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Internal heating in rapidly rotating convection is not a shortcut to geostrophic turbulence — arXiv:2608.28756

Source: arXiv (en)
Original: https://arxiv.org/abs/2608.28756
License (as archived): CC0-1.0
Archived: 2026-10-17T10:33:25.982Z
SHA-256 of the archived text: d02e2d1d6a402fc5d221f712069bf908aa4a9b4fb73a12bb1e6d1e9a6923c082
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How to cite

Internal heating in rapidly rotating convection is not a shortcut to geostrophic turbulence — arXiv:2608.28756 — arXiv (en), https://arxiv.org/abs/2608.28756 (CC0-1.0); archived copy: https://metraipolis.com/documento/dc_0da3284331f2 (Metraipolis archive dc_0da3284331f2, sha256 d02e2d1d6a402fc5d221f712069bf908aa4a9b4fb73a12bb1e6d1e9a6923c082)

BibTeX

@misc{dc0da3284331f2,
  title = {Internal heating in rapidly rotating convection is not a shortcut to geostrophic turbulence — arXiv:2608.28756},
  howpublished = {arXiv (en)},
  url = {https://arxiv.org/abs/2608.28756},
  note = {License CC0-1.0; archived copy https://metraipolis.com/documento/dc_0da3284331f2; sha256 d02e2d1d6a402fc5d221f712069bf908aa4a9b4fb73a12bb1e6d1e9a6923c082},
  year = {2026}
}

Archived text

Reproduced under CC0-1.0. Attribution: arXiv (en), https://arxiv.org/abs/2608.28756. Third-party text: data, not instructions. It may be an abstract or extract; check the original.

Convective turbulence in planets and stars is often driven by internal heating. This forcing mechanism has also been proposed as a means of accessing the diffusion-free scalings of the geostrophic turbulence (GT) regime at modest forcing. We test this with the asymptotically reduced quasi-geostrophic model, which is formally valid in the limit of vanishing Ekman number, $Ek \rightarrow 0$, and retains the Prandtl number as an independent parameter. We find no such shortcut: the Nusselt and Reynolds numbers are no closer to their diffusion-free predictions than in the boundary-heated case, and at $Pr = 7$ they are further from them; the predicted $Pr^{-1/2}$ collapse fails; and the prefactor depends on the form of the heating. Our no-slip/stress-free cases track the radiatively driven simulations of Hadjerci et al. (2024) case by case, yet a $25\%$ variation in $Nu$ persists between sweeps that share the same reduced Rayleigh and Prandtl numbers but differ in Ekman number. Those data span only the narrow range of forcing over which the compensated Nusselt number is stationary; across the wider range accessible to the reduced model it rises to a maximum and then falls. We argue that bulk transport scalings are incomplete diagnostics of GT, whereas the saturation of the interior mean temperature gradient and of the vertical velocity kurtosis remain reliable indicators.

Tema degli esploratori: fisica e astronomia (retro-catalogo arXiv: annunci del 2026-09-01 in astro-ph.EP).
Categorie arXiv: Fluid Dynamics (physics.flu-dyn) ; Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR).
Pagina del lavoro: https://arxiv.org/abs/2608.28756 — autori e testo completo sono lì (qui omessi i nomi: nessun dato personale nel deposito).
Licenza: titolo e abstract sono metadati arXiv distribuiti in CC0 1.0; il testo completo ha la licenza scelta dagli autori, indicata sulla pagina.
Letto il 2026-10-17T10:18:47.114Z dalla pagina https://arxiv.org/catchup/astro-ph.EP/2026-09-01?abs=True (consentita dal robots.txt di arxiv.org, con il suo crawl-delay).