VSTAR Modelling of the Infrared Spectrum of Uranus
arXiv:1303.3330
Abstract
We modelled the H-band spectrum obtained with the Infrared Imaging Spectrograph (IRIS2) at the Anglo-Australian Telescope in order to infer the cloud structure and composition of the atmosphere of the planet between 0.1 and 11 bar. Such modelling can be used to derive the D/H ratio in the atmosphere of Uranus, which is an important diagnostic of the conditions in early history of the planetary formation. We describe here our modelling technique based on the Versatile Software for Transfer of Atmospheric Radiation (VSTAR) (Bailey2012a). Since the infrared spectrum of Uranus is dominated by absorption from methane, the accuracy of the models is limited largely by the quality of the low temperature, methane line databases used. Our modelling includes the latest laboratory line data for methane described in Bailey (2011). The parameters of this model will be applied in the future to model our observations of GNIRS high resolution spectra of Uranus and derive the D/H ratio in the 1.58 micron window based on absorption in the deuterated methane band in this region.
arXiv comment11 pages, 4 figures, accepted for the proceedings of the Australian Space Science Conference in 2012
References in corpus (6)
- Uranus at equinox: Cloud morphology and dynamics
- Dynamics of cloud features on Uranus
- The Near-IR Spectrum of Titan Modeled with an Improved Methane Line List
- A Comparison of Water Vapor Line Parameters for Modeling the Venus Deep Atmosphere
- Constraints from deuterium on the formation of icy bodies in the Jovian system and beyond
- Observations of the D/H ratio in Methane in the atmosphere of Saturn's moon, Titan - where did the Saturnian system form?