Modeling Of The Uranian Atmosphere Using Near-infrared Spectra From Irtf/spex

Details Modeling Of The Uranian Atmosphere Using Near-infrared Spectra From Irtf/spex Modeling Of The Uranian Atmosphere Using Near-infrared Spectra From Irtf/spex

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.4405n&link_type=abstract

American Astronomical Society, DPS meeting #42, #44.05; Bulletin of the American Astronomical Society, Vol. 42, p.1046

Astronomy and Astrophysics

Astronomy

Scientific paper

We present results from modeling the atmosphere of Uranus to reproduce near-infrared spectra. Our spectral dataset consists of spectra from 0.8-2.5 μm (R = 1200), obtained using the instrument SpeX at NASA's Infrared Telescope Facility on Mauna Kea. These spectra were obtained over three nights each in September 2006 and September 2007. During these observations, we oriented the 0.5" × 15" spectrographic slit perpendicular to Uranus' central meridian, obtaining simultaneous spectral information from center to limb with each slit placement, while minimizing the range of latitudes contributing to each spectrum.
For this analysis we employed an adding-doubling code, modeling the Uranian atmosphere as a vertical series of homogeneous layers and solving primarily for the pressure levels and optical depths of the haze and cloud layers. With the observations in our dataset, we have investigated latitudinal variations in the atmospheric structure of Uranus, as well as temporal changes occurring between 2006 and 2007, most notably the fading of the polar collar at 45° S and the appearance of its counterpart at 45° N.
This project was funded by a NASA Earth and Space Science Fellowship.

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