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Cited by 77Stellar, planetary, and galactic studiesAstro and Planetary ScienceAstronomy and Astrophysical Research

EXTENDED HEAT DEPOSITION IN HOT JUPITERS: APPLICATION TO OHMIC HEATING

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Ginzburg, Sivan, Sari, Re’em·2016·The Astrophysical Journal
DOI 10.3847/0004-637x/819/2/116
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Abstract

The observed radii of many giant exoplanets in close orbits exceed theoretical predictions. One suggested origin for this discrepancy is heat deposited deep inside the atmospheres of these “hot Jupiters”. Here, we study extended power sources that distribute heat from the photosphere to the deep interior of the planet. Our analytical treatment is a generalization of a previous analysis of localized “point sources”. We model the deposition profile as a power law in the optical depth and find that planetary cooling and contraction halt when the internal luminosity (i.e., cooling rate) of the planet drops below the heat deposited in the planet’s convective region. A slowdown in the evolutionary cooling prior to equilibrium is possible only for sources that do not extend to the planet’s center. We estimate the ohmic dissipation resulting from the interaction between the atmospheric winds and the planet’s magnetic field, and apply our analytical model to ohmically heated planets. Our model can account for the observed radii of most inflated planets, which have equilibrium temperatures of ≈1500–2500 K and are inflated to a radius of . However, some extremely inflated planets remain unexplained by our model. We also argue that ohmically inflated planets have already reached their equilibrium phase, and no longer contract. Following Wu & Lithwick, who argued that ohmic heating could only suspend and not reverse contraction, we calculate the time it takes ohmic heating to re-inflate a cold planet to its equilibrium configuration. We find that while it is possible to re-inflate a cold planet, the re-inflation timescales are longer by a factor of than the cooling time.

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  • Heating mechanisms that decay with depth, such as ohmic dissipation, have extremely long re-inflation timescales and are unable to re-inflate a Jupiter within the star's lifetime if it cools before arrival.

    “An important caveat is that heating mechanisms that decay with depth, such as the commonly invoked stellar irradiation deposition mechanism of ohmic dissipation (e.g., Batygin & Stevenson 2010), have extremely long re-inflation timescales and are unable to re-inflate a Jupiter within the star's lifetime if it cools before arrival (e.g., Ginzburg & Sari 2016; see also Wu & Lithwick 2013”

    From Origins of Hot Jupiters (2018) · cites this paper as Ginzburg & Sari 2016

    Section 5 (page not available in our copy) estimates an ohmic re-inflation timescale of about 30 Gyr for the modeled case and says a previously cooled planet will not reach its final equilibrium state. But it also says ohmic dissipation can mildly re-inflate the planet, by up to about 0.2 Jupiter radii; the claim's unqualified statement that it is unable to re-inflate is too strong. (LLM, conf=0.88)

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Cited by

Sorted by citations

Authors
Ginzburg, S., & Sari, R.
Affiliations
Hebrew University of Jerusalem (IL)
ORCID
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2016-03-04
Volume
819
Issue
2
Pages
116
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.3847/0004-637x/819/2/116
OpenAlex
W1917754518
Cited by
77
References
1
Citations by year
2025: 7 · 2024: 6 · 2023: 4 · 2022: 5 · 2021: 5 · 2020: 9 · 2019: 3 · 2018: 26 · 2017: 9 · 2016: 2
FWCI
6.38
Type
journal article
Language
en
Open access
Licence
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (publishedVersion)
  • arXiv (Cornell University)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
  • Physical Sciences › Physics and Astronomy › Instrumentation › Astronomy and Astrophysical Research
Keywords
hot Jupiters, Joule heating, planetary radius, planetary cooling, magnetic field, atmospheric winds, equilibrium temperature

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