Seismic Oscillations Excited by Giant Impacts in Directly-Imaged Giant Planets
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arXiv
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| Autores principales: | , , |
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| Formato: | Preprint |
| Publicado: |
2025
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| _version_ | 1866916941438910464 |
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| author | Zanazzi, J. J. Chiang, Eugene Zhou, Yifan |
| author_facet | Zanazzi, J. J. Chiang, Eugene Zhou, Yifan |
| contents | The radii and masses of many giant exoplanets imply their interiors each contain more than $\sim$100 $M_\oplus$ of solids. A large metal content may arise when a giant planet grows by colliding and merging with multiple $\sim$10 $M_\oplus$ solid cores. Here we show that a giant impact with a young gas giant excites long-lived seismic oscillations that can be detected photometrically. Mode lifetimes are close to the planet's Kelvin-Helmholtz time, a significant fraction of a young planet's age. Oscillation periods lie between tens of minutes to an hour, and variability amplitudes can exceed a percent for several million years. Beta Pictoris b is a young super-Jupiter known to be highly metal-enriched. If a Neptune-mass (17 $M_\oplus$) body impacted $β$ Pictoris b in the past $\sim$9--18 Myr, the planet could still be ringing with a percent-level photometric variability measurable with JWST. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2505_01496 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Seismic Oscillations Excited by Giant Impacts in Directly-Imaged Giant Planets Zanazzi, J. J. Chiang, Eugene Zhou, Yifan Earth and Planetary Astrophysics The radii and masses of many giant exoplanets imply their interiors each contain more than $\sim$100 $M_\oplus$ of solids. A large metal content may arise when a giant planet grows by colliding and merging with multiple $\sim$10 $M_\oplus$ solid cores. Here we show that a giant impact with a young gas giant excites long-lived seismic oscillations that can be detected photometrically. Mode lifetimes are close to the planet's Kelvin-Helmholtz time, a significant fraction of a young planet's age. Oscillation periods lie between tens of minutes to an hour, and variability amplitudes can exceed a percent for several million years. Beta Pictoris b is a young super-Jupiter known to be highly metal-enriched. If a Neptune-mass (17 $M_\oplus$) body impacted $β$ Pictoris b in the past $\sim$9--18 Myr, the planet could still be ringing with a percent-level photometric variability measurable with JWST. |
| title | Seismic Oscillations Excited by Giant Impacts in Directly-Imaged Giant Planets |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2505.01496 |