Stellar Obliquity of the Ultra-Short-Period Planet System HD 93963
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2025
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| author | Teng, Huan-Yu Dai, Fei Howard, Andrew W. Halverson, Samuel Isaacson, Howard Kokubo, Eiichiro Rubenzahl, Ryan A. Fulton, Benjamin Householder, Aaron Lubin, Jack Giacalone, Steven Handley, Luke Van Zandt, Judah Petigura, Erik A. Ong, J. M. Joel Premnath, Pranav Yu, Haochuan Gibson, Steven R. Rider, Kodi Roy, Arpita Baker, Ashley Edelstein, Jerry Smith, Chris Walawender, Josh Lee, Byeong-Cheol Liu, Yu-Juan Winn, Joshua N. |
| author_facet | Teng, Huan-Yu Dai, Fei Howard, Andrew W. Halverson, Samuel Isaacson, Howard Kokubo, Eiichiro Rubenzahl, Ryan A. Fulton, Benjamin Householder, Aaron Lubin, Jack Giacalone, Steven Handley, Luke Van Zandt, Judah Petigura, Erik A. Ong, J. M. Joel Premnath, Pranav Yu, Haochuan Gibson, Steven R. Rider, Kodi Roy, Arpita Baker, Ashley Edelstein, Jerry Smith, Chris Walawender, Josh Lee, Byeong-Cheol Liu, Yu-Juan Winn, Joshua N. |
| contents | We report an observation of the Rossiter-McLaughlin (RM) effect of the transiting planet HD 93963 Ac, a mini-Neptune planet orbiting a G0-type star with an orbital period of $P_{\rm{c}} = 3.65\,\mathrm{d}$, accompanied by an inner super-Earth planet with $P_{\rm{b}} = 1.04\,\mathrm{d}$. We observed a full transit of planet c on 2024 May 3rd UT with Keck/KPF. The observed RM effect has an amplitude of $\sim 1\,\mathrm{m\,s}^{-1}$ and implies a sky-projected obliquity of $λ= 14^{+17}_{-19}$ degrees for HD 93963 Ac. Our dynamical analysis suggests that the two inner planets are likely well aligned with the stellar spin, to within a few degrees, thus allowing both to transit. Along with WASP-47, 55 Cnc, and HD 3167, HD 93963 is the fourth planetary system with an ultra-short-period planet and obliquity measurement(s) of any planet(s) in the system. HD 93963, WASP-47, and 55 Cnc favor largely coplanar orbital architectures, whereas HD 3167 has been reported to have a large mutual inclination ($\sim$100$^\circ$) between its transiting planets b and c. In this configuration, the probability that both planets transit is low. Moreover, one planet would quickly evolve to be non-transiting due to nodal precession. Future missions such as ESO/PLATO should detect the resulting transit duration variations. We encourage additional obliquity measurements of the HD 3167 system to better constrain its orbital architecture. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2505_10804 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Stellar Obliquity of the Ultra-Short-Period Planet System HD 93963 Teng, Huan-Yu Dai, Fei Howard, Andrew W. Halverson, Samuel Isaacson, Howard Kokubo, Eiichiro Rubenzahl, Ryan A. Fulton, Benjamin Householder, Aaron Lubin, Jack Giacalone, Steven Handley, Luke Van Zandt, Judah Petigura, Erik A. Ong, J. M. Joel Premnath, Pranav Yu, Haochuan Gibson, Steven R. Rider, Kodi Roy, Arpita Baker, Ashley Edelstein, Jerry Smith, Chris Walawender, Josh Lee, Byeong-Cheol Liu, Yu-Juan Winn, Joshua N. Earth and Planetary Astrophysics We report an observation of the Rossiter-McLaughlin (RM) effect of the transiting planet HD 93963 Ac, a mini-Neptune planet orbiting a G0-type star with an orbital period of $P_{\rm{c}} = 3.65\,\mathrm{d}$, accompanied by an inner super-Earth planet with $P_{\rm{b}} = 1.04\,\mathrm{d}$. We observed a full transit of planet c on 2024 May 3rd UT with Keck/KPF. The observed RM effect has an amplitude of $\sim 1\,\mathrm{m\,s}^{-1}$ and implies a sky-projected obliquity of $λ= 14^{+17}_{-19}$ degrees for HD 93963 Ac. Our dynamical analysis suggests that the two inner planets are likely well aligned with the stellar spin, to within a few degrees, thus allowing both to transit. Along with WASP-47, 55 Cnc, and HD 3167, HD 93963 is the fourth planetary system with an ultra-short-period planet and obliquity measurement(s) of any planet(s) in the system. HD 93963, WASP-47, and 55 Cnc favor largely coplanar orbital architectures, whereas HD 3167 has been reported to have a large mutual inclination ($\sim$100$^\circ$) between its transiting planets b and c. In this configuration, the probability that both planets transit is low. Moreover, one planet would quickly evolve to be non-transiting due to nodal precession. Future missions such as ESO/PLATO should detect the resulting transit duration variations. We encourage additional obliquity measurements of the HD 3167 system to better constrain its orbital architecture. |
| title | Stellar Obliquity of the Ultra-Short-Period Planet System HD 93963 |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2505.10804 |