Spherical Radiative Transfer in C++ (SRTC++): A Parallel Monte Carlo Radiative Transfer Model for Titan

Barnes, Jason W.; MacKenzie, Shannon; Young, E. F.; Trouille, Laura; Rodríguez, S.; Cornet, T.; Jackson, Brian; Ádámkovics, Máté; Sotin, C.; Soderblom, Jason M.

doi:10.3847/1538-3881/aac2db

Cited by 9 publications

(10 citation statements)

References 55 publications

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“…Fig. 6 shows that for incidence angles lower than 30 , we have differences between solvers smaller than 1%, which is in agreement with Barnes et al (2018) result with a Monte-Carlo RT model. Errors reach more than 5% in Titan's atmospheric windows at 60 .…”

Section: Tests Of the Model In A Spherical Viewingsupporting

confidence: 87%

“…[ Barnes et al (2018) consider as acceptable the use of parallel-plane approximation up to 60 for incidence or emergence angles. In this work, we compared the results obtained respectively with SHDOMPP in a parallel-plane approximation and SPSDISORT in a pseudo-spherical J o u r n a l P r e -p r o o f geometry at different incident angles (see Fig.…”

Section: Tests Of the Model Against The Number Of Streamsmentioning

confidence: 99%

See 1 more Smart Citation

Distribution and intensity of water ice signature in South Xanadu and Tui Regio

Coutelier

Cordier

Seignovert

et al. 2021

Icarus

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Section: Tests Of the Model In A Spherical Viewingsupporting

confidence: 87%

Section: Tests Of the Model Against The Number Of Streamsmentioning

confidence: 99%

Distribution and intensity of water ice signature in South Xanadu and Tui Regio

Coutelier

Cordier

Seignovert

et al. 2021

Icarus

View full text Add to dashboard Cite

show abstract

“…Once the radiative transfer equations are derived, they are applied to the images and the haze is removed as best as possible. However, this process is not perfect, and workers are still trying to develop more sophisticated models for haze removal (Barnes et al, 2018). It is due to these atmospheric restrictions that make VIMS data much more qualitative in comparison to data from other bodies in the solar system.…”

Section: Visible and Infrared Mapping Spectrometer (Vims)mentioning

confidence: 99%

Compositional variations of Titan's impact craters indicates active surface erosion

Werynski

Neish

Gall

et al. 2019

Icarus

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Impact craters on Titan are relatively scarce but provide ample information about the subsurface properties and modification processes present there. This study utilizes impact craters to examine compositional variations across Titan's surface and their subsequent modification. Fifteen craters and their ejecta blankets were studied. Subsurface composition was inferred from emissivity data from Cassini's RADAR instrument, and surficial composition from Cassini's Visible and Infrared Mapping Spectrometer (VIMS). Results show subsurface composition of these craters is controlled by their degradation state and local environment. Older craters are more infilled with organics than younger, and dunes craters show more organic enrichment than plains craters. Surficial composition is only controlled by the local environment (i.e. dunes or plains regions). Since degraded craters show organic rich subsurfaces, but varying surface compositions, it is likely there is an active surface process clearing the surface of sediments and infilling the craters' subsurface fractures.

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“…For example, for a cube made of 4096 pixels, the RT model using SPSDISORT has a runtime of less than 24 hours when using 500 processors. Barnes et al (2018) consider as acceptable the use of parallel-plane approximation up to 60 • for incidence or emergence angles. In this work, we compared the results obtained respectively with SHDOMPP in a parallel-plane approximation and SPSDISORT in a pseudo-spherical geometry at different incident angles (see Fig.…”

Section: Test and Preparation Of The Model For Surface Analysismentioning

confidence: 99%

Distribution and intensity of water ice signature in South Xanadu and Tui Regio

Coutelier¹,

Cordier²,

Rannou³

et al. 2024

Preprint

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Titan's surface was revealed by Cassini 's instruments, showing the presence of liquid hydrocarbons in lakes, and features like dry riverbed. In order to study the sediment transport in Titan's channels and to map distribution of the water-ice signature in these terrains, we use a radiative transfer model to retrieve the surface albedo, after we estimated VIMS error via an original method. We also establish a criteria related to the intensity of the water ice signature. The tuning of the radiative transfer model shows that the fractal dimension of Titan's aerosols is higher than previously thought, around 2.3 -2.4. We find spots of increasing signal of water ice downstream, at the margins of Tui Regio, that could correspond to alluvial fans, deltas or crater rims. We also observe a very low water ice signal on Tui Regio, with a positive gradient between the central region and the boundary of the area, possibly due to the thickness variation of an evaporitic layer. The riverbeds show within the error bars a decreasing grain size from the top to the bottom of the channels.

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Spherical Radiative Transfer in C++ (SRTC++): A Parallel Monte Carlo Radiative Transfer Model for Titan

Cited by 9 publications

References 55 publications

Distribution and intensity of water ice signature in South Xanadu and Tui Regio

Distribution and intensity of water ice signature in South Xanadu and Tui Regio

Compositional variations of Titan's impact craters indicates active surface erosion

Distribution and intensity of water ice signature in South Xanadu and Tui Regio

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