J. Ribeiro, P. Machado, S. Pérez-Hoyos, J. A Dias, P. G. J. Irwin
Abstract
The study of isotopic ratios in planetary atmospheres gives an insight into the formation history and evolution of these objects. The more we can constrain these ratios, the better we can understand the history and future of our solar system. To help in this endeavour, we used Infrared Space Observatory Short Wavelength Spectrometer (ISO/SWS) Jupiter observations in the 793–1500 cm-1 region together with the Nonlinear Optimal Estimator for MultivariatE Spectral analySIS (NEMESIS) radiative transfer suite to retrieve the temperature–pressure profile and the chemical abundances for various chemical species. We also used the 1500–2499 cm-1 region to determine the cloud and aerosol structure of the upper troposphere. We obtained a best-fit simulated spectrum with χ2/N=0.47 for the 793–1500 cm-1 region and χ2/N=0.71 for the 1500–2499 cm-1 region. From the retrieved methane abundances, we obtained, within a 1σ uncertainty, a 12C/13C ratio of 84 ± 27 and a D/H ratio of (3.5 ± 0.6) × 10-5 , and these ratios are consistent with other published results from the literature.
Keywords
Jupiter; vertical structure; spectroscopy; radiative transfer
Atmosphere
Volume 14, Number 1731
2023 December
