Europlanet Science Congress 2020
Virtual meeting
21 September – 9 October 2020
Europlanet Science Congress 2020
Virtual meeting
21 September – 9 October 2020
EPSC Abstracts
Vol. 14, EPSC2020-707, 2020, updated on 12 May 2021
https://doi.org/10.5194/epsc2020-707
Europlanet Science Congress 2020
© Author(s) 2021. This work is distributed under
the Creative Commons Attribution 4.0 License.

Optical constants of Pluto tholins

Lora Jovanovic1, Thomas Gautier1, Laurent Broch2, Marie Fayolle3,4, Eric Quirico3, Tanguy Bertrand5, Luc Johann2, Aotmane En Naciri2, and Nathalie Carrasco1
Lora Jovanovic et al.
  • 1Université Paris-Saclay, UVSQ, CNRS, Sorbonne Université, LATMOS/IPSL, Guyancourt, France (lora.jovanovic@latmos.ipsl.fr)
  • 2Université de Lorraine, LCP-A2MC, Metz, France
  • 3Université Grenoble Alpes, CNRS, IPAG, Grenoble, France
  • 4Delft University of Technology, The Netherlands
  • 5NASA Ames Research Center, Moffett Field, CA 94035, USA

I. Introduction

On July 14th, 2015, the New Horizons spacecraft flew by Pluto and revealed the presence of aerosols in the atmosphere [1,2,3] and a curiously dark reddish equatorial region named Cthulhu [1,4]. These photochemical aerosols, extending at more than 350 km of altitude [2,3,5], may affect Pluto atmospheric chemistry and climate [6,7]. Furthermore, it was suggested that these aerosols sediment to constitute the non-icy dark material on the surface of Pluto [4,8]. To interpret the data provided by New Horizons, the atmospheric (e.g. [7]) and surface models (e.g. [4,9]) have so far used the optical constants determined for Titan tholins. Nevertheless, since optical constants strongly depend on the chemical composition of the materials [10], and as Pluto tholins differ chemically from those of Titan [11], Pluto aerosol analogues were synthesized in laboratory and their optical constants were determined by spectroscopic ellipsometry.

II. Experimental setup and analyses protocol

  • Synthesis of Pluto tholins

We used the PAMPRE experimental setup [12] (LATMOS, France) to synthesize Pluto tholins as thin films onto silicon wafers. For this study, the gas mixture injected into the reactor was composed of variable proportions of N2 and CH4, with 500 ppm of CO [5,13], to simulate photochemical aerosols formed at different altitudes on Pluto (Table 1). The experiments were conducted at a pressure of 0.9 ± 0.1 mbar and at ambient temperature.

Table 1: Types of Pluto tholins analyzed in this study

Composition of the gas mixture Corresponding altitude on Pluto [5] Name of the sample
99.5% N2 : 0.5% CH4 : 500 ppm CO < 350 km PH
99% N2 : 1% CH4 : 500 ppm CO 400 km P400
95% N2 : 5% CH4 : 500 ppm CO 600 km P600

 

  • Spectroscopic ellipsometry

We used the UVISEL (Horiba Jobin Yvon) spectroscopic ellipsometer to analyze Pluto tholins thin films. Spectroscopic ellipsometry is a technique measuring the changes in the polarization state between incident and reflected light on the sample, as a function of wavelength. DeltaPsi2® software was used to fit the ellipsometric data. More precisely, a modified Tauc-Lorentz dispersion model determined the thicknesses of the thin films, and a wavelength-by-wavelength inversion method was used to retrieve the refractive indices n (Fig. 1) and the absorption coefficients k (Fig. 2), from 270 to 2100 nm.

III. Optical constants of Pluto tholins from UV to near-IR

Our study shows: (1) the refractive indices n of Pluto tholins vary from 1.60 to 1.77, and such n-values can correspond to organic polymers [14]; (2) a strong absorption of UV and Visible radiation by Pluto tholins, due to their N- and O-bearing molecules [15,16,17]; (3) a lower absorption in the near-IR with k-values of a few 10-3; (4) a dependency of n and k indices to the altitude of aerosols formation, with especially higher n- and k-values in the UV-Vis spectral range for Pluto low-altitude aerosols (PH and P400).

IV. Discussion and Conclusion

Due to higher n-values for the samples PH and P400, compared to the P600 sample, we can suppose that aerosols formed in Pluto's lower atmosphere (≤ 400 km of altitude) will differently scatter the light compared to aerosols formed at higher altitudes (> 400 km of altitude) [18], and thus differently affect the photon flux reaching the lower atmosphere and the surface. The strong absorption below 600 nm is likely due to the presence of N- and O-bearing molecules with lone pair, N- and O-containing polycyclic aromatic compounds and unsaturated molecules with extensive conjugated multiple bonds [14-17]. Since the nitrogen and oxygen content is higher in low-altitude tholins [11], their k indices are higher in the UV-Vis wavelength range. We can thus suppose that in Pluto's atmosphere the aerosols formed at different altitudes will differently absorb the photon flux and differently affect Pluto atmospheric and surface radiative transfer [18].

As Pluto tholins are chemically different from Titan’s [11], we propose a new set of optical constants to update Pluto atmospheric and surface models that were hitherto based on the optical constants of Titan tholins.

Acknowledgements

We are grateful to the European Research Council Starting Grant PrimChem for funding this work (grant agreement n° 636829).

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How to cite: Jovanovic, L., Gautier, T., Broch, L., Fayolle, M., Quirico, E., Bertrand, T., Johann, L., En Naciri, A., and Carrasco, N.: Optical constants of Pluto tholins, Europlanet Science Congress 2020, online, 21 Sep–9 Oct 2020, EPSC2020-707, https://doi.org/10.5194/epsc2020-707, 2020.