou et al 2020; Montet et al 2020) and TOI 942 b, (Wirth et al 2021; Zhou et al 2021), have the potential to deliver key insights on the formation and
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