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

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 it has been unclear if they also result from different planet formation processes, and if there is 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 ≃ 2.5 d, R p ≃ 1.22 R J , M p = 0.72 M J ) and TOI-2981 b ( P ≃ 3.6 d, R P ≃ 1.2 R J , M P = 2 M J ) are hot Jupiters on nearly circular orbits, while TOI-4914 b ( P ≃ 10.6 d, R P ≃ 1.15 R J , M p = 0.72 M J ) is a warm Jupiter with a significant eccentricity ( e = 0.41 ± 0.02) that orbits a star more metal-poor ([Fe/H] = −0.13) than most of the stars known to host giant planets. Similarly, TOI-2981 b orbits a metal-poor star ([Fe/H] = −0.11), while TOI-2714 b orbits a metal-rich star ([Fe/H] = 0.30). Our radial velocity 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 ( R p ≃ 1.15 R J ) and low insolation flux ( F ⋆ < 2 × 108 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.

Authors

Institutions

Publication Details

Journal
Astronomy and Astrophysics
Published
2024-09-20
DOI
https://doi.org/10.1051/0004-6361/202451841
Citations
2
Primary Topic
Astro and Planetary Science
Type
article
Field-Weighted Citation Impact
0.66

Funders

Controls
|||
ALL TIME
JAN
FEB
MAR
APR
MAY
JUN
JUL
AUG
SEP
OCT
article

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

Thiam-Guan Tan, F. Z. Majidi, A. Collier Cameron, Andrew W. Mann et al.
2 citations
Astronomy and Astrophysics
Astro and Planetary Science
0.66
article

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

Thiam-Guan Tan, F. Z. Majidi, A. Collier Cameron, Andrew W. Mann, D. J. Radford, S. Desidera, L. Borsato, D. W. Latham, F. J. Pozuelos, V. Nascimbeni, K. Barkaoui, F. Marzari, G. Piotto, T. Zingales, S. Seager, K. Biazzo, G. Mantovan, Michael Fausnaugh, J. M. Jenkins, L. Malavolta, P. Rowden, V. Granata, M. Timmermans, K. A. Collins, A. Bieryla, D. Nardiello, V. Kostov, T. G. Wilson, J. N. Winn, P. A. Evans, M. Montalto, L. Mignon, Cristilyn N. Watkins, K. G. Stassun, H. M. Relles
article en
2 citations

Abstract

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 it has been unclear if they also result from different planet formation processes, and if there is 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 ≃ 2.5 d, R p ≃ 1.22 R J , M p = 0.72 M J ) and TOI-2981 b ( P ≃ 3.6 d, R P ≃ 1.2 R J , M P = 2 M J ) are hot Jupiters on nearly circular orbits, while TOI-4914 b ( P ≃ 10.6 d, R P ≃ 1.15 R J , M p = 0.72 M J ) is a warm Jupiter with a significant eccentricity ( e = 0.41 ± 0.02) that orbits a star more metal-poor ([Fe/H] = −0.13) than most of the stars known to host giant planets. Similarly, TOI-2981 b orbits a metal-poor star ([Fe/H] = −0.11), while TOI-2714 b orbits a metal-rich star ([Fe/H] = 0.30). Our radial velocity 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 ( R p ≃ 1.15 R J ) and low insolation flux ( F ⋆ < 2 × 108 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.

Astronomy and AstrophysicsVol. 691
University of North Carolina at Chapel Hill (US), University of Geneva (CH), Texas Tech University (US), Ames Research Center (US), Royal Astronomical Society (GB), Centre National de la Recherche Scientifique (FR), Planetary Science Institute (US), Goddard Space Flight Center (US), University of Padua (IT), University of Liège (BE), University of St Andrews (GB), American Association of Variable Star Observers (US), Vanderbilt University (US), Princeton University (US), Astronomical Observatory of Rome (IT), University of Warwick (GB), Blue Sky Research (United States) (US), Perth Exoplanet Survey Telescope Observatory (AU), Osservatorio Astrofisico di Catania (IT), Center for Astrophysics Harvard & Smithsonian (US), Instituto de Astrofísica de Canarias (ES), Instituto de Astrofísica de Andalucía (ES), Osservatorio Astronomico di Padova (IT), American Institute of Aeronautics and Astronautics (US), Massachusetts Institute of Technology (US), Search for Extraterrestrial Intelligence (US), National Institute for Astrophysics (IT), Université Grenoble Alpes (FR)
National Science Foundation, National Aeronautics and Space Administration, Michigan State University, UK Space Agency, Space Telescope Science Institute, University of Warwick, Fonds De La Recherche Scientifique - FNRS, Fédération Wallonie-Bruxelles, Ministério da Ciência, Tecnologia e Inovação, Agenzia Spaziale Italiana, Ministerio de Ciencia e Innovación, Ames Research Center, College of Engineering, Michigan State University, University of North Carolina at Chapel Hill, Science Mission Directorate, Science and Technology Facilities Council, Fonds pour la Formation à la Recherche dans l’Industrie et dans l’Agriculture, Agencia Estatal de Investigación
Openalex Percentile: Top 28%
Astro and Planetary Science
0.66
DOIOpen Access PDFOpenAlex
AI Navigator

Ask Laika to Summarize, Analyze, and Connect papers live on the map.

Summarize Papers & Methodologies

Extract key findings, datasets, and comparative methods across publications.

Benchmark Rankings & Visual Analytics

Rank top research institutions, authors, funders, topics, and journals by Field-Weighted Citation Impact (FWCI) and paper volume with instant charts.

Connect Distant Disciplines

Bridge topological clusters on the map to find hidden collaborative intersections.