J. V. Seidel, B. Prinoth, L. Pino, L. A. Dos Santos, H. Chakraborty, V. Parmentier, E. Sedaghati, J. P. Wardenier, C. Farret Jentink, M. R. Zapatero Osorio, R. Allart, D. Ehrenreich, M. Lendl, G. Roccetti, Y. C. Damasceno, V. Bourrier, J. Lillo-Box, H. J. Hoeijmakers, E. Pallé, N. C. Santos, A. Suárez Mascareño, S. G. Sousa, H. M. Tabernero, F. A. Pepe
Abstract
Ultra-hot Jupiters, an extreme class of planets not found in our Solar System, provide a unique window into atmospheric processes. The extreme temperature contrasts between their day and night sides pose a fundamental climate puzzle: how is energy distributed? To address this, we must observe the three-dimensional structure of these atmospheres, particularly their vertical circulation patterns that can serve as a testbed for advanced global circulation models, for example, in ref. 1. Here we show a notable shift in atmospheric circulation in an ultra-hot Jupiter: a unilateral flow from the hot star-facing side to the cooler space-facing side of the planet sits below an equatorial super-rotational jet stream. By resolving the vertical structure of atmospheric dynamics, we move beyond integrated global snapshots of the atmosphere, enabling more accurate identification of flow patterns and allowing for a more nuanced comparison to models. Global circulation models based on first principles struggle to replicate the observed circulation pattern2 underscoring a critical gap between theoretical understanding of atmospheric flows and observational evidence. This work serves as a testbed to develop more comprehensive models applicable beyond our Solar System as we prepare for the next generation of giant telescopes.
Keywords
Atmospheric dynamics / Exoplanets
Nature
Volume 639, Page 902
2025 March
