Using JWST transits and occultations to determine $\sim1\%$ stellar radii and temperatures of low-mass stars
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| Format: | Preprint |
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2024
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| author | Mahajan, Alexandra S. Eastman, Jason D. Kirk, James |
| author_facet | Mahajan, Alexandra S. Eastman, Jason D. Kirk, James |
| contents | Using JWST observations of a primary transit and two secondary eclipses for GJ 1214b, we determine an eccentricity that is more precise than a decade of HARPS data, which enables us to measure the stellar density to 2.62%. Coupled with a prior on the stellar mass from a dynamically calibrated K-$M_*$ relation, we determine $R_*$ to 1.13% -- 3 times more precise than any other published analysis of this system. Then, using the bolometric flux from an spectral energy distribution model, we determine $T_{\rm eff}$ to 1.39% -- 40% more precise than systematic floors from spectroscopy. Within the global model, these also improve the planetary radius and insolation. This is a proof of concept for a new method to determine accurate $R_*$ and $T_{\rm eff}$ to a precision currently achieved for only a small number of low-mass stars. By applying our method to all high signal-to-noise ratio planetary transits and occultations, we can expand the sample of precisely measured stars without assuming tidal circularization and calibrate new relations to improve our understanding of all low-mass stars. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2402_05991 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Using JWST transits and occultations to determine $\sim1\%$ stellar radii and temperatures of low-mass stars Mahajan, Alexandra S. Eastman, Jason D. Kirk, James Solar and Stellar Astrophysics Earth and Planetary Astrophysics Using JWST observations of a primary transit and two secondary eclipses for GJ 1214b, we determine an eccentricity that is more precise than a decade of HARPS data, which enables us to measure the stellar density to 2.62%. Coupled with a prior on the stellar mass from a dynamically calibrated K-$M_*$ relation, we determine $R_*$ to 1.13% -- 3 times more precise than any other published analysis of this system. Then, using the bolometric flux from an spectral energy distribution model, we determine $T_{\rm eff}$ to 1.39% -- 40% more precise than systematic floors from spectroscopy. Within the global model, these also improve the planetary radius and insolation. This is a proof of concept for a new method to determine accurate $R_*$ and $T_{\rm eff}$ to a precision currently achieved for only a small number of low-mass stars. By applying our method to all high signal-to-noise ratio planetary transits and occultations, we can expand the sample of precisely measured stars without assuming tidal circularization and calibrate new relations to improve our understanding of all low-mass stars. |
| title | Using JWST transits and occultations to determine $\sim1\%$ stellar radii and temperatures of low-mass stars |
| topic | Solar and Stellar Astrophysics Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2402.05991 |