Abstract
We report the detection of HCN on Jupiter. Three R-branch lines of the ν 2 fundamental of HCN near 13.5 μm were observed in absorption, from which the HCN column density is inferred to be 5 × 10 −3 cm-am with an uncertainty of a factor of 2. If emission from the stratosphere exists, then the derived column density is only a lowe limit. We suggest that the Jovian HCN most likely originates from the photolysis of CH 4 and NH 3 in the lower stratosphere and upper troposphere. In addition, an upper limit of 2.5 × 10 −2 cm-am was established for the column density of HCN on Saturn.
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