A second planet transiting LTT 1445A and a determination of the masses of both worlds
LTT 1445 is a hierarchical triple M-dwarf star system located at a distance of 6.86 pc. The primary star LTT 1445A (0.257 M ⊙) is known to host the transiting planet LTT 1445Ab with an orbital period of 5.36 days, making it the second-closest known transiting exoplanet system, and the closest one fo...
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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
2022 March 14
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| In: |
The astronomical journal
Year: 2022, Volume: 163, Issue: 4, Pages: 1-18 |
| ISSN: | 1538-3881 |
| DOI: | 10.3847/1538-3881/ac50a9 |
| Online Access: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.3847/1538-3881/ac50a9 |
| Author Notes: | Jennifer G. Winters, Julian Stürmer [und weitere Verfasser] |
MARC
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| 100 | 1 | |a Winters, Jennifer G. |e VerfasserIn |0 (DE-588)1255272171 |0 (DE-627)1799360342 |4 aut | |
| 245 | 1 | 2 | |a A second planet transiting LTT 1445A and a determination of the masses of both worlds |c Jennifer G. Winters, Julian Stürmer [und weitere Verfasser] |
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| 520 | |a LTT 1445 is a hierarchical triple M-dwarf star system located at a distance of 6.86 pc. The primary star LTT 1445A (0.257 M ⊙) is known to host the transiting planet LTT 1445Ab with an orbital period of 5.36 days, making it the second-closest known transiting exoplanet system, and the closest one for which the host is an M dwarf. Using Transiting Exoplanet Survey Satellite data, we present the discovery of a second planet in the LTT 1445 system, with an orbital period of 3.12 days. We combine radial-velocity measurements obtained from the five spectrographs, Echelle Spectrograph for Rocky Exoplanets and Stable Spectroscopic Observations, High Accuracy Radial Velocity Planet Searcher, High-Resolution Echelle Spectrometer, MAROON-X, and Planet Finder Spectrograph to establish that the new world also orbits LTT 1445A. We determine the mass and radius of LTT 1445Ab to be 2.87 ± 0.25 M ⊕ and R ⊕, consistent with an Earth-like composition. For the newly discovered LTT 1445Ac, we measure a mass of M ⊕ and a minimum radius of 1.15 R ⊕, but we cannot determine the radius directly as the signal-to-noise ratio of our light curve permits both grazing and nongrazing configurations. Using MEarth photometry and ground-based spectroscopy, we establish that star C (0.161 M ⊙) is likely the source of the 1.4 day rotation period, and star B (0.215 M ⊙) has a likely rotation period of 6.7 days. We estimate a probable rotation period of 85 days for LTT 1445A. Thus, this triple M-dwarf system appears to be in a special evolutionary stage where the most massive M dwarf has spun down, the intermediate mass M dwarf is in the process of spinning down, while the least massive stellar component has not yet begun to spin down. | ||
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| 700 | 1 | |a Terentev, Ivan A. |e VerfasserIn |4 aut | |
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