Inflated hot Jupiters: Inferring average atmospheric velocity via Ohmic models coupled with internal dynamo evolution Article Swipe
Daniele Viganò
,
Soumya Sengupta
,
Clàudia Soriano-Guerrero
,
Rosalba Perna
,
Albert Elias-López
,
Sandeep Kumar
,
Taner Akgün
·
YOU?
·
· 2025
· Open Access
·
· DOI: https://doi.org/10.1051/0004-6361/202555219
YOU?
·
· 2025
· Open Access
·
· DOI: https://doi.org/10.1051/0004-6361/202555219
Aims . The inflated radii observed in hundreds of hot Jupiters (HJ) represent a long-standing open issue. In this study, we quantitatively investigate this phenomenon within the framework of Ohmic dissipation arising from magnetic induction in the atmosphere, one of the most promising mechanisms for explaining the radius anomaly. Methods . Using MESA, we simulated the evolution of irradiated giant planets spanning the observed range of masses and equilibrium temperatures, incorporating an internal source of Ohmic dissipation that extends to deep layers of the envelope. We considered the heat-flux-dependent evolution of the deep-seated dynamo field on which the induced field depends. We adopted a state-of-the-art electrical conductivity, considering the thermal ionisation of alkali metals in the outer layers and the pressure-ionisation in the interior and the corresponding solutions for the induced currents across the planet. Results . We inferred that, in order to reproduce the range of observed radii, the atmospheric wind intensities averaged in the region p ≲ 10 bar have to be in the range O 0.01-1 km/s and to decrease roughly linearly with planetary mass and much more steeply with equilibrium temperature. This is consistent with the expected effects of magnetic drag from the induced field, which is higher for more intense irradiation, via conductivity, and for larger masses, which have higher dynamo fields. Due to the evolution of the dynamo field and the proportionality of the induced currents on it, the Ohmic efficiency typically decreases by at least one order of magnitude from 0.1 to 10 Gyr, which is in contrast with the common assumption of a constant-in-time value. Notably, the extent of the main convective region and the associated heat flux supporting the dynamo is reduced in the presence of strong Ohmic dissipation, which in turn depends on the dynamo field strength, generating a non-trivial coupling of the latter with the atmospheric induction and potentially leading to the oscillatory behaviour of the field strength. These findings remain generally valid even when accounting for a long-term increase in the main-sequence host star luminosity, although this case can more readily lead to HJ re-inflation, consistent with previous studies.
Related Topics
Concepts
Physics
Dynamo
Hot Jupiter
Astrophysics
Dynamo theory
Planet
Astronomy
Exoplanet
Magnetic field
Quantum mechanics
Metadata
- Type
- article
- Language
- en
- Landing Page
- https://doi.org/10.1051/0004-6361/202555219
- OA Status
- hybrid
- References
- 135
- Related Works
- 10
- OpenAlex ID
- https://openalex.org/W4412622470
All OpenAlex metadata
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- DOI
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https://doi.org/10.1051/0004-6361/202555219Digital Object Identifier
- Title
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Inflated hot Jupiters: Inferring average atmospheric velocity via Ohmic models coupled with internal dynamo evolutionWork title
- Type
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articleOpenAlex work type
- Language
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enPrimary language
- Publication year
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2025Year of publication
- Publication date
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2025-07-24Full publication date if available
- Authors
-
Daniele Viganò, Soumya Sengupta, Clàudia Soriano-Guerrero, Rosalba Perna, Albert Elias-López, Sandeep Kumar, Taner AkgünList of authors in order
- Landing page
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https://doi.org/10.1051/0004-6361/202555219Publisher landing page
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YesWhether a free full text is available
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hybridOpen access status per OpenAlex
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https://doi.org/10.1051/0004-6361/202555219Direct OA link when available
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0Total citation count in OpenAlex
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