Slow Rotation for the Super-Puff Planet Kepler-51d
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arXiv
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| Autores principales: | , |
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| Formato: | Preprint |
| Publicado: |
2024
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| _version_ | 1866915014987743232 |
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| author | Lammers, Caleb Winn, Joshua N. |
| author_facet | Lammers, Caleb Winn, Joshua N. |
| contents | Super-puffs are low-density planets of unknown origin and composition. If they form by accreting nebular gas through a circumplanetary disk, one might expect super-puffs to be spinning quickly. Here, we derive upper limits on the rotational oblateness of the super-puff Kepler-51d, based on precise transit observations with the NIRSpec instrument aboard the James Webb Space Telescope. The absence of detectable oblateness-related anomalies in the light curve leads to an upper limit of about $0.15$ on the planet's sky-projected oblateness. Assuming the sky-projected oblateness to be representative of the true oblateness, the rotation period of Kepler-51d is $\gtrsim 40$ hours, or equivalently, its rotation speed is $\lesssim 42\%$ of the breakup speed. Alternatively, if the apparently low density of Kepler-51d is due to an opaque planetary ring, the ring must be oriented within $30°$ of face-on and have an inner radius smaller than $1.2$ times the planet's radius. Separately, the lack of anomalies exceeding $0.01\%$ in the ingress and egress portions of the light curve places a constraint on the model of Wang & Dai, in which the planet's apparently low density is due to a dusty outflowing atmosphere. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2409_06697 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Slow Rotation for the Super-Puff Planet Kepler-51d Lammers, Caleb Winn, Joshua N. Earth and Planetary Astrophysics Super-puffs are low-density planets of unknown origin and composition. If they form by accreting nebular gas through a circumplanetary disk, one might expect super-puffs to be spinning quickly. Here, we derive upper limits on the rotational oblateness of the super-puff Kepler-51d, based on precise transit observations with the NIRSpec instrument aboard the James Webb Space Telescope. The absence of detectable oblateness-related anomalies in the light curve leads to an upper limit of about $0.15$ on the planet's sky-projected oblateness. Assuming the sky-projected oblateness to be representative of the true oblateness, the rotation period of Kepler-51d is $\gtrsim 40$ hours, or equivalently, its rotation speed is $\lesssim 42\%$ of the breakup speed. Alternatively, if the apparently low density of Kepler-51d is due to an opaque planetary ring, the ring must be oriented within $30°$ of face-on and have an inner radius smaller than $1.2$ times the planet's radius. Separately, the lack of anomalies exceeding $0.01\%$ in the ingress and egress portions of the light curve places a constraint on the model of Wang & Dai, in which the planet's apparently low density is due to a dusty outflowing atmosphere. |
| title | Slow Rotation for the Super-Puff Planet Kepler-51d |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2409.06697 |