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

被引：0

作者：

Mantovan, G. ^{[1
,2
]}

Wilson, T. G. ^{[3
]}

Borsato, L. ^{[2
]}

Zingales, T. ^{[1
,2
]}

Biazzo, K. ^{[4
]}

Nardiello, D. ^{[1
,2
]}

Malavolta, L. ^{[1
,2
]}

Desidera, S. ^{[2
]}

Marzari, F. ^{[1
]}

Collier Cameron, A. ^{[5
]}

Nascimbeni, V. ^{[2
]}

Majidi, F. Z. ^{[6
]}

Montalto, M. ^{[7
]}

Piotto, G. ^{[1
]}

Stassun, K. G. ^{[8
]}

Winn, J. N. ^{[9
]}

Jenkins, J. M. ^{[10
]}

Mignon, L. ^{[11
,12
]}

Bieryla, A. ^{[13
]}

Latham, D. W. ^{[13
]}

Barkaoui, K. ^{[14
,15
,16
]}

Collins, K. A. ^{[13
]}

Evans, P. ^{[17
]}

Fausnaugh, M. M. ^{[18
]}

Granata, V. ^{[2
,19
,20
]}

Kostov, V. ^{[21
,22
]}

Mann, A. W. ^{[23
]}

Pozuelos, F. J. ^{[24
]}

Radford, D. J. ^{[25
]}

Relles, H. M. ^{[13
]}

Rowden, P. ^{[26
]}

Seager, S. ^{[15
,27
,28
]}

Tan, T. -g. ^{[29
]}

Timmermans, M. ^{[14
]}

Watkins, C. N. ^{[13
]}

机构：

[1] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy

[2] Ist Nazl Astrofis, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[3] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, England

[4] INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Roma, Italy

[5] Univ St Andrews, Ctr Exoplanet Sci, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Scotland

[6] Blue Skies Space SRL, Milan, Italy

[7] INAF Osservatorio Astrofisico Catania, Via S Sofia 78, I-95123 Catania, Italy

[8] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA

[9] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

[10] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

[11] Univ Geneva, Dept Astron, Chemin Pegasi 51, CH-1290 Versoix, Switzerland

[12] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France

[13] Ctr Astrophys Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138 USA

[14] Univ Liege, Astrobiol Res Unit, 19C Allee 6 Aout, B-4000 Liege, Belgium

[15] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[16] Inst Astrofis Canarias IAC, Tenerife 38205, Spain

[17] El Sauce Observ, Coquimbo, Coquimbo Provin, Chile

[18] Texas Tech Univ, Dept Phys & Astron, Lubbock, TX 79409 USA

[19] Univ Padua, Ctr Ateneo Studi & Att Spaziali Giuseppe Colombo C, Via Venezia 15, I-35131 Padua, Italy

[20] Univ Studi Padova, INFN Sez Padova, Via Marzolo 8, I-35131 Padua, Italy

[21] NASA Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA

[22] SETI Inst, 189 N Bernardo Ave Suite 200, Mountain View, CA 94043 USA

[23] Univ North Carolina Chapel Hill, Dept Phys & Astron, Chapel Hill, NC 27599 USA

[24] Inst Astrofis Andalucia IAA CSIC, Glorieta Astron s n, Granada 18008, Spain

[25] Amer Assoc Variable Star Observers, 49 Bay State Rd, Cambridge, MA 02138 USA

[26] Royal Astron Soc, Burlington House, London W1J 0BQ, England

[27] MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA

[28] MIT, Dept Aeronaut & Astronaut, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[29] Perth Exoplanet Survey Telescope, Perth, WA, Australia

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 691卷

关键词：

techniques: photometric; techniques: radial velocities; planets and satellites: fundamental parameters; planets and satellites: gaseous planets; stars: fundamental parameters; MOLECULAR LINE LISTS; GIANT PLANETS; EXTRASOLAR PLANETS; RADIAL-VELOCITIES; SUPER-EARTH; HARPS-N; SPECKLE INTERFEROMETRY; ERROR-CORRECTION; I-ARCHITECTURE; GAPS PROGRAM;

D O I：

10.1051/0004-6361/202451841

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 similar or equal to 2.5 d, R-p similar or equal to 1.22 RJ, M-p=0.72 M-J) and TOI-2981 b (P similar or equal to 3.6 d, R-P similar or equal to 1.2 R-J, M-P=2M(J)) are hot Jupiters on nearly circular orbits, while TOI-4914 b (P similar or equal to 10.6 d, R-P similar or equal to 1.15 R-J,M-p = 0.72 MJ) 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 sigma, respectively) and to place a strong constraint on the eccentricity of TOI-4914 b (18 sigma). TOI-4914 b, with its large radius (R-p similar or equal to 1.15 R-J) and low insolation flux (F star < 2 x 10(8 )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.

引用

页数：20

共 23 条

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Alves, Douglas R.
Jenkins, James S.
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MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2025, 536 (03) : 3137 - 3137
[22] The GAPS programme at TNG LVII. TOI-5076b: A warm sub-Neptune planet orbiting a thin-to-thick-disk transition star in a wide binary system
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ASTRONOMY & ASTROPHYSICS, 2024, 687
[23] Correction : NGTS-21b: an inflated Super-Jupiter orbiting a metal-poor K dwarf(Monthly Notices of the Royal Astronomical Society(2022) 517:3 (4447–4457) DOI:10.1093/mnras/stac2884)
Mon. Not. R. Astron. Soc., 3 (3137):

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