Mechanisms of convective storm initiation on Jupiter and Saturn
In the atmospheres of giant planets such as Jupiter and Saturn, huge convective storms occasionally develop which can change the visual appearance of the planets’ entire bands. These storms occur when the atmosphere’s water vapor rises and cools, releasing energy and making less dense the ascending...
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| Formato: | tesis de maestría |
| Fecha de publicación: | 2025 |
| País: | España |
| Recursos: | Universidad del País Vasco |
| Repositorio: | Addi. Archivo Digital para la Docencia y la Investigación |
| OAI Identifier: | oai:addi.ehu.eus:10810/75437 |
| Acesso em linha: | http://hdl.handle.net/10810/75437 |
| Access Level: | acceso abierto |
| Palavra-chave: | convective storm moist convection Jupiter and Saturn's atmospheres |
| Resumo: | In the atmospheres of giant planets such as Jupiter and Saturn, huge convective storms occasionally develop which can change the visual appearance of the planets’ entire bands. These storms occur when the atmosphere’s water vapor rises and cools, releasing energy and making less dense the ascending air. However, in the helium and hydrogen atmospheres, the moist air is denser than the dry air, making convection more difficult to initiate. As water vapor is located in the deep levels of the atmosphere tens of kilometers below the upper clouds, the details around the formation of the convective storms are unknown. This Master’s Thesis runs numerical simulations of Jupiter and Saturn convective storms using an existing numerical model developed in the Planetary Sciences Group at UPV/EHU. The specific objective of this work is to investigate alternatives to moist convective initialization beyond classical warm bubbles perturbations. |
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