Impacts of Organic Ice Condensation on the Optical Properties of Haze on Pluto
Abstract
The flyby of the New Horizons spacecraft in 2015 July revealed an unexpected cold atmosphere of Pluto and confirmed the existence of its atmospheric haze. The observed and simulated vertical profiles of chemical species and microphysical processes suggest that the haze particles in Pluto's middle and lower atmosphere may contain organic ice condensation. Such organic ice components can potentially affect Pluto's haze chemistry and optical properties, as well as its energy budget. This study investigates the influence of the ice components on the scattering properties of Pluto's haze by comparing New Horizons observations and simulated particle scattering properties. Comprehensive tests are performed for various haze particle parameters, including their size, chemical component, ice content, and morphology. Scattering properties of these ice-bearing haze particles are calculated by a discrete dipole approximation method and compared to multispectral observations obtained by four New Horizons instruments in spectral regions ranging from the ultraviolet to the near-infrared. The results indicate that the inclusion of the organic ice component leads to higher ratios of backscattering in the visible to extinction in the ultraviolet and provides better agreement with observations compared to monodispersed homogeneous aggregates. But it alone is not sufficient to explain the observed forward scattering values in the visible and near-infrared. Therefore, other scattering sources and/or mechanisms are still required to explain the full set of scattering observations. Further observations, as well as laboratory measurements and numerical tests, are anticipated to improve our understanding of the morphology and ice content of Pluto's haze.
Additional Information
© 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. The authors thank Drs. Maxim A. Yurkin and Alfons G. Hoekstra for their ADDA code. The simulations are conducted in the High-Performance Computing Center of Nanjing University of Information Science & Technology. This work is supported by the National Natural Science Foundation of China (grant No. 42122038). Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (grant No. 80NM0018D0004). Y.L.Y. was supported in part by a NASA NFDAP grant (grant No. 80NSSC19K0823) to Caltech.Attached Files
Published - Wang_2023_Planet._Sci._J._4_17.pdf
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Additional details
- Eprint ID
- 119611
- Resolver ID
- CaltechAUTHORS:20230301-701033500.13
- 42122038
- National Natural Science Foundation of China
- 80NM0018D0004
- NASA/JPL/Caltech
- 80NSSC19K0823
- NASA/Caltech
- Created
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2023-05-12Created from EPrint's datestamp field
- Updated
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2023-05-12Created from EPrint's last_modified field
- Caltech groups
- Division of Geological and Planetary Sciences