I'm working on a true color processing of the outer planets maps, projected by the HST team.
The selection of filters varied from year to year, resulting in slightly inconsistent spectral reconstructions, so I tried to recreate the data for the missing filters using synthetic maps. It worked.
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![A clump of gas in front of a hot Jupiter
An attempt to (relatively) realistically paint a hot Jupiter with a quasi-closed type of atmosphere, according to [1][2].
For hot Jupiters, the Lagrange points L1 and L2 are just within a few planetary radii, so it's easy for the atmosphere to escape outward and inward of the orbit. With a lower semi-major axis, the speed of the leaked atmosphere is higher, so it goes in the direction of motion. But solar wind (and light pressure) can stop the leak and form a quasi-closed configuration.
The color of the photometric surface is blue according to modeling ([3] for example) and measurements ([4] for example), but mostly overexposed here. The color of the upper atmosphere is blue due to Rayleigh scattering.
In reality there may be the following differences: smaller photometric radius relative to the outer atmosphere, the planet may not have a clear boundary, the photometric properties of the outer atmosphere are not clear. The brightness balance has also not been calculated.
[1] Gas envelopes of exoplanets - hot Jupiters: https://ui.adsabs.harvard.edu/abs/2021PhyU...64..747B/abstract
[2] Types of Hot Jupiter Atmospheres: https://www.researchgate.net/publication/269725888_Types_of_Hot_Jupiter_Atmospheres
[3] Albedo and Reflection Spectra of Extrasolar Giant Planets: https://ui.adsabs.harvard.edu/abs/2000ApJ...538..885S/abstract
[4] The Deep Blue Color of HD189733b: Albedo Measurements with Hubble Space Telescope/Space Telescope Imaging Spectrograph at Visible Wavelengths: https://ui.adsabs.harvard.edu/abs/2013ApJ...772L..16E/abstract](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:xbjs5d6srll42cljj3kqpdrr/bafkreiclm5qkucfbkj2k56feryg5jtrn724fqhcevfp5m7lio4sfnppzne)
