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Detection of hydrogen sulfide above the clouds in Uranus’s atmosphere
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Detection of hydrogen sulfide above the clouds in Uranus’s atmosphere
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Journal Article
Detection of hydrogen sulfide above the clouds in Uranus’s atmosphere
2018
Overview
Visible-to-near-infrared observations indicate that the cloud top of the main cloud deck on Uranus lies at a pressure level of between 1.2 bar and 3 bar. However, its composition has never been unambiguously identified, although it is widely assumed to be composed primarily of either ammonia or hydrogen sulfide (H
2
S) ice. Here, we present evidence of a clear detection of gaseous H
2
S above this cloud deck in the wavelength region 1.57–1.59 μm with a mole fraction of 0.4–0.8 ppm at the cloud top. Its detection constrains the deep bulk sulfur/nitrogen abundance to exceed unity (>4.4–5.0 times the solar value) in Uranus’s bulk atmosphere, and places a lower limit on the mole fraction of H
2
S below the observed cloud of
(
1.0
-
2.5
)
×
1
0
-
5
. The detection of gaseous H
2
S at these pressure levels adds to the weight of evidence that the principal constituent of 1.2–3-bar cloud is likely to be H
2
S ice.
Ground-based near-infrared spectra of Uranus detected hydrogen sulfide (H
2
S) above the main cloud deck (at a pressure of 1.2–3 bar), suggesting that the bulk sulfur/nitrogen ratio in Uranus’s atmosphere exceeds unity and that the clouds are dominated by H
2
S ice.
