TOI-2458 b: A mini-Neptune consistent with in situ hot Jupiter formation
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| Title: | TOI-2458 b: A mini-Neptune consistent with in situ hot Jupiter formation |
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| Authors: | Šubjak, J., Gandolfi, D., Goffo, E., Rapetti, D., Jankowski, Dawid, Mizuki, Toshiyuki, Dai, Fei, Serrano, L. M., Wilson, T.G., Goåºdziewski, Krzysztof, Nowak, G., Jenkins, Jon M., Twicken, J. D., Winn, J. N., Bieryla, Allyson, Ciardi, D. R., Cochran, William, Collins, Karen A., Deeg, H., García, R. A., Guenther, E. W., Hatzes, A., Kabath, Petr, Korth, Judith, 1987, Latham, D. W., Livingston, J.H., Lund, M. B., Mathur, S., Narita, Norio, Orell-Miquel, J., Palle, Enric, Persson, Carina, 1964, Redfield, S., Schwarz, R., Watanabe, David, Ziegler, C. |
| Source: | Exoplaneter från rymden - CHEOPS och PLATO, ESA's nästa två rymdteleskop (fas 2) Astronomy and Astrophysics TOI-2458 b: A mini-Neptune consistent with in situ hot Jupiter formation (Additional material). 693 |
| Subject Terms: | Planets and satellites: dynamical evolution and stability, Techniques: spectroscopic, Techniques: photometric, Planetary systems, Planets and satellites: formation, Techniques: radial velocities |
| Description: | We report on the discovery and spectroscopic confirmation of TOI-2458 b, a transiting mini-Neptune around an F-type star leaving the main-sequence with a mass of M∗ = 1.05 ± 0.03 M⊙, a radius of R∗ = 1.31 ± 0.03 R⊙, an effective temperature of Teff = 6005 ± 50 K, and a metallicity of 0.10 ± 0.05 dex. By combining TESS photometry with high-resolution spectra acquired with the HARPS spectrograph, we found that the transiting planet has an orbital period of 3.74 days, a mass of Mp = 13.31 ± 0.99 M⊕ and a radius of Rp = 2.83 ± 0.20 R⊕. The host star TOI-2458 shows a short activity cycle of ∼54 days revealed in the HARPS S-index and Ha times series. We took the opportunity to investigate other F stars showing activity cycle periods comparable to that of TOI-2458 and found that they have shorter rotation periods than would be expected based on the gyrochronology predictions. In addition, we determined TOI-2458's stellar inclination angle to be i∗ = 10.610.6+13.3 degrees. We discuss that both phenomena (fast stellar rotation and planet orbit inclination) could be explained by in situ formation of a hot Jupiter interior to TOI-2458 b. It is plausible that this hot Jupiter was recently engulfed by the star. Analysis of HARPS spectra has identified the presence of another planet with a period of P = 16.55 ± 0.06 days and a minimum mass of Mp sin i = 10.22 ± 1.90 M⊕. Using dynamical stability analysis, we constrained the mass of this planet to the range Mc ≃ (10, 25) M⊕ |
| File Description: | electronic |
| Access URL: | https://research.chalmers.se/publication/545027 https://research.chalmers.se/publication/545027/file/545027_Fulltext.pdf |
| Database: | SwePub |
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Nájsť tento článok vo Web of Science | Abstract: | We report on the discovery and spectroscopic confirmation of TOI-2458 b, a transiting mini-Neptune around an F-type star leaving the main-sequence with a mass of M∗ = 1.05 ± 0.03 M⊙, a radius of R∗ = 1.31 ± 0.03 R⊙, an effective temperature of Teff = 6005 ± 50 K, and a metallicity of 0.10 ± 0.05 dex. By combining TESS photometry with high-resolution spectra acquired with the HARPS spectrograph, we found that the transiting planet has an orbital period of 3.74 days, a mass of Mp = 13.31 ± 0.99 M⊕ and a radius of Rp = 2.83 ± 0.20 R⊕. The host star TOI-2458 shows a short activity cycle of ∼54 days revealed in the HARPS S-index and Ha times series. We took the opportunity to investigate other F stars showing activity cycle periods comparable to that of TOI-2458 and found that they have shorter rotation periods than would be expected based on the gyrochronology predictions. In addition, we determined TOI-2458's stellar inclination angle to be i∗ = 10.610.6+13.3 degrees. We discuss that both phenomena (fast stellar rotation and planet orbit inclination) could be explained by in situ formation of a hot Jupiter interior to TOI-2458 b. It is plausible that this hot Jupiter was recently engulfed by the star. Analysis of HARPS spectra has identified the presence of another planet with a period of P = 16.55 ± 0.06 days and a minimum mass of Mp sin i = 10.22 ± 1.90 M⊕. Using dynamical stability analysis, we constrained the mass of this planet to the range Mc ≃ (10, 25) M⊕ |
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| ISSN: | 00046361 14320746 |
| DOI: | 10.1051/0004-6361/202451057 |