Uranus' cloud particle properties and latitudinal methane variation from IRTF SpeX observations

Dane S. Tice*, Patrick G. J. Irwin, Leigh N. Fletcher, Nick A. Teanby, Jane Hurley, Glenn S. Orton, Gary R. Davis

*Corresponding author for this work

Research output: Contribution to journalArticle (Academic Journal)peer-review

18 Citations (Scopus)

Abstract

The Uranian atmosphere was observed in August 2009 from 0.8 to 1.8 mu m using the near-infrared spectrometer, SpeX, at NASA's Infrared Telescope Facility. The observations had a spectral resolution of R=1200 and an average seeing of between 0.5" in the H-Band (1.4-1.8 mu m) and 0.6" in the I-Band (0.8-0.9 mu m). The reduced data were analyzed with a multiple-scattering retrieval code. We were able to reproduce observations when using a vertically-compact cloud in the upper troposphere and a vertically-extended, optically-thin haze above the 1-bar level. The existence of these two clouds is consistent with previous studies.

The sub-micron portion of the data are most sensitive to very small scattering particles, allowing more insight into particle size than other portions of the infrared spectrum. This portion of the spectrum was therefore of particular interest and was not available in most previous studies of the planet. We assumed the particles in both clouds to be relatively strong forward scatterers (with a Henyey-Greenstein asymmetry factor of g = 0.7). Given this assumption, we found single-scattering albedos in the tropospheric cloud particles to be (omega) over bar = 0.7 at wavelengths above 1.4 mu m and to gradually increase to (omega) over bar = 1.0 at wavelengths shortward of 1.0 mu m. In the upper haze, we found single-scattering albedos to be (omega) over bar = 1.0 with the exception of a narrow drop at 1.0 mu m to (omega) over bar = 0.6. We found a preference for upper haze particle radii at r = 0.10 mu m. Retrievals of base pressure, fractional scale height, and optical depth in both cloud layers showed the best agreement with data when the base pressure of the upper haze was fixed just above the tropospheric clouds, rather than at or above the tropopausal cold trap. We found that these same retrievals strongly preferred tropospheric cloud particles of 1.35-mu m radii, and observed cloud top height to increase away from the equator in the case of latitudinally invariant methane abundance.

Latitudinal methane variability was also considered, both through a reflectivity study at the 825-nm collision-induced hydrogen absorption feature, as well as through radiative transfer analysis, using forward modeling and retrievals of cloud properties and methane abundance. The data suggested that methane abundance above the tropospheric clouds increased when moving from the midlatitudes towards the equator by at least 9%. The peak of this equatorial methane enrichment was determined to be at 4 +/- 2 degrees S latitude, having moved nearly 15 degrees northward since a reflectance study of 2002 data (Karkoschka and Tomasko, 2009). (C) 2013 Elsevier Inc. All rights reserved.

Original languageEnglish
Pages (from-to)684-698
Number of pages15
JournalIcarus
Volume223
Issue number2
DOIs
Publication statusPublished - Apr 2013

Keywords

  • Atmospheres, Composition
  • Atmospheres, Structure
  • Uranus, Atmosphere
  • PLANETS
  • Data reduction techniques
  • CH4
  • ATMOSPHERE
  • TEMPERATURES
  • INFRARED-ABSORPTION SPECTRA
  • SPECTROGRAPH
  • CM(-1)
  • HYDROGEN
  • UKIRT
  • OVERTONE BAND

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