Inflation of migrated hot Jupiters

Lous, M.A.S. Mol; Miguel, Yamila

doi:10.1093/mnras/staa1405

Cited by 7 publications

(2 citation statements)

References 63 publications

(60 reference statements)

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“…A larger absorption of stellar flux in the atmosphere can cause the radiative-convective boundary (RCB) to move deeper, which in turn suppresses planetary cooling (e.g., Guillot et al 1996). To date, most planetary evolution theories adopt a one-dimensional (1D) approach and use the mean stellar flux (e.g., Graboske et al 1975;Guillot et al 1996;Marley et al 1996;Burrows et al 1997;Hubbard et al 1999;Fortney & Hubbard 2003;Fortney et al 2007;Ginzburg & Sari 2016;Komacek & Youdin 2017;Komacek et al 2020;Mol Lous 2020). These frameworks have primarily focused on the average characteristics of atmospheres and their effects on interior cooling.…”

Section: Introductionmentioning

confidence: 99%

The Inhomogeneity Effect. II. Rotational and Orbital States Impact Planetary Cooling

Zhang

2023

ApJ

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We generalize the theory of the inhomogeneity effect to enable comparison among different inhomogeneous planets. A metric of inhomogeneity based on the cumulative distribution function is applied to investigate the dependence of planetary cooling on previously overlooked parameters. The mean surface temperature of airless planets increases with rotational rate and surface thermal inertia, which bounds the value in the tidally locked configuration and the equilibrium temperature. Using an analytical model, we demonstrate that the internal heat flux of giant planets exhibits significant spatial variability, primarily emitted from the nightside and high-latitude regions acting as radiator fins. Given a horizontally uniform interior temperature in the convective zone, the outgoing internal flux increases up to several folds as the inhomogeneity of the incoming stellar flux increases. The enhancement decreases with increasing heat redistribution through planetary dynamics or rotation. The outgoing internal flux on rapidly rotating planets generally increases with planetary obliquity and orbital eccentricity. The radiative timescale and true anomaly of the vernal equinox also play significant roles. If the radiative timescale is long, the outgoing internal flux shows a slightly decreasing but nonlinear trend with obliquity. Our findings indicate that rotational and orbital states greatly influence the cooling of planets and impact the interior evolution of giant planets, particularly for tidally locked planets and planets with high eccentricity and obliquity (such as Uranus), as well as the spatial and temporal variations of their cooling fluxes.

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Section: Introductionmentioning

confidence: 99%

The Inhomogeneity Effect. II. Rotational and Orbital States Impact Planetary Cooling

Zhang

2023

ApJ

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“…A common denominator from all these studies is that the inflation of hot-Jupiters is caused by the intense stellar irradiation that these planets receive, and therefore changes in the stellar irradiation either due to stellar evolution (e.g., [39,40,70]) or to the planet migration-that changes their semi major axis and the received Flux-(e.g., [12,101]), can cause a change in the inflation rate of planets, reflecting the planet history.…”

Section: Inflation Of Hot-jupitersmentioning

confidence: 99%

Ariel planetary interiors White Paper

et al. 2021

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The recently adopted Ariel ESA mission will measure the atmospheric composition of a large number of exoplanets. This information will then be used to better constrain planetary bulk compositions. While the connection between the composition of a planetary atmosphere and the bulk interior is still being investigated, the combination of the atmospheric composition with the measured mass and radius of exoplanets will push the field of exoplanet characterisation to the next level, and provide new insights of the nature of planets in our galaxy. In this white paper, we outline the ongoing activities of the interior working group of the Ariel mission, and list the desirable theoretical developments as well as the challenges in linking planetary atmospheres, bulk composition and interior structure.

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Evidence of three mechanisms explaining the radius anomaly of hot Jupiters

Sarkis

Mordasini

Henning

et al. 2021

A&A

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Context. The anomalously large radii of hot Jupiters are still not fully understood, and all of the proposed explanations are based on the idea that these close-in giant planets possess hot interiors. Most of the mechanisms proposed have been tested on a handful of exoplanets. Aims. We approach the radius anomaly problem by adopting a statistical approach. We want to infer the internal luminosity for the sample of hot Jupiters, study its effect on the interior structure, and put constraints on which mechanism is the dominant one. Methods. We developed a flexible and robust hierarchical Bayesian model that couples the interior structure of exoplanets to the observed properties of close-in giant planets. We applied the model to 314 hot Jupiters and inferred the internal luminosity distribution for each planet and studied at the population level (i) the mass–luminosity–radius distribution and as a function of equilibrium temperature the distributions of the (ii) heating efficiency, (iii) internal temperature, and the (iv) pressure of the radiative–convective–boundary (RCB). Results. We find that hot Jupiters tend to have high internal luminosity with 104 LJ for the largest planets. As a result, we show that all the inflated planets have hot interiors with an internal temperature ranging from 200 up to 800 K for the most irradiated ones. This has important consequences on the cooling rate and we find that the RCB is located at low pressures between 3 and 100 bar. Assuming that the ultimate source of the extra heating is the irradiation from the host star, we also illustrate that the heating efficiency increases with increasing equilibrium temperature and reaches a maximum of 2.5% at ~1860 K, beyond which the efficiency decreases, which is in agreement with previous results. We discuss our findings in the context of the proposed heating mechanisms and illustrate that ohmic dissipation, the advection of potential temperature, and thermal tides are in agreement with certain trends inferred from our analysis and thus all three models can explain various aspects of the observations. Conclusions. We provide new insights on the interior structure of hot Jupiters and show that with our current knowledge, it is still challenging to firmly identify the universal mechanism driving the inflated radii.

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Inflation of migrated hot Jupiters

Cited by 7 publications

References 63 publications

The Inhomogeneity Effect. II. Rotational and Orbital States Impact Planetary Cooling

The Inhomogeneity Effect. II. Rotational and Orbital States Impact Planetary Cooling

Ariel planetary interiors White Paper

Evidence of three mechanisms explaining the radius anomaly of hot Jupiters

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