Haze in Pluto's atmosphere

  title={Haze in Pluto's atmosphere},
  author={Andrew F. Cheng and Michael E. Summers and G. Randall Gladstone and Darrell F. Strobel and Leslie A. Young and Panayotis Lavvas and Joshua A. Kammer and Carey M. Lisse and Alex H. Parker and Eliot F. Young and S. Alan Stern and H. Weaver and Cathy B. Olkin and Kimberley Ennico},
LORRI observations of waves in Pluto's atmosphere
A bimodal distribution of haze in Pluto’s atmosphere
Observational evidence that Pluto’s haze particles are bimodally distributed is reported, which successfully reproduces the full phase scattering observations from New Horizons and suggests that haze particles in reducing atmospheres undergo rapid shape change near pressure levels ~0.5 Pa and favors a photochemical rather than a dynamical origin for the formation of Titan's detached haze.
Pluto's haze as a surface material
Characteristics of Pluto’s Haze and Surface from an Analytic Radiative Transfer Model
Observations of Pluto from New Horizons have been combined with previous ground-based observations and fit to a radiative transfer model based on Chandrasekhar’s planetary problem and Hapke theory to
Multilayer hazes over Saturn’s hexagon from Cassini ISS limb images
A system of multi-layered hazes above Saturn’s hexagonal-wave cloud tops in the visual range is analyzed, suggesting the formation to be caused by condensation processes, and the vertical distribution of stacked layers by the upward propagation of internal gravity waves.
A major ice component in Pluto’s haze
Pluto, Titan and Triton all have low-temperature environments with an N 2 , CH 4 and CO atmospheric composition in which solar radiation drives an intense organic photochemistry. Titan is rich in
Constraints on Uranus's haze structure, formation and transport
Aggregate Hazes in Exoplanet Atmospheres
Photochemical hazes have been frequently used to interpret exoplanet transmission spectra that show an upward slope towards shorter wavelengths and weak molecular features. While previous studies
Pluto’s Haze Abundance and Size Distribution from Limb Scatter Observations by MVIC
The New Horizons spacecraft observed Pluto and Charon at solar-phase angles between 16° and 169°. In this work, we use the Multispectral Visible Imaging Camera (MVIC) observations to construct


Pluto's atmosphere
The recent expansion of Pluto's atmosphere
Observations at a variety of visible and infrared wavelengths of an occultation of a star by Pluto in August 2002 reveal evidence for extinction in Pluto's atmosphere and show that it has indeed changed, having expanded rather than collapsed, since 1988.
The atmosphere of Pluto as observed by New Horizons
The New Horizons team presents the complex surface features and geology of Pluto and its large moon Charon, including evidence of tectonics, glacial flow, and possible cryovolcanoes, and their analysis of the encounter data downloaded so far.
The Pluto system: Initial results from its exploration by New Horizons
The New Horizons encounter revealed that Pluto displays a surprisingly wide variety of geological landforms, including those resulting from glaciological and surface-atmosphere interactions as well as impact, tectonic, possible cryovolcanic, and mass-wasting processes.
Pluto’s interaction with its space environment: Solar wind, energetic particles, and dust
Preliminary results from the two New Horizons instruments that measure charged particles are the Solar Wind Around Pluto (SWAP) instrument and the Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) instrument are described, which suggest that very few atmospheric molecules are escaping upstream and becoming ionized.