Modelling the near-IR spectra of Jupiter using line-by-line methods

TL;DR

This study uses high-resolution infrared spectra and line-by-line radiative transfer modeling to analyze Jupiter's atmospheric composition and cloud distribution, achieving a close match with observed spectra and improving understanding of its atmospheric constituents.

Contribution

It introduces a detailed line-by-line modeling approach for Jupiter's near-IR spectra, enhancing the accuracy of atmospheric and cloud property estimations compared to previous low-resolution models.

Findings

Modeled spectra match observations well at K band and low-pressure H band.

Results support previous cloud distribution models for Jupiter.

High-resolution spectra can better constrain atmospheric chemical composition.

Abstract

We have obtained long-slit, infrared spectra of Jupiter with the Anglo Australian Telescope in the K and H bands at a resolving power of 2260. Using a line-by-line, radiative transfer model with the latest, improved spectral line data for methane and ammonia, we derive a model of the zonal characteristics in the atmosphere of this giant planet. We fit our model to the spectra of the zones and belts visible at 2.1 {\mu}m using different distributions of cloud opacities. The modeled spectra for each region match observations remarkably well at K band and in low pressure regions at the H band. Our results for the upper deck cloud distribution are consistent with previous models (Banfield et al.1998) fitted to low resolution, grism spectra. The ability to obtain and model high resolution planetary spectra in order to search for weakly absorbing atmospheric constituents can provide better constraints on the chemical composition of planetary atmospheres.