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I would like to know what would happen with the atmosphere of Venus when it gets tidally locked, i.e. when one side would perpetually face the Sun.
Probably a thermal low would be at the subsolar region then.

At the surface Venus has an atmospheric pressure of 92 atm. and a temperature of 462$⁰$ C.

Are there General Circulation Models or Global Climate Models that can handle such input parameters ?

If so, are there GCM users (groups, universities etc.) who could run a tidally locked Venus simulation ?

Cornelis
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  • You'd be more likely to get a good answer if you asked this question on Astronomy Stack. – Michael Walsby Nov 23 '19 at 17:38
  • I'm voting to close, because I'm pretty sure Venus isn't the Earth. –  Nov 23 '19 at 18:09
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    @BarryCarter The feeling a few years ago was that planetary atmospheres are on-topic here because they're on-topic at AGU/EGU. When it veers into worldbuilding/fiction we tend to close. – Deditos Nov 23 '19 at 19:49
  • I've retraced my close vote. My thought was that Venus is so different from Earth, Earth Science can't help here. We might be able to say something about Mars, because that's more similar to Earth, though, again, not really that much. –  Nov 23 '19 at 19:51
  • A tidally locked Venus would be no different on the surface than current Venus: The atmosphere is so thick and the winds are superrotating, which causes heat redistribution to be very efficient, and hence, Venus is horizontally isothermal on the surface. Tidal locking won't change that. – AtmosphericPrisonEscape Nov 24 '19 at 00:51
  • @AtmosphericPrisonEscape Nevertheless i would think that in the course of many (maybe thousands) years the thermal low would go deeper and deeper into the atmosphere, eventually reaching the surface. When the causes of the rotating winds (the rotation of the planet and diurnal heating) are not there anymore then they would stop because of that, won't they ? – Cornelis Nov 24 '19 at 09:47
  • Atmospheres attain vertical radiative balance within seconds, and convective energy transport in the lower parts of the vertical is as fast as the convective velocity works, which is on the timescale of hours at the worst. Therefore no adjustment on the timescale of many years will happen. And the heat redistribution properties of supercritical $CO_2$ won't just magically disappear, as wont the equatorial jets. – AtmosphericPrisonEscape Nov 24 '19 at 11:23

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I'm not sure of their current status, but I read some papers based on these models a few years ago:

It looks like the introduction of Yamamoto et al (2019) has a more up-to-date summary of the current set of models, and there's quite a healthy selection from groups around the world.

Deditos
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  • Actually i should have asked for a tidally locked Venus model, but you already answered the original question, thank you ! – Cornelis Nov 23 '19 at 22:35