Juno perijove 5, March 27, 2017 |
Juno perijove 5, March 27, 2017 |
Mar 16 2017, 10:24 PM
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IMG to PNG GOD Group: Moderator Posts: 2251 Joined: 19-February 04 From: Near fire and ice Member No.: 38 |
Juno's perijove 5 is coming up less than two weeks from now - it's on March 27, 2017.
The target selection voting has started and is open until almost four days from now: https://www.missionjuno.swri.edu/junocam/voting?current A large part of the data volume will be reserved for polar time lapse sequences though. John Rogers has written a helpful summary of the upcoming perijove 5: https://www.britastro.org/node/9377 |
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Apr 3 2017, 04:40 PM
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Senior Member Group: Members Posts: 1639 Joined: 5-March 05 From: Boulder, CO Member No.: 184 |
We can see these variable hot-spots in the belts as I'm here reproducing one of the images from the link in post #35. The IR blocking areas in the belts appear to be where white clouds are mixing with the red ones. However the white clouds in the belts appear different in nature/structure than the white clouds in the zones (in #109), so it's unclear to me whether entrainment from the zones is really going on.
The convective clouds in #109 are mostly in a zone, so I wonder if the visible cumuliform cloud is all an overshooting top, or if we can see (through the cirrus) deeper to the source region of the water vapor. It also seems like the rising motion in the zones would be dynamically forced on the large scale with the convection happening more on the small scales. I would continue to entertain the notion that in the zones we're seeing a combination of thin white high ammonia haze, with more structured denser white clouds at a lower altitude. This possibly explains why we see structure in the visible and not so much in the IR. The convection could be happening between these two levels. Some of the darker areas in the zones (and belts) would be where we are seeing even deeper. This link is actually suggesting that the zones have large scale descent. Though it's interesting that they say most convective elements are in the belts. Maybe that's true of some larger storms that could be seen in the Cassini flyby in 2000, or the embedded convective elements in the whiter clouds within the belts as in Bjorn's image in post #31. Perhaps looking at Juno's images now is giving some fresh perspectives on all this. Possibly larger convective storms tend to be in the belts and smaller ones in the zones. On another note I can see rotation in Gerald's oval A6. -------------------- Steve [ my home page and planetary maps page ]
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