Cloud clearing in the wake of Saturn’s Great Storm of 2010 – 2011
Cloud clearing in the wake of Saturn’s Great Storm of 2010 – 2011 and suggested new constraints on Saturn’s He/H2 ratio
L. A. Sromovsky, K. H. Baines, P. M. Fry, T. W. Momary
(Submitted on 11 Nov 2016)
Saturn’s Great Storm of 2010 – 2011 produced a planet-encircling wake that slowly transitioned from a region that was mainly dark at 5 microns in February 2011 to a region that was almost entirely bright and remarkably uniform by December of 2012. The uniformity and high emission levels suggested that the entire wake region had been cleared not only of the ammonia clouds that the storm had generated and exposed, but also of any other aerosols that might provide significant blocking of the thermal emission from Saturn’s deeper and warmer atmospheric layers. Our analysis of VIMS wake spectra from December 2012 provides no evidence of ammonia ice absorption, but shows that at least one significant cloud layer remained behind: a non-absorbing layer of 3 – 4 optical depths (at 2 microns) extending from 150 to ~400 mbar. A second layer of absorbing and scattering particles, with less than 1 optical depth and located near 1 bar, is also suggested, but its existence as a model requirement depends on what value of the He/H2 ratio is assumed. The observations can be fit well with just a single (upper) cloud layer for a He/H2 ratio of 0.064 in combination with a PH3 deep volume mixing ratio of 5 ppm. At lower He/H2 ratios, the observed spectra can be modeled without particles in this region. At higher ratios, in order to fit the brightest wake spectrum, models must include either significant cloud opacity in this region, or significantly increased absorption by PH3, NH3, and AsH3. As the exceptional horizontal uniformity in the late wake is most easily understood as a complete removal of a deep cloud layer, and after considering independent constraints on trace gas mixing ratios, we conclude that the existence of this remarkable wake uniformity is most consistent with a He/H2 mixing ratio of 0.055 (+0.010, -0.015), which is on the low side of the 0.038 – 0.135 range of previous estimates.
Comments: 20 pages, 21 figures, 5 tables
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Journal reference: Icarus 276 (2016) 141-162
DOI: 10.1016/j.icarus.2016.04.031
Cite as: arXiv:1611.03775 [astro-ph.EP] (or arXiv:1611.03775v1 [astro-ph.EP] for this version)
Submission history
From: Lawrence Sromovsky
[v1] Fri, 11 Nov 2016 16:46:49 GMT (2722kb)
https://arxiv.org/abs/1611.03775
