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

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

2011-02-09

arxiv.org/abs/1102.1775v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

Accepted by MNRAS on the 7th February 2011

Scientific paper

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.

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