TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Creators: name: Saunders, Nicholas
name: Grunblatt, Samuel K.
name: Chontos, Ashley
name: Dai, Fei
name: Huber, Daniel
name: Zhang, Jingwen
name: Stefansson, Gudmundur
name: van Saders, Jennifer L.
name: Winn, Joshua N.
name: Hey, Daniel
name: Howard, Andrew W.
name: Fulton, Benjamin
name: Isaacson, Howard
name: Beard, Corey
name: Giacalone, Steven
name: van Zandt, Judah
name: Murphey, Joseph M. Akana
name: Rice, Malena
name: Blunt, Sarah
name: Turtelboom, Emma
name: Dalba, Paul A.
name: Lubin, Jack
name: Brinkman, Casey
name: Louden, Emma M.
name: Page, Emma
name: Watkins, Cristilyn N.
name: Collins, Karen A.
name: Stockdale, Chris
name: Tan, Thiam-Guan
name: Schwarz, Richard P.
name: Massey, Bob
name: Howell, Steve B.
name: Vanderburg, Andrew
name: Ricker, George R.
name: Jenkins, Jon M.
name: Seager, Sara
name: Christiansen, Jessie L.
name: Daylan, Tansu
name: Falk, Ben
name: Brodheim, Max
name: Gibson, Steven R.
name: Hill, Grant M.
name: Holden, Bradford
name: Householder, Aaron
name: Kaye, Stephen
name: Laher, Russ R.
name: Lanclos, Kyle
name: Petigura, Erik A.
name: Roy, Arpita
name: Rubenzahl, Ryan A.
name: Schwab, Christian
name: Shaum, Abby P.
name: Sirk, Martin M.
name: Smith, Christopher L.
name: Walawender, Josh
name: Yeh, Sherry
Publisher: name: arXiv
Year: 2024
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The degree of alignment between a star's spin axis and the orbital plane of its planets (the stellar obliquity) is related to interesting and poorly understood processes that occur during planet formation and evolution. Hot Jupiters orbiting hot stars ($\gtrsim$6250 K) display a wide range of obliquities, while similar planets orbiting cool stars are preferentially aligned. Tidal dissipation is expected to be more rapid in stars with thick convective envelopes, potentially explaining this trend. Evolved stars provide an opportunity to test the damping hypothesis, particularly stars that were hot on the main sequence and have since cooled and developed deep convective envelopes. We present the first systematic study of the obliquities of hot Jupiters orbiting subgiants that recently developed convective envelopes using Rossiter-McLaughlin observations. Our sample includes two newly discovered systems in the Giants Transiting Giants Survey (TOI-6029 b, TOI-4379 b). We find that the orbits of hot Jupiters orbiting subgiants that have cooled below $\sim$6250 K are aligned or nearly aligned with the spin-axis of their host stars, indicating rapid tidal realignment after the emergence of a stellar convective envelope. We place an upper limit for the timescale of realignment for hot Jupiters orbiting subgiants at $\sim$500 Myr. Comparison with a simplified tidal evolution model shows that obliquity damping needs to be $\sim$4 orders of magnitude more efficient than orbital period decay to damp the obliquity without destroying the planet, which is consistent with recent predictions for tidal dissipation from inertial waves excited by hot Jupiters on misaligned orbits.
description: 22 pages, 14 figures, 3 tables