The inflated, eccentric warm Jupiter TOI-4914 b orbiting a metal-poor star, and the hot Jupiters TOI-2714 b and TOI-2981 b

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Main Authors:	Mantovan, G., Wilson, T. G., Borsato, L., Zingales, T., Biazzo, K., Nardiello, D., Malavolta, L., Desidera, S., Marzari, F., Cameron, A. Collier, Nascimbeni, V., Majidi, F. Z., Montalto, M., Piotto, G., Stassun, K. G., Winn, J. N., Jenkins, J. M., Mignon, L., Bieryla, A., Latham, D. W., Barkaoui, K., Collins, K. A., Evans, P., Fausnaugh, M. M., Granata, V., Kostov, V., Mann, A. W., Pozuelos, F. J., Radford, D. J., Relles, H. M., Rowden, P., Seager, S., Tan, T. -G., Timmermans, M., Watkins, C. N.
Format:	Preprint
Published:	2024
Subjects:	Earth and Planetary Astrophysics Solar and Stellar Astrophysics
Online Access:	Acceder al recurso
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author	Mantovan, G. Wilson, T. G. Borsato, L. Zingales, T. Biazzo, K. Nardiello, D. Malavolta, L. Desidera, S. Marzari, F. Cameron, A. Collier Nascimbeni, V. Majidi, F. Z. Montalto, M. Piotto, G. Stassun, K. G. Winn, J. N. Jenkins, J. M. Mignon, L. Bieryla, A. Latham, D. W. Barkaoui, K. Collins, K. A. Evans, P. Fausnaugh, M. M. Granata, V. Kostov, V. Mann, A. W. Pozuelos, F. J. Radford, D. J. Relles, H. M. Rowden, P. Seager, S. Tan, T. -G. Timmermans, M. Watkins, C. N.
author_facet	Mantovan, G. Wilson, T. G. Borsato, L. Zingales, T. Biazzo, K. Nardiello, D. Malavolta, L. Desidera, S. Marzari, F. Cameron, A. Collier Nascimbeni, V. Majidi, F. Z. Montalto, M. Piotto, G. Stassun, K. G. Winn, J. N. Jenkins, J. M. Mignon, L. Bieryla, A. Latham, D. W. Barkaoui, K. Collins, K. A. Evans, P. Fausnaugh, M. M. Granata, V. Kostov, V. Mann, A. W. Pozuelos, F. J. Radford, D. J. Relles, H. M. Rowden, P. Seager, S. Tan, T. -G. Timmermans, M. Watkins, C. N.
contents	Recent observations of giant planets have revealed unexpected bulk densities. Hot Jupiters, in particular, appear larger than expected for their masses compared to planetary evolution models, while warm Jupiters seem denser than expected. These differences are often attributed to the influence of the stellar incident flux, but could they also result from different planet formation processes? Is there a trend linking the planetary density to the chemical composition of the host star? In this work we present the confirmation of three giant planets in orbit around solar analogue stars. TOI-2714 b ($P \simeq 2.5$ d, $R_{\rm p} \simeq 1.22 R_{\rm J}$, $M_{\rm p} = 0.72 M_{\rm J}$) and TOI-2981 b ($P \simeq 3.6$ d, $R_{\rm p} \simeq 1.2 R_{\rm J}$, $M_{\rm p} = 2 M_{\rm J}$) are hot Jupiters on nearly circular orbits, while TOI-4914 b ($P \simeq 10.6$ d, $R_{\rm p} \simeq 1.15 R_{\rm J}$, $M_{\rm p} = 0.72 M_{\rm J}$) is a warm Jupiter with a significant eccentricity ($e = 0.41 \pm 0.02$) that orbits a star more metal-poor ([Fe/H]$~= -0.13$) than most of the stars known to host giant planets. Our radial velocity (RV) follow-up with the HARPS spectrograph allows us to detect their Keplerian signals at high significance (7, 30, and 23$σ$, respectively) and to place a strong constraint on the eccentricity of TOI-4914 b (18$σ$). TOI-4914 b, with its large radius and low insolation flux ($F_\star < 2 \times 10^8~{\rm erg~s^{-1}~cm^{-2}}$), appears to be more inflated than what is supported by current theoretical models for giant planets. Moreover, it does not conform to the previously noted trend that warm giant planets orbiting metal-poor stars have low eccentricities. This study thus provides insights into the diverse orbital characteristics and formation processes of giant exoplanets, in particular the role of stellar metallicity in the evolution of planetary systems.
format	Preprint
id	arxiv_https___arxiv_org_abs_2409_07520
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	The inflated, eccentric warm Jupiter TOI-4914 b orbiting a metal-poor star, and the hot Jupiters TOI-2714 b and TOI-2981 b Mantovan, G. Wilson, T. G. Borsato, L. Zingales, T. Biazzo, K. Nardiello, D. Malavolta, L. Desidera, S. Marzari, F. Cameron, A. Collier Nascimbeni, V. Majidi, F. Z. Montalto, M. Piotto, G. Stassun, K. G. Winn, J. N. Jenkins, J. M. Mignon, L. Bieryla, A. Latham, D. W. Barkaoui, K. Collins, K. A. Evans, P. Fausnaugh, M. M. Granata, V. Kostov, V. Mann, A. W. Pozuelos, F. J. Radford, D. J. Relles, H. M. Rowden, P. Seager, S. Tan, T. -G. Timmermans, M. Watkins, C. N. Earth and Planetary Astrophysics Solar and Stellar Astrophysics Recent observations of giant planets have revealed unexpected bulk densities. Hot Jupiters, in particular, appear larger than expected for their masses compared to planetary evolution models, while warm Jupiters seem denser than expected. These differences are often attributed to the influence of the stellar incident flux, but could they also result from different planet formation processes? Is there a trend linking the planetary density to the chemical composition of the host star? In this work we present the confirmation of three giant planets in orbit around solar analogue stars. TOI-2714 b ($P \simeq 2.5$ d, $R_{\rm p} \simeq 1.22 R_{\rm J}$, $M_{\rm p} = 0.72 M_{\rm J}$) and TOI-2981 b ($P \simeq 3.6$ d, $R_{\rm p} \simeq 1.2 R_{\rm J}$, $M_{\rm p} = 2 M_{\rm J}$) are hot Jupiters on nearly circular orbits, while TOI-4914 b ($P \simeq 10.6$ d, $R_{\rm p} \simeq 1.15 R_{\rm J}$, $M_{\rm p} = 0.72 M_{\rm J}$) is a warm Jupiter with a significant eccentricity ($e = 0.41 \pm 0.02$) that orbits a star more metal-poor ([Fe/H]$~= -0.13$) than most of the stars known to host giant planets. Our radial velocity (RV) follow-up with the HARPS spectrograph allows us to detect their Keplerian signals at high significance (7, 30, and 23$σ$, respectively) and to place a strong constraint on the eccentricity of TOI-4914 b (18$σ$). TOI-4914 b, with its large radius and low insolation flux ($F_\star < 2 \times 10^8~{\rm erg~s^{-1}~cm^{-2}}$), appears to be more inflated than what is supported by current theoretical models for giant planets. Moreover, it does not conform to the previously noted trend that warm giant planets orbiting metal-poor stars have low eccentricities. This study thus provides insights into the diverse orbital characteristics and formation processes of giant exoplanets, in particular the role of stellar metallicity in the evolution of planetary systems.
title	The inflated, eccentric warm Jupiter TOI-4914 b orbiting a metal-poor star, and the hot Jupiters TOI-2714 b and TOI-2981 b
topic	Earth and Planetary Astrophysics Solar and Stellar Astrophysics
url	https://arxiv.org/abs/2409.07520