Website powered by
Orbital Illustration
3D artist & modeller
Home
Resume

Sudarsky Classes

In the 2000 paper 'Albedo and Reflection Spectra of Extrasolar Giant Planets', David Sudarsky, Adam Burrows and Philip Pinto describe theoretical modelling of the cloud chemistry of gas giant planets. This can be used artistically to create a scientifically informed representation of a planet with a specific set of attributes. Of course, the predictions of Sudarsky et al are limited by the assumptions of their model, and planets will vary in appearance on an individual basis- compare the vivid bands and storms of Jupiter to the muted appearance of Saturn.

Class I (second from the left here), ammonia clouds; similar to Saturn or Jupiter. It should be noted that the model does not include the non-equilibrium compounds that contribute to the color of those planets, though a similar appearance is shown here.

Class I (second from the left here), ammonia clouds; similar to Saturn or Jupiter. It should be noted that the model does not include the non-equilibrium compounds that contribute to the color of those planets, though a similar appearance is shown here.

Class II, water clouds; similar to those we are familiar with on Earth, although in a hydrogen rich atmosphere. This class is the most reflective, with an albedo of 0.8.

Class II, water clouds; similar to those we are familiar with on Earth, although in a hydrogen rich atmosphere. This class is the most reflective, with an albedo of 0.8.

Class III, cloudless; these planets exist at a temperature where there are no compounds readily present to condense into clouds. They have a deep blue hue due to scattering and absorption of light deep into their atmospheres.

Class III, cloudless; these planets exist at a temperature where there are no compounds readily present to condense into clouds. They have a deep blue hue due to scattering and absorption of light deep into their atmospheres.

Class IV, alkali haze; these planets have a very low albedo and dark brown appearance due to the strong absorption spectra of metals such as sodium and potassium, found in a vapor state at these temperatures.

Class IV, alkali haze; these planets have a very low albedo and dark brown appearance due to the strong absorption spectra of metals such as sodium and potassium, found in a vapor state at these temperatures.

Class V, silicate clouds; these planets are so hot that their clouds are comprised of silicate compounds.

Class V, silicate clouds; these planets are so hot that their clouds are comprised of silicate compounds.

Included leftmost is a 'Class 0', to represent planets colder than Class I planets, like Uranus and Neptune. Planets in this temperature range were not part of Sudarsky et al's original analysis.

Included leftmost is a 'Class 0', to represent planets colder than Class I planets, like Uranus and Neptune. Planets in this temperature range were not part of Sudarsky et al's original analysis.

Report