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Chen DC, Xie JW, Zhou JL, Dong S, Yang JY, Zhu W, Liu C, Huang Y, Xiang MS, Wang HF, Zheng Z, Luo AL, Zhang JH, Zhu Z. The evolution of hot Jupiters revealed by the age distribution of their host stars. Proc Natl Acad Sci U S A 2023; 120:e2304179120. [PMID: 37903265 PMCID: PMC10636359 DOI: 10.1073/pnas.2304179120] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/15/2023] [Accepted: 08/15/2023] [Indexed: 11/01/2023] Open
Abstract
The unexpected discovery of hot Jupiters challenged the classical theory of planet formation inspired by our solar system. Until now, the origin and evolution of hot Jupiters are still uncertain. Determining their age distribution and temporal evolution can provide more clues into the mechanism of their formation and subsequent evolution. Using a sample of 383 giant planets around Sun-like stars collected from the kinematic catalogs of the Planets Across Space and Time project, we find that hot Jupiters are preferentially hosted by relatively younger stars in the Galactic thin disk. We subsequently find that the frequency of hot Jupiters declines with age as [Formula: see text]. In contrast, the frequency of warm/cold Jupiters shows no significant dependence on age. Such a trend is expected from the tidal evolution of hot Jupiters' orbits, and our result offers supporting evidence using a large sample. We also perform a joint analysis on the planet frequencies in the stellar age-metallicity plane. The result suggests that the frequencies of hot Jupiters and warm/cold Jupiters, after removing the age dependence are both correlated with stellar metallicities as [Formula: see text] and [Formula: see text], respectively. Moreover, we show that the above correlations can explain the bulk of the discrepancy in hot Jupiter frequencies inferred from the transit and radial velocity (RV) surveys, given that RV targets tend to be more metal-rich and younger than transits.
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Affiliation(s)
- Di-Chang Chen
- School of Astronomy and Space Science, Nanjing University, Nanjing210023, China
- Key Laboratory of Modern Astronomy and Astrophysics, Ministry of Education, Nanjing210023, China
- LAMOST Fellow
| | - Ji-Wei Xie
- School of Astronomy and Space Science, Nanjing University, Nanjing210023, China
- Key Laboratory of Modern Astronomy and Astrophysics, Ministry of Education, Nanjing210023, China
| | - Ji-Lin Zhou
- School of Astronomy and Space Science, Nanjing University, Nanjing210023, China
- Key Laboratory of Modern Astronomy and Astrophysics, Ministry of Education, Nanjing210023, China
| | - Subo Dong
- Department of Astronomy, School of Physics, Peking University, Beijing100871, China
- Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing100871, China
| | - Jia-Yi Yang
- School of Astronomy and Space Science, Nanjing University, Nanjing210023, China
- Key Laboratory of Modern Astronomy and Astrophysics, Ministry of Education, Nanjing210023, China
| | - Wei Zhu
- Department of Astronomy, Tsinghua University, Beijing100084, China
| | - Chao Liu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing100012, China
| | - Yang Huang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing100012, China
- University of Chinese Academy of Sciences, Beijing100049, China
| | - Mao-Sheng Xiang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing100012, China
| | | | - Zheng Zheng
- Department of Physics and Astronomy, University of Utah, Salt Lake City, UT84112
| | - A-Li Luo
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing100012, China
| | - Jing-Hua Zhang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing100012, China
| | - Zi Zhu
- School of Astronomy and Space Science, Nanjing University, Nanjing210023, China
- Key Laboratory of Modern Astronomy and Astrophysics, Ministry of Education, Nanjing210023, China
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Gratton R, Mesa D, Bonavita M, Zurlo A, Marino S, Kervella P, Desidera S, D'Orazi V, Rigliaco E. Jupiter-like planets might be common in a low-density environment. Nat Commun 2023; 14:6232. [PMID: 37848416 PMCID: PMC10582043 DOI: 10.1038/s41467-023-41665-0] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/17/2023] [Accepted: 09/06/2023] [Indexed: 10/19/2023] Open
Abstract
Radial velocity surveys suggest that the Solar System may be unusual and that Jupiter-like planets have a frequency < 20% around solar-type stars. However, they may be much more common in one of the closest associations in the solar neighbourhood. Young moving stellar groups are the best targets for direct imaging of exoplanets and four massive Jupiter-like planets have been already discovered in the nearby young β Pic Moving Group (BPMG) via high-contrast imaging, and four others were suggested via high precision astrometry by the European Space Agency's Gaia satellite. Here we analyze 30 stars in BPMG and show that 20 of them might potentially host a Jupiter-like planet as their orbits would be stable. Considering incompleteness in observations, our results suggest that Jupiter-like planets may be more common than previously found. The next Gaia data release will likely confirm our prediction.
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Affiliation(s)
- Raffaele Gratton
- INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, I-35122, Italy.
| | - Dino Mesa
- INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, I-35122, Italy
| | - Mariangela Bonavita
- INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, I-35122, Italy
- School of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
| | - Alice Zurlo
- Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejército 441, Santiago, Chile
- Escuela de Ingeniería Industrial, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejército 441, Santiago, Chile
- Millennium Nucleus on Young Exoplanets and their Moons (YEMS), Santiago, Chile
| | - Sebastian Marino
- Department of Physics and Astronomy, University of Exeter, Stocker Road, Exeter, EX4 4QL, UK
| | - Pierre Kervella
- LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris Cité, 5 place Jules Janssen, 92195, Meudon, France
| | - Silvano Desidera
- INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, I-35122, Italy
| | - Valentina D'Orazi
- INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, I-35122, Italy
- Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica 1, 00133, Roma, Italy
| | - Elisabetta Rigliaco
- INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, I-35122, Italy
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Emsenhuber A, Mordasini C, Burn R. Planetary population synthesis and the emergence of four classes of planetary system architectures. EUROPEAN PHYSICAL JOURNAL PLUS 2023; 138:181. [PMID: 36874528 PMCID: PMC9971156 DOI: 10.1140/epjp/s13360-023-03784-x] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 07/18/2022] [Accepted: 02/09/2023] [Indexed: 06/18/2023]
Abstract
Planetary population synthesis is a helpful tool to understand the physics of planetary system formation. It builds on a global model, meaning that the model has to include a multitude of physical processes. The outcome can be statistically compared with exoplanet observations. Here, we review the population synthesis method and then use one population computed using the Generation III Bern model to explore how different planetary system architectures emerge and which conditions lead to their formation. The emerging systems can be classified into four main architectures: Class I of near in situ compositionally ordered terrestrial and ice planets, Class II of migrated sub-Neptunes, Class III of mixed low-mass and giant planets, broadly similar to the Solar System, and Class IV of dynamically active giants without inner low-mass planets. These four classes exhibit distinct typical formation pathways and are characterised by certain mass scales. We find that Class I forms from the local accretion of planetesimals followed by a giant impact phase, and the final planet masses correspond to what is expected from such a scenario, the 'Goldreich mass'. Class II, the migrated sub-Neptune systems form when planets reach the 'equality mass' where accretion and migration timescales are comparable before the dispersal of the gas disc, but not large enough to allow for rapid gas accretion. Giant planets form when the 'equality mass' allows for gas accretion to proceed while the planet is migrating, i.e. when the critical core mass is reached. The main discriminant of the four classes is the initial mass of solids in the disc, with contributions from the lifetime and mass of the gas disc. The distinction between mixed Class III systems and Class IV dynamically active giants is in part due to the stochastic nature of dynamical interactions, such as scatterings between giant planets, rather than the initial conditions only. The breakdown of system into classes allows to better interpret the outcome of a complex model and understand which physical processes are dominant. Comparison with observations reveals differences to the actual population, pointing at limitation of theoretical understanding. For example, the overrepresentation of synthetic super-Earths and sub-Neptunes in Class I systems causes these planets to be found at lower metallicities than in observations.
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Affiliation(s)
- Alexandre Emsenhuber
- Universitäts-Sternwarte, Ludwig-Maximilians-Universität München, Scheinerstraße 1, 81679 Munich, Germany
- Space Research and Planetary Sciences, Universität Bern, Gesellschaftsstrasse 6, 3012 Bern, Switzerland
- Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721 USA
| | - Christoph Mordasini
- Space Research and Planetary Sciences, Universität Bern, Gesellschaftsstrasse 6, 3012 Bern, Switzerland
| | - Remo Burn
- Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
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Cvetojevic N, Norris BRM, Gross S, Jovanovic N, Arriola A, Lacour S, Kotani T, Lawrence JS, Withford MJ, Tuthill P. Building hybridized 28-baseline pupil-remapping photonic interferometers for future high-resolution imaging. APPLIED OPTICS 2021; 60:D33-D42. [PMID: 34263826 DOI: 10.1364/ao.422729] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/15/2021] [Accepted: 04/17/2021] [Indexed: 06/13/2023]
Abstract
One key advantage of single-mode photonic technologies for interferometric use is their ability to easily scale to an ever-increasing number of inputs without a major increase in the overall device size, compared to traditional bulk optics. This is particularly important for the upcoming extremely large telescope (ELT) generation of telescopes currently under construction. We demonstrate the fabrication and characterization of a hybridized photonic interferometer, with eight simultaneous inputs, forming 28 baselines, which is the largest amount to date, to the best of our knowledge. Using different photonic fabrication technologies, we combine a 3D pupil remapper with a planar eight-port ABCD pairwise beam combiner, along with the injection optics necessary for telescope use, into a single integrated monolithic device. We successfully realized a combined device called Dragonfly, which demonstrates a raw instrumental closure-phase stability down to 0.9° over $8\pi$ phase piston error, relating to a detection contrast of ${\sim}6.5 \times {10^{- 4}}$ on an adaptive-optics-corrected 8 m telescope. This prototype successfully demonstrates advanced hybridization and packaging techniques necessary for on-sky use for high-contrast detection at small inner working angles, ideally complementing what can currently be achieved using coronagraphs.
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The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-3881/ab16e9] [Citation(s) in RCA: 178] [Impact Index Per Article: 35.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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