Deep radiative zones affect the planetary cooling and internal structure: implications for exoplanet characterisation
Fuente:
arXiv
Salvato in:
| Autori principali: | , |
|---|---|
| Natura: | Preprint |
| Pubblicazione: |
2026
|
| Soggetti: | |
| Accesso online: | |
| Tags: |
Aggiungi Tag
Nessun Tag, puoi essere il primo ad aggiungerne!!
|
| _version_ | 1866911545086181376 |
|---|---|
| author | Müller, Simon Helled, Ravit |
| author_facet | Müller, Simon Helled, Ravit |
| contents | The thermal evolution and interior structure of giant exoplanets are sensitive to the treatment of radiative opacity. At temperatures of ~2000 K, depletion of alkali metals can create a window of reduced opacity, potentially giving rise to deep radiative zones. While such zones have been discussed for Jupiter, their role in the evolution and characterisation of warm giant exoplanets has not been systematically investigated. We investigate how opacity windows and the resulting deep radiative zones affect the cooling, radius evolution, and the characterisation of interiors and atmospheres of giant exoplanets. We computed thermal evolution models for warm Jupiters spanning masses of 0.3 to 1.0 Jupiter masses with equilibrium temperatures of 200 to 800 K, with a parametrised reduction of the radiative opacity near ~2000 K. Deep radiative zones develop in moderately irradiated Jupiters older than ~4 Gyr even with unmodified opacities, and earlier and more extensively when the opacity is reduced. A deep opacity window accelerates the planetary cooling, reducing predicted radii by up to 5% and interior temperatures on the order of a few 10%. We show that this translates to a ~10 percentage point difference in inferred bulk metallicity. Deep radiative zones are likely common in warm giant exoplanets and could decouple atmospheric composition from bulk interior composition, complicating the interpretation of atmospheric observations. We suggest that the opacity treatment introduces significant uncertainties in atmospheric and interior characterisation. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2603_24777 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Deep radiative zones affect the planetary cooling and internal structure: implications for exoplanet characterisation Müller, Simon Helled, Ravit Earth and Planetary Astrophysics The thermal evolution and interior structure of giant exoplanets are sensitive to the treatment of radiative opacity. At temperatures of ~2000 K, depletion of alkali metals can create a window of reduced opacity, potentially giving rise to deep radiative zones. While such zones have been discussed for Jupiter, their role in the evolution and characterisation of warm giant exoplanets has not been systematically investigated. We investigate how opacity windows and the resulting deep radiative zones affect the cooling, radius evolution, and the characterisation of interiors and atmospheres of giant exoplanets. We computed thermal evolution models for warm Jupiters spanning masses of 0.3 to 1.0 Jupiter masses with equilibrium temperatures of 200 to 800 K, with a parametrised reduction of the radiative opacity near ~2000 K. Deep radiative zones develop in moderately irradiated Jupiters older than ~4 Gyr even with unmodified opacities, and earlier and more extensively when the opacity is reduced. A deep opacity window accelerates the planetary cooling, reducing predicted radii by up to 5% and interior temperatures on the order of a few 10%. We show that this translates to a ~10 percentage point difference in inferred bulk metallicity. Deep radiative zones are likely common in warm giant exoplanets and could decouple atmospheric composition from bulk interior composition, complicating the interpretation of atmospheric observations. We suggest that the opacity treatment introduces significant uncertainties in atmospheric and interior characterisation. |
| title | Deep radiative zones affect the planetary cooling and internal structure: implications for exoplanet characterisation |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2603.24777 |