A Larger Sample Confirms Small Planets around Hot Stars Are Misaligned
Article
Louden, Emma M., Wang, Songhu, Winn, Joshua N., Petigura, Erik A., Isaacson, Howard, Handley, Luke, Yee, Samuel W., Beard, Corey, Akana Murphy, Joseph M. and Laughlin, Gregory. 2024. "A Larger Sample Confirms Small Planets around Hot Stars Are Misaligned." The Astrophysical Journal Letters. 968 (1). https://doi.org/10.3847/2041-8213/ad4b1b
Article Title | A Larger Sample Confirms Small Planets around Hot Stars Are Misaligned |
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ERA Journal ID | 45091 |
Article Category | Article |
Authors | Louden, Emma M., Wang, Songhu, Winn, Joshua N., Petigura, Erik A., Isaacson, Howard, Handley, Luke, Yee, Samuel W., Beard, Corey, Akana Murphy, Joseph M. and Laughlin, Gregory |
Journal Title | The Astrophysical Journal Letters |
Journal Citation | 968 (1) |
Article Number | L2 |
Number of Pages | 13 |
Year | 2024 |
Publisher | IOP Publishing |
Place of Publication | United Kingdom |
ISSN | 2041-8205 |
2041-8213 | |
Digital Object Identifier (DOI) | https://doi.org/10.3847/2041-8213/ad4b1b |
Web Address (URL) | https://iopscience.iop.org/article/10.3847/2041-8213/ad4b1b |
Abstract | The distribution of stellar obliquities provides critical insight into the formation and evolution pathways of exoplanets. In the past decade, it was found that hot stars hosting hot Jupiters are more likely to have high obliquities than cool stars, but it is not clear whether this trend exists only for hot Jupiters or holds for other types of planets. In this work, we extend the study of the obliquities of hot (6250-7000 K) stars with transiting super-Earth-sized and sub-Neptune-sized planets. We constrain the obliquity distribution based on measurements of the stars’ projected rotation velocities. Our sample consists of 170 TESS and Kepler planet-hosting stars and 180 control stars chosen to have indistinguishable spectroscopic characteristics. In our analysis, we find evidence suggesting that the planet hosts have a systematically higher ? sin i ? compared to the control sample. This result implies that the planet hosts tend to have lower obliquities. However, the observed difference in ? sin i ? is not significant enough to confirm spin-orbit alignment as it is 3.8? away from perfect alignment. We also find evidence that within the planet-hosting stars there is a trend of higher obliquity (lower ? sin i ? ) for the hotter stars (T eff > 6250 K) than for the cooler stars in the sample. This suggests that hot stars hosting smaller planets exhibit a broader obliquity distribution ( ? sin i ? = 0.79 ± 0.053 ) than cooler planet-hosting stars, indicating that high obliquities are not exclusive to hot Jupiters and instead are more broadly tied to hot stars. © 2024. The Author(s). Published by the American Astronomical Society. |
Keywords | Exoplanets; Exoplanet dynam |
Contains Sensitive Content | Does not contain sensitive content |
ANZSRC Field of Research 2020 | 5101. Astronomical sciences |
Byline Affiliations | Yale University, United States |
Indiana University, United States | |
Princeton University, United States | |
University of California Berkeley, United States | |
University of California Los Angeles, United States | |
Centre for Astrophysics | |
California Institute of Technology (Caltech), United States | |
Center for Astrophysics Harvard and Smithsonian, United States | |
University of California Irvine, United States | |
University of California Santa Cruz, United States |
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