TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Article
Saunders, Nicholas, Grunblatt, Samuel K., Chontos, Ashley, Dai, Fei, Huber, Daniel, Zhang, Jingwen, Stefánsson, Guđmundur, van Saders, Jennifer L., Winn, Joshua N., Hey, Daniel, Howard, Andrew W., Fulton, Benjamin, Isaacson, Howard, Beard, Corey, Giacalone, Steven, Van Zandt, Judah, Akana Murphy, Joseph M., Rice, Malena, Blunt, Sarah, ..., Yeh, Sherry. 2024. "TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence." The Astronomical Journal. 168 (2). https://doi.org/10.3847/1538-3881/ad543b
| Article Title | TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence |
|---|---|
| ERA Journal ID | 1048 |
| Article Category | Article |
| Authors | Saunders, Nicholas, Grunblatt, Samuel K., Chontos, Ashley, Dai, Fei, Huber, Daniel, Zhang, Jingwen, Stefánsson, Guđmundur, van Saders, Jennifer L., Winn, Joshua N., Hey, Daniel, Howard, Andrew W., Fulton, Benjamin, Isaacson, Howard, Beard, Corey, Giacalone, Steven, Van Zandt, Judah, Akana Murphy, Joseph M., Rice, Malena, Blunt, Sarah, Turtelboom, Emma, Dalba, Paul A., Lubin, Jack, Brinkman, Casey, Louden, Emma M., Page, Emma, Watkins, Cristilyn N., Collins, Karen A., Stockdale, Chris, Tan, Thiam-Guan, Schwarz, Richard P., Massey, Bob, Howell, Steve B., Vanderburg, Andrew, Ricker, George R., Jenkins, Jon M., Seager, Sara, Christiansen, Jessie L., Daylan, Tansu, Falk, Ben, Brodheim, Max, Gibson, Steven R., Hill, Grant M., Holden, Bradford, Householder, Aaron, Kaye, Stephen, Laher, Russ R., Lanclos, Kyle, Petigura, Erik A., Roy, Arpita, Rubenzahl, Ryan A., Schwab, Christian, Shaum, Abby P., Sirk, Martin M., Smith, Christopher L., Walawende, Josh and Yeh, Sherry |
| Journal Title | The Astronomical Journal |
| Journal Citation | 168 (2) |
| Article Number | 81 |
| Number of Pages | 17 |
| Year | 2024 |
| Publisher | IOP Publishing |
| Place of Publication | United States |
| ISSN | 0004-6256 |
| 1538-3881 | |
| Digital Object Identifier (DOI) | https://doi.org/10.3847/1538-3881/ad543b |
| Web Address (URL) | https://iopscience.iop.org/article/10.3847/1538-3881/ad543b |
| Abstract | 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 (≳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 ∼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 ∼500 Myr. Comparison with a simplified tidal evolution model shows that obliquity damping needs to be ∼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. |
| Keywords | Stellar evolution; Tides; Exoplanet astronomy; Exoplanet dynamics; Exoplanet detection methods; Exoplanet evolution; Exoplanet migration; Exoplanets ; Late stellar evolution |
| Contains Sensitive Content | Does not contain sensitive content |
| ANZSRC Field of Research 2020 | 5101. Astronomical sciences |
| Byline Affiliations | University of Hawaii, United States |
| Johns Hopkins University, United States | |
| Princeton University, United States | |
| University of Amsterdam, Netherlands | |
| California Institute of Technology (Caltech), United States | |
| NASA Exoplanet Science Institute, United States | |
| University of California Berkeley, United States | |
| Centre for Astrophysics | |
| University of California Irvine, United States | |
| University of California Santa Cruz, United States | |
| Yale University, United States | |
| Northwestern University, United States | |
| Lehigh University, United States | |
| Center for Astrophysics Harvard and Smithsonian, United States | |
| Hazelwood Observatory, Australia | |
| Perth Exoplanet Survey Telescope Observatory, Australia | |
| Villa ‘39 Observatory, United States | |
| NASA Ames Research Center, United States | |
| Massachusetts Institute of Technology, United States | |
| Washington University of St Louis, United States | |
| Space Telescope Science Institute, United States | |
| W. M. Keck Observatory, United States | |
| Caltech Optical Observatories, United States | |
| University of California Los Angeles, United States | |
| Astrophysics & Space Institute, United States | |
| Macquarie University |
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