The Time-Resolved Observations of the Dynamic Atmospheres of Uranus and Neptune

Details The Time-Resolved Observations of the Dynamic Atmospheres of Uranus and Neptune The Time-Resolved Observations of the Dynamic Atmospheres of Uranus and Neptune

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sptz.prop20500o&link_type=abstract

Spitzer Proposal ID #20500

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Scientific paper

We propose to continue an important and efficient study of the long-term and rotational variability of the 5-25 micron spectra of Uranus and Neptune using IRS, and the 35-95 micron spectrum of Neptune using MIPS SED. The study pursues evidence in our collaborative work with GTO and our Cycle-1 GO (PID 3534) program which detected both long-term and rotational variations of the spectra of Uranus and Neptune, involving both spectroscopic "window" and stratospheric emission features. We will take advantage of Spitzer's extreme sensitivity and spectral grasp to determine whether the observed properties are the result of changes of temperature, gaseous abundance or condensate cloud thickness. The extension of Neptune's spectrum using MIPS SED will greatly improve the accuracy of the 35-95 micron spectrum of Neptune and improve the determination of Neptune's He/H2 ratio with the goal of determining whether Neptune has retained its primordial abundance of helium or whether helium separation has begun in the outer levels of the atmosphere, as is the case with Jupiter and Saturn. This study is important in order to understand the impact of extreme seasonal forcing on planetary atmospheres (Uranus), creating a paradigm for the spectral variation of small gas giant discoveries around other stars, and characterizing the reliability of Uranus and Neptune as flux calibration sources for the Herschel mission.

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