The OATMEAL Survey. I. Low Stellar Obliquity in the Transiting Brown Dwarf System GPX-1

November 2024 • 2024AJ....168..189G

Authors • Giacalone, Steven • Dai, Fei • Zanazzi, J. J. • Howard, Andrew W. • Dressing, Courtney D. • Winn, Joshua N. • Rubenzahl, Ryan A. • Carmichael, Theron W. • Vowell, Noah • Kesseli, Aurora • Halverson, Samuel • Isaacson, Howard • Brodheim, Max • Deich, William • Fulton, Benjamin J. • Gibson, Steven R. • Hill, Grant M. • Holden, Bradford • Householder, Aaron • Kaye, Stephen • Laher, Russ R. • Lanclos, Kyle • Payne, Joel • Petigura, Erik A. • Roy, Arpita • Schwab, Christian • Shaum, Abby P. • Sirk, Martin M. • Smith, Chris • Stefánsson, Guðmundur • Walawender, Josh • Wang, Sharon X. • Weiss, Lauren M. • Yeh, Sherry

Abstract • We introduce the OATMEAL survey, an effort to measure the obliquities of stars with transiting brown dwarf companions. We observed a transit of the close-in (P _orb = 1.74 days) brown dwarf GPX-1 b using the Keck Planet Finder spectrograph to measure the sky-projected angle between its orbital axis and the spin axis of its early F-type host star (λ). We measured λ = 6.°9 ± 10.°0, suggesting an orbit that is prograde and well aligned with the stellar equator. Hot Jupiters around early F stars are frequently found to have highly misaligned orbits, with polar and retrograde orbits being commonplace. It has been theorized that these misalignments stem from dynamical interactions, such as von Zeipel–Kozai–Lidov cycles, and are retained over long timescales due to weak tidal dissipation in stars with radiative envelopes. By comparing GPX-1 to similar systems under the frameworks of different tidal evolution theories, we argued that the rate of tidal dissipation is too slow to have re-aligned the system. This suggests that GPX-1 may have arrived at its close-in orbit via coplanar high-eccentricity migration or migration through an aligned protoplanetary disk. Our result for GPX-1 is one of few measurements of the obliquity of a star with a transiting brown dwarf. By enlarging the number of such measurements and comparing them with hot-Jupiter systems, we will more clearly discern the differences between the mechanisms that dictate the formation and evolution of both classes of objects.

Links

• PREPRINT http://arxiv.org/abs/2407.21235
• ELECTR https://doi.org/10.3847%2F1538-3881%2Fad785a