Keywords

Comet C/2016 R2 (PanSTARRS) has a peculiar volatile composition, with CO being the dominant volatile, as opposed to H₂O, and one of the largest N₂/CO ratios ever observed in a comet. Using observations obtained with the Spitzer Space Telescope, NASA's Infrared Telescope Facility, the 3.5 m Astrophysical Research Consortium telescope at Apache Point Observatory, the Discovery Channel Telescope at Lowell Observatory, and the Arizona Radio Observatory 10 m Submillimeter Telescope, we quantified the abundances of 12 different species in the coma of R2 PanSTARRS: CO, CO₂, H₂O, CH₄, C₂H₆, HCN, CH₃OH, H₂CO, OCS, C₂H₂, NH₃, and N₂. We confirm the high abundances of CO and N₂ and heavy depletions of H₂O, HCN, CH₃OH, and H₂CO compared to CO reported by previous studies. We provide the first measurements (or most sensitive measurements/constraints) on H₂O, CO₂, CH₄, C₂H₆, OCS, C₂H₂, and NH₃, all of which are depleted relative to CO by at least 1–2 orders of magnitude compared to values commonly observed in comets. The observed species also show strong enhancements relative to H₂O, and, even when compared to other species like CH₄ or CH₃OH, most species show deviations from typical comets by at least a factor of 2–3. The only mixing ratios found to be close to typical are CH₃OH/CO₂ and CH₃OH/CH₄. The CO₂/CO ratio is within a factor of 2 of those observed for C/1995 O1 (Hale-Bopp) and C/2006 W3 (Christensen) at a similar heliocentric distance, though it is at least an order of magnitude lower than many other comets observed with AKARI. While R2 PanSTARRS was located at a heliocentric distance of 2.8 au at the time of our observations in 2018 January/February, we argue, using sublimation models and comparison to other comets observed at similar heliocentric distance, that this alone cannot account for the peculiar observed composition of this comet and therefore must reflect its intrinsic composition. We discuss possible implications for this clear outlier in compositional studies of comets obtained to date and encourage future dynamical and chemical modeling in order to better understand what the composition of R2 PanSTARRS tells us about the early solar system.

We present a new quantitative model for detailed solar-pumped fluorescent emission of the main isotopologue of CN. The derived fluorescence efficiencies permit estimation and interpretation of ro-vibrational infrared line intensities of CN in exospheres exposed to solar (or stellar) radiation. Our g-factors are applicable to astronomical observations of CN extending from infrared to optical wavelengths, and we compare them with previous calculations in the literature. The new model enables extraction of rotational temperature, column abundance, and production rate from astronomical observations of CN in the inner coma of comets. Our model accounts for excitation and de-excitation of rotational levels in the ground vibrational state by collisions, solar excitation to the ${A}^{2}{{\rm{\Pi }}}_{{\rm{i}}}$ and ${B}^{2}{{\rm{\Sigma }}}^{+}$ electronically excited states followed by cascade to ro-vibrational levels of ${X}^{2}{{\rm{\Sigma }}}^{+}$, and direct solar infrared pumping of ro-vibrational levels in the ${X}^{2}{{\rm{\Sigma }}}^{+}$ state. The model uses advanced solar spectra acquired at high spectral resolution at the relevant infrared and optical wavelengths and considers the heliocentric radial velocity of the comet (the Swings effect) when assessing the exciting solar flux for a given transition. We present model predictions for the variation of fluorescence rates with rotational temperature and heliocentric radial velocity. Furthermore, we test our fluorescence model by comparing predicted and measured line-by-line intensities for ${X}^{2}{{\rm{\Sigma }}}^{+}$ (1–0) in comet C/2014 Q2 (Lovejoy), thereby identifying multiple emission lines observed at IR wavelengths.