High Altitude Hazes

By Candy on 2017-12-28 UT

Our first PJ1 images showed a high altitude cloud extending above the terminator.  Other images show bands of haze.


  1. comment by Philosophia-47 on 2018-09-25 22:10 UT

    Here is our abstract for my talk given at the EPSC in Berlin in 2018 September, summarising the main patterns of haze bands in both hemispheres:

    'Jupiter’s high-latitude hazes as mapped by JunoCam'

  2. comment by Maquet-80 on 2018-08-11 13:53 UT

    The subcomments of this comment will be used for a more complete survey of Jupiter's limb. The rectification algorithm is refined, and uses the mean brightness of the zone of the steepest brightness slope as a definition for limb.

    Attached is a PJ12 survey. Considered are only close-up RGB images with the terminator outside the field of view.

  3. comment by Maquet-80 on 2018-08-11 01:45 UT

    In PJ12, image #87, there is a section of a limb showing two layers of presumably detached haze. This might hint towards four stacked separate weather systems, three of which forming their own inversion layer. On Earth, inversion layers form when warm air is layered above cold air. For Jupiter, it's usually assumed, that temperature is decreasing with altitude. This assumption would suggest hazes of different chemical composition resublimating for specific temperature and pressure conditions, which gradually change with altitude. 

  4. comment by Maquet-80 on 2018-08-05 17:05 UT

    A more complete survey of the Jupiter's limb during PJ14.

  5. comment by Maquet-80 on 2018-08-04 14:27 UT

    Here a crop of the brightness gradient, where a detached haze layer occurs.

  6. comment by Maquet-80 on 2018-08-04 14:25 UT

    The attached zip file shows an approach to analyse Jupiter's haze layer by observing the limb.

    is a draft processing of Perijove 14 image #23, JNCE_2018197_14C00023_V01.

    The green lines in image file
    show the automatically detected limb.

    This limb is used for the limb rectification shown in image file

    Along vertical sections of this rectified view, brightness values can be plotted into diagrams like indicated in file

    The first derivative of the brightness plot shows the structure of the haze layer more distincly. This is shown in file

    The same method can be applied for each of the three color channels separately:

    A large number of sections can be visualized by compiling the diagrams into a movie:

    Note especially the time between 00:15 and 0:35, where there is forming a detached haze layer. But also continuous appearing haze can vary in its brightness gradient.