Interior and Evolution of the Giant Planets

Miguel, Yamila; Vazan, Allona

doi:10.3390/rs15030681

Cited by 11 publications

(5 citation statements)

References 170 publications

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“…We used the latter here merely to test our atmosphere calculations in light of previous work. In summary, these new boundary tables and atmospheres are meant to support the next generation of comprehensive giant planet models, which is already well underway (Nettelmann et al 2015;Mankovich et al 2016;Püstow et al 2016;Vazan et al 2016Vazan et al , 2018Mankovich & Fortney 2020;Miguel & Vazan 2023). Frontier Center, under Award PHY-2020249.…”

Section: Discussionmentioning

confidence: 99%

Jupiter Atmospheric Models and Outer Boundary Conditions for Giant Planet Evolutionary Calculations

Chen,

Burrows,

Sur

et al. 2023

ApJ

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We present updated atmospheric tables suitable for calculating the post-formation evolution and cooling of Jupiter and Jupiter-like exoplanets. These tables are generated using a 1D radiative transfer modeling code that incorporates the latest opacities and realistic prescriptions for stellar irradiation and ammonia clouds. To ensure the accuracy of our model parameters, we calibrate them against the measured temperature structure and geometric albedo spectrum of Jupiter, its effective temperature, and its inferred internal temperature. As a test case, we calculate the cooling history of Jupiter using an adiabatic and homogeneous interior and compare with extant models now used to evolve Jupiter and the giant planets. We find that our model reasonably matches Jupiter after evolving a hot-start initial condition to the present age of the solar system, with a discrepancy in brightness temperature/radius within 2%. Our algorithm allows us to customize for different cloud, irradiation, and metallicity parameters. This class of boundary conditions can be used to study the evolution of solar system giant planets and exoplanets with more complicated interior structures and nonadiabatic, inhomogeneous internal profiles.

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Section: Discussionmentioning

confidence: 99%

Jupiter Atmospheric Models and Outer Boundary Conditions for Giant Planet Evolutionary Calculations

Chen,

Burrows,

Sur

et al. 2023

ApJ

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“…In Figure 2 we compare the estimated heavy-element content (M Z ) for GEMS from planetary interior models (Thorngren et al 2016), with disk dust masses (M d ) and show that assuming an optimistic planet formation efficiency of 10% through pebble accretion (Liu et al 2019b) necessitates disks with many 100 s of M ⊕ of heavy elements. We note the caveat here that recent giant planet interior models tend to predict a lower heavy-element content when incorporating results from newer equations of state, results from the Solar-system gas giants, and atmospheric metallicity estimates (Müller & Helled 2021Miguel et al 2022;Miguel & Vazan 2023), which might alleviate some of this mass deficit. The second is the timescale of the formation of a solid massive core to initiate runaway gaseous…”

Section: Formation During Protoplanetary Phasementioning

confidence: 92%

Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation

Kanodia,

Cañas,

Mahadevan

et al. 2024

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Recent discoveries of transiting giant exoplanets around M-dwarf stars (GEMS), aided by the all-sky coverage of TESS, are starting to stretch theories of planet formation through the core-accretion scenario. Recent upper limits on their occurrence suggest that they decrease with lower stellar masses, with fewer GEMS around lower-mass stars compared to solar-type. In this paper, we discuss existing GEMS both through confirmed planets, as well as protoplanetary disk observations, and a combination of tests to reconcile these with theoretical predictions. We then introduce the Searching for GEMS survey, where we utilize multidimensional nonparameteric statistics to simulate hypothetical survey scenarios to predict the required sample size of transiting GEMS with mass measurements to robustly compare their bulk-density with canonical hot Jupiters orbiting FGK stars. Our Monte Carlo simulations predict that a robust comparison requires about 40 transiting GEMS (compared to the existing sample of ∼15) with 5σ mass measurements. Furthermore, we discuss the limitations of existing occurrence estimates for GEMS and provide a brief description of our planned systematic search to improve the occurrence rate estimates for GEMS.

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“…Looking to our solar system, the ice giant planets Uranus and Neptune are the most similar to TOI-1751 b in mass. However, their internal compositions, gravitational fields, rotation periods, and atmospheric dynamics are poorly constrained (Podolak & Helled 2012;Neuenschwander & Helled 2022;Miguel & Vazan 2023). These substantial uncertainties about ice giant interiors inhibit the use of solar system benchmarks to inform models of extrasolar planets.…”

Section: Toi-1751 B In Contextmentioning

confidence: 99%

The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System

Desai,

Turtelboom,

Harada

et al. 2024

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We present and confirm TOI-1751 b, a transiting sub-Neptune orbiting a slightly evolved, solar-type, metal-poor star (T eff = 5996 ± 110 K, log ( g ) = 4.2 ± 0.1 , V = 9.3 mag, [Fe/H] = −0.40 ± 0.06 dex) every 37.47 days. We use TESS photometry to measure a planet radius of 2.77 − 0.07 + 0.15 R ⊕ . We also use both Keck/HIRES and APF/Levy radial velocities (RV) to derive a planet mass of 14.5 − 3.14 + 3.15 M ⊕ , and thus a planet density of 3.6 ± 0.9 g cm−3. There is also a long-period (∼400 days) signal that is observed in only the Keck/HIRES data. We conclude that this long-period signal is not planetary in nature and is likely due to the window function of the Keck/HIRES observations. This highlights the role of complementary observations from multiple observatories to identify and exclude aliases in RV data. Finally, we investigate the potential compositions of this planet, including rocky and water-rich solutions, as well as theoretical irradiated ocean models. TOI-1751 b is a warm sub-Neptune with an equilibrium temperature of ∼820 K. As TOI-1751 is a metal-poor star, TOI-1751 b may have formed in a water-enriched formation environment. We thus favor a volatile-rich interior composition for this planet.

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Interior and Evolution of the Giant Planets

Cited by 11 publications

References 170 publications

Jupiter Atmospheric Models and Outer Boundary Conditions for Giant Planet Evolutionary Calculations

Jupiter Atmospheric Models and Outer Boundary Conditions for Giant Planet Evolutionary Calculations

Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation

The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System

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