Optical constants of Pluto aerosol analogues from UV to near-IR

• Published in: Icarus (New York, N.Y. 1962) N.Y. 1962), 2021-07, Vol.362 (July), p.114398, Article 114398
• Main Authors: Jovanović, Lora, Gautier, Thomas, Broch, Laurent, Protopapa, Silvia, Bertrand, Tanguy, Rannou, Pascal, Fayolle, Marie, Quirico, Eric, Johann, Luc, En Naciri, Aotmane, Carrasco, Nathalie
• Format: Article
• Language: English
• Subjects: Optical constants; Pluto; Pluto, aerosols, haze; Pluto, atmosphere; Pluto, surface; Sciences of the Universe
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1016/j.icarus.2021.114398

Photochemical aerosols were detected as high as 350 km of altitude in Pluto's atmosphere during the New Horizons fly-by. These aerosols are thought to affect Pluto's climate, by acting as cooling agents, and the colours of Pluto's surface, in particular in the dark regions named Cthulhu and Krun and at the North Pole. Pluto atmospheric and surface models have so far used the optical constants of Titan aerosol analogues (tholins), whereas their chemical composition is known to differ from that of Pluto aerosol analogues. In order to provide a new set of optical constants for Pluto tholins, we synthesized analogues of Pluto's aerosols and determined with spectroscopic ellipsometry their optical constants from 270 to 2100 nm. Three types of samples were produced from N2:CH4:CO gas mixtures differing in their CH4:N2 mixing ratio, representative of different altitudes in Pluto's current atmosphere or different seasons or epochs of Pluto. Our analysis shows a strong absorption by Pluto tholins in the UV and visible spectral ranges, with k index of a few 10−1 at 270 nm, in agreement with N- and O-bearing organic molecules. Pluto tholins are less absorbent in the near-IR than in the UV–Vis wavelength range, with k of a few 10−3 between 600 and 2100 nm. Our comparative study highlights the dependency of n and k indices to the CH4:N2 mixing ratio. Aerosols formed at different altitudes in Pluto's atmosphere or during different seasons or epochs of Pluto will therefore affect the budget of Pluto radiative transfer differently. The optical constants presented in this study were tested with a Pluto surface model and with a model of light scattering. The surface modelling results highlight the suitability of these optical constants to reproduce Pluto compositional observations in the visible spectral range by MVIC and LEISA. The atmospheric modelling results conclude that Pluto tholins absorb 5 to 10 times less than Titan tholins at 500 nm, and this lower absorption is consistent with Alice observations of Pluto's haze. •Optical constants [n,k] of Pluto tholins determined by spectroscopic ellipsometry from UV to near-IR•Strong absorption of UV and visible radiations by Pluto tholins, in agreement with N- and O-bearing organic molecules•Dependency of n and k indices to the altitude or epoch of aerosol formation•Suitability of Pluto tholins optical constants to reproduce Pluto compositional observations by MVIC and LEISA•Absorption in the Vis by Pluto tholins weaker than