Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c
Article
de Beurs, Zoë, de Wit, Julien, Venner, Alexander, Berardo, David, Bryan, Jared, Winn, Joshua N., Fulton, Benjamin J and Howard, Andrew W. 2023. "Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c." The Astronomical Journal. 166 (4). https://doi.org/10.3847/1538-3881/acedf1
| Article Title | Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c |
|---|---|
| ERA Journal ID | 1048 |
| Article Category | Article |
| Authors | de Beurs, Zoë, de Wit, Julien, Venner, Alexander, Berardo, David, Bryan, Jared, Winn, Joshua N., Fulton, Benjamin J and Howard, Andrew W |
| Journal Title | The Astronomical Journal |
| Journal Citation | 166 (4) |
| Article Number | 136 |
| Number of Pages | 13 |
| Year | 2023 |
| Publisher | IOP Publishing |
| Place of Publication | United States |
| ISSN | 0004-6256 |
| 1538-3881 | |
| Digital Object Identifier (DOI) | https://doi.org/10.3847/1538-3881/acedf1 |
| Web Address (URL) | https://iopscience.iop.org/article/10.3847/1538-3881/acedf1/meta |
| Abstract | One possible formation mechanism for Hot Jupiters is that high-eccentricity gas giants experience tidal interactions with their host star that cause them to lose orbital energy and migrate inwards. We study these types of tidal interactions in an eccentric Hot Jupiter called HAT-P-2 b, which is a system where a long-period companion has been suggested and hints of orbital evolution were detected. Using 5 additional years of radial velocity (RV) measurements, we further investigate these phenomena. We investigated the long-period companion by jointly fitting RVs and Hipparcos-Gaia astrometry and confirmed this long-period companion, significantly narrowed down the range of possible periods ( P 2 = 8500 ? 1500 + 2600 days), and determined that it must be a substellar object ( 10.7 ? 2.2 + 5.2 M j). We also developed a modular pipeline to simultaneously model rapid orbital evolution and the long-period companion. We find that the rate and significance of evolution are highly dependent on the long-period companion modeling choices. In some cases the orbital rates of change reached de / dt = 3.28 ? 1.72 + 1.75 × 10 ? 3 yr?1, d ?/dt = 1.12° ± 0.22° yr?1, which corresponds to a ?321 yr apsidal precession period. In other cases, the data is consistent with de/dt = 7.67 ± 18.6 × 10?4 yr?1, d ?/dt = 0.76° ± 0.24° yr?1. The most rapid changes found are significantly larger than the expected relativistic precession rate and could be caused by transient tidal planet-star interactions. To definitively determine the magnitude and significance of potential orbital evolution in HAT-P-2 b, we recommend further monitoring with RVs and precise transit and eclipse timings. |
| Keywords | Star-planet interactions; Orbital evolution; Astrometry; Radial velocity; Hot Jupiters; Exoplanets |
| ANZSRC Field of Research 2020 | 5101. Astronomical sciences |
| Byline Affiliations | Massachusetts Institute of Technology, United States |
| Centre for Astrophysics | |
| Princeton University, United States | |
| California Institute of Technology (Caltech), United States |
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