The PFS view of TOI-677 b: A spin-orbit aligned warm Jupiter in a dynamically hot system
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| Format: | Preprint |
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2024
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| author | Hu, Qingru Rice, Malena Wang, Xian-Yu Wang, Songhu Shporer, Avi Teske, Johanna K. Yee, Samuel W. Butler, R. Paul Shectman, Stephen Crane, Jeffrey D. Collins, Karen A. Collins, Kevin I. |
| author_facet | Hu, Qingru Rice, Malena Wang, Xian-Yu Wang, Songhu Shporer, Avi Teske, Johanna K. Yee, Samuel W. Butler, R. Paul Shectman, Stephen Crane, Jeffrey D. Collins, Karen A. Collins, Kevin I. |
| contents | TOI-677 b is part of an emerging class of ``tidally-detached'' gas giants ($a/R_\star \gtrsim 11$) that exhibit large orbital eccentricities and yet low stellar obliquities. Such sources pose a challenge for models of giant planet formation, which must account for the excitation of high eccentricities without large changes in the orbital inclination. In this work, we present a new Rossiter-McLaughlin (RM) measurement for the tidally-detached warm Jupiter TOI-677 b, obtained using high-precision radial velocity observations from the PFS/Magellan spectrograph. Combined with previously published observations from the ESPRESSO/VLT spectrograph, we derive one of the most precisely constrained sky-projected spin-orbit angle measurements to date for an exoplanet. The combined fit offers a refined set of self-consistent parameters, including a low sky-projected stellar obliquity of $λ=3.2^{+1.6}_{-1.5}$ deg and a moderately high eccentricity of $e=0.460^{+0.019}_{-0.018}$, that further constrains the puzzling architecture of this system. We examine several potential scenarios that may have produced the current TOI-677 orbital configuration, ultimately concluding that TOI-677 b most likely had its eccentricity excited through disk-planet interactions. This system adds to a growing population of aligned warm Jupiters on eccentric orbits around hot ($T_{\rm eff}>6100$ K) stars. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2402_07346 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The PFS view of TOI-677 b: A spin-orbit aligned warm Jupiter in a dynamically hot system Hu, Qingru Rice, Malena Wang, Xian-Yu Wang, Songhu Shporer, Avi Teske, Johanna K. Yee, Samuel W. Butler, R. Paul Shectman, Stephen Crane, Jeffrey D. Collins, Karen A. Collins, Kevin I. Earth and Planetary Astrophysics TOI-677 b is part of an emerging class of ``tidally-detached'' gas giants ($a/R_\star \gtrsim 11$) that exhibit large orbital eccentricities and yet low stellar obliquities. Such sources pose a challenge for models of giant planet formation, which must account for the excitation of high eccentricities without large changes in the orbital inclination. In this work, we present a new Rossiter-McLaughlin (RM) measurement for the tidally-detached warm Jupiter TOI-677 b, obtained using high-precision radial velocity observations from the PFS/Magellan spectrograph. Combined with previously published observations from the ESPRESSO/VLT spectrograph, we derive one of the most precisely constrained sky-projected spin-orbit angle measurements to date for an exoplanet. The combined fit offers a refined set of self-consistent parameters, including a low sky-projected stellar obliquity of $λ=3.2^{+1.6}_{-1.5}$ deg and a moderately high eccentricity of $e=0.460^{+0.019}_{-0.018}$, that further constrains the puzzling architecture of this system. We examine several potential scenarios that may have produced the current TOI-677 orbital configuration, ultimately concluding that TOI-677 b most likely had its eccentricity excited through disk-planet interactions. This system adds to a growing population of aligned warm Jupiters on eccentric orbits around hot ($T_{\rm eff}>6100$ K) stars. |
| title | The PFS view of TOI-677 b: A spin-orbit aligned warm Jupiter in a dynamically hot system |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2402.07346 |