1,955 research outputs found
Are NH and CO ice present on Miranda?
Published near-infrared spectra of the four largest classical Uranian
satellites display the presence of discrete deposits of CO ice, along with
subtle absorption features around 2.2 m. The two innermost satellites,
Miranda and Ariel, also possess surfaces heavily modified by past endogenic
activity. Previous observations of the smallest satellite, Miranda, have not
detected the presence of CO ice, and a report of an absorption feature at
2.2 m has not been confirmed. An absorption feature at 2.2 m could
result from exposed or emplaced NH- or NH-bearing species, which have a
limited lifetime on Miranda's surface, and therefore may imply that Miranda's
internal activity was relatively recent. In this work, we analyzed
near-infrared spectra of Miranda to determine whether CO ice and the
2.2-m feature are present. We measured the band area and depth of the
CO ice triplet (1.966, 2.012, and 2.070 m), a weak 2.13-m band
attributed to CO ice mixed with HO ice, and the 2.2-m band. We
confirmed a prior detection of a 2.2-m band on Miranda, but we found no
evidence for CO ice, either as discrete deposits or mixed with HO ice.
We compared a high signal-to-noise spectrum of Miranda to synthetic and
laboratory spectra of various candidate compounds to shed light on what species
may be responsible for the 2.2-m band. We conclude that the 2.2-m
absorption is best matched by a combination of NH ice with NH-hydrates
or NH-HO mixtures. NH-bearing salts like NHCl are also
promising candidates that warrant further investigation.Comment: 29 pages, 10 figures. Accepted for publication in Planetary Science
Journa
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