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At wavelengths between 0.15 and 0.19 $\mu$m, the far-ultraviolet spectrum ofJupiter is dominated by the scattered solar spectrum, attenuated by molecularabsorptions primarily by acetylene and ethane, and to a lesser extent ammoniaand phosphine. We describe the development of our radiative transfer code thatenables the retrieval of abundances of these molecular species from ultravioletreflectance spectra. As a proof-of-concept we present an analysis of CassiniUltraviolet Imaging Spectrograph (UVIS) observations of the disk of Jupiterduring the 2000/2001 flyby. The ultraviolet-retrieved acetylene abundances inthe upper stratosphere are lower than those predicted by models based solely oninfrared thermal emission from the mid-stratosphere observed by the CompositeInfrared Spectrometer (CIRS), requiring an adjustment to the vertical profilesabove 1 mbar. We produce a vertical acetylene abundance profile that iscompatible with both CIRS and UVIS, with reduced abundances at pressures $<$1mbar: the 0.1 mbar abundances are $1.21 \pm 0.07$ ppm for acetylene and $20.8\pm 5.1$ ppm for ethane. Finally, we perform a sensitivity study for the JUICEUVS instrument, which has extended wavelength coverage out to 0.21 $\mu$m,enabling the retrieval of ammonia and phosphine abundances, in addition toacetylene and ethane.

Jupiter in the ultraviolet: acetylene and ethane abundances in the stratosphere of Jupiter from Cassini observations between 0.15 and 0.19 $\mu$m