Judy/Geckzilla, who processed the JWST data, confirmed the following on
https://geckzilla.com/:
Red (screen): NIRCam F322W2-F323N (this is not a subtraction function, both filters were used at the same time)
Blue: NIRCam F212N
Background is a grayscale combination of both filters. There were gaps in the data that had to be filled in using either filter to complete the other.
This page,
https://jwst-docs.stsci.edu/jwst-near-i ... am-filters, shows the wavelengths involved for these filters:
F322W-F323N: 2.5 to 4.1 microns
F212N: 2.1 to 2.15 microns
This page from NASA,
https://science.nasa.gov/ems/07_infraredwaves, has an interesting discussion related to interpreting infrared [IR] imaging.
It has some images showing a calibration between temp and colors in a dog image. This Jupiter image is not calibrated to specific temperatures but we can get a sense of hot and cold. Here is my reasoning.
Consider the image of the dog at the NASA page noted above.
Consider that the light areas of the IR image go with areas of the dog where the temp is high and IR energy is reflected (not absorbed). Dark areas of the IR image go with areas of the dog where temp is not high and IR energy is absorbed.
Quoted from the above NASA page,
Infrared waves have longer wavelengths than visible light and can pass through dense regions of gas and dust in space with less scattering and absorption.
In the JWST image of Jupiter processed by Geckzilla, we can see that the horizontal bands, or zonal flows, have different temps. (Jupiter is characterized by bands that alternately have rotational momentum in opposite directions.) The JWST/Geckzilla image shows cold temps at the poles and interestingly, the Great Red Spot [GRS] is cold at the depth to which the IR rays penetrate.
Additional temp data for the GRS comes from Juno's Microwave Radiometer, which penetrates to about 350 km. Here is a slide from a presentation at the 2019 AGU Fall Meeting which shows a range of temps with depth - and even a range of temps within the same depth.
In this case, with microwave EM as imaged by Galanti et.al., darker colors indicate cooler temps and lighter colors indicate warmer temps. Note that at 0 km, the temp is mostly cooler. At 50 km, it is mostly warmer. At 350 km, about 25% to 33% of the depth range is cooler with the remaining 66% to 75% being warmer.
VictorBorun asked:
Why evening clouds gap, 670 km at the equator?
Why bright polar cups?
It seems to me that the gap that is noted on the right side of the image is due to IR waves passing through the dust and gases that are present so that they are not being scattered/reflected or absorbed. The gap probably does not exist in visible light.
The reason for the bright polar caps and bright GRS, according to the model I submit in my published poster at AGU Fall Meeting 2020,
https://agu2020fallmeeting-agu.iposters ... 5-8F-8C-6A is that Jupiter has gaseous debris on top of an ice shell. Gases on a rotating body accumulate at the equator, and are sparse at the poles. Evidently, the gases and other debris are about 3750 km thick at the equator; because, T. Guillot et. al. report in a paper that the gravity data from Juno reveals rigid-body rotation under 3500 km - 3750 km of equatorial gases. Guillot, T., Miguel, Y., Militzer, B. et al. A suppression of differential rotation in Jupiter’s deep interior. Nature 555, 227–230 (2018).
https://doi.org/10.1038/nature25775. (To be clear the authors of the paper attribute the rigid-body rotation to electromagnetic effects, NOT an ice layer.)
My research uses UV data from Juno to reveal that Jupiter's poles exhibit complete absorption of UV in a characteristic wavelength range for UV absorption by ice in space (vacuum UV [VUV]). Brightness for water ice in space goes to zero for VUV at 165 nm to 180 nm. I show this in the 6th evidence section in the "Evidence from Juno, Cassini and Other" part of my poster. This is true for UV brightness readings from latitudes +90 deg to -74.5 deg and -90 deg to -74.5 deg. I found it to be true even in the area of the auroras.
A UV loss cone was reported by Allegrini et. al. 2020, "Energy flux and characteristic energy of electrons over Jupiter's main auroral emission." Journal of Geophysical Research; Space Physics, 125, e2019JA027693. The Allegrini team was focused on the aurora activity and did not track UV at specific wavelengths. I believe that this is why they did not see the UV loss at wavelengths 165 nm to 180 nm in the regions of the aurorae.
Jupiter's temperature story involves heat due to friction with the differential flows of debris on top of the ice shell. This heat maintains a thin water layer between the ice shell and the outer swirling debris... according to the model I assert.
To be clear, the trusted professors of space science do not even entertain the idea that Jupiter could have an ice shell. Even though Scott Bolton, the lead investigator of the Juno mission said that Jupiter is a whole new planet from what we thought, the team is still, for the most part, using the same models that they were prior to Juno's insertion into its planetary orbits.
Anyway, I thought that some of my fellow Asterisk participants might be interested in some of this info, Please forgive me if I have stepped out of bounds to bring up a nonstandard interpretation of data observations.
I sign off with my favorite image of Jupiter in infrared light, from the far side of Jupiter.
Judy/Geckzilla, who processed the JWST data, confirmed the following on [url]https://geckzilla.com/[/url]:
[quote]Red (screen): NIRCam F322W2-F323N (this is not a subtraction function, both filters were used at the same time)
Blue: NIRCam F212N
Background is a grayscale combination of both filters. There were gaps in the data that had to be filled in using either filter to complete the other.[/quote]
This page, [url]https://jwst-docs.stsci.edu/jwst-near-infrared-camera/nircam-instrumentation/nircam-filters[/url], shows the wavelengths involved for these filters:
F322W-F323N: 2.5 to 4.1 microns
F212N: 2.1 to 2.15 microns
This page from NASA, [url]https://science.nasa.gov/ems/07_infraredwaves[/url], has an interesting discussion related to interpreting infrared [IR] imaging.
It has some images showing a calibration between temp and colors in a dog image. This Jupiter image is not calibrated to specific temperatures but we can get a sense of hot and cold. Here is my reasoning.
Consider the image of the dog at the NASA page noted above.
[img]https://science.nasa.gov/science-pink/s3fs-public/styles/large/public/thumbnails/image/infrared-4.jpg[/img]
Consider that the light areas of the IR image go with areas of the dog where the temp is high and IR energy is reflected (not absorbed). Dark areas of the IR image go with areas of the dog where temp is not high and IR energy is absorbed.
Quoted from the above NASA page, [quote]Infrared waves have longer wavelengths than visible light and can pass through dense regions of gas and dust in space with less scattering and absorption.[/quote]
In the JWST image of Jupiter processed by Geckzilla, we can see that the horizontal bands, or zonal flows, have different temps. (Jupiter is characterized by bands that alternately have rotational momentum in opposite directions.) The JWST/Geckzilla image shows cold temps at the poles and interestingly, the Great Red Spot [GRS] is cold at the depth to which the IR rays penetrate.
Additional temp data for the GRS comes from Juno's Microwave Radiometer, which penetrates to about 350 km. Here is a slide from a presentation at the 2019 AGU Fall Meeting which shows a range of temps with depth - and even a range of temps within the same depth.
[img2]https://massvortex.science/wp-content/uploads/2022/07/Temp-with-depth-GRedSpot-AGU-2019-Galanti-et-al-IMG_0240-scaled.jpg[/img2]
In this case, with microwave EM as imaged by Galanti et.al., darker colors indicate cooler temps and lighter colors indicate warmer temps. Note that at 0 km, the temp is mostly cooler. At 50 km, it is mostly warmer. At 350 km, about 25% to 33% of the depth range is cooler with the remaining 66% to 75% being warmer.
VictorBorun asked:
[quote]Why evening clouds gap, 670 km at the equator?
Why bright polar cups?[/quote]
It seems to me that the gap that is noted on the right side of the image is due to IR waves passing through the dust and gases that are present so that they are not being scattered/reflected or absorbed. The gap probably does not exist in visible light.
The reason for the bright polar caps and bright GRS, according to the model I submit in my published poster at AGU Fall Meeting 2020, [url]https://agu2020fallmeeting-agu.ipostersessions.com/Default.aspx?s=83-F0-05-90-75-F7-6D-C6-E5-B2-AF-C9-25-8F-8C-6A[/url] is that Jupiter has gaseous debris on top of an ice shell. Gases on a rotating body accumulate at the equator, and are sparse at the poles. Evidently, the gases and other debris are about 3750 km thick at the equator; because, T. Guillot et. al. report in a paper that the gravity data from Juno reveals rigid-body rotation under 3500 km - 3750 km of equatorial gases. Guillot, T., Miguel, Y., Militzer, B. et al. A suppression of differential rotation in Jupiter’s deep interior. Nature 555, 227–230 (2018). https://doi.org/10.1038/nature25775. (To be clear the authors of the paper attribute the rigid-body rotation to electromagnetic effects, NOT an ice layer.)
My research uses UV data from Juno to reveal that Jupiter's poles exhibit complete absorption of UV in a characteristic wavelength range for UV absorption by ice in space (vacuum UV [VUV]). Brightness for water ice in space goes to zero for VUV at 165 nm to 180 nm. I show this in the 6th evidence section in the "Evidence from Juno, Cassini and Other" part of my poster. This is true for UV brightness readings from latitudes +90 deg to -74.5 deg and -90 deg to -74.5 deg. I found it to be true even in the area of the auroras.
A UV loss cone was reported by Allegrini et. al. 2020, "Energy flux and characteristic energy of electrons over Jupiter's main auroral emission." Journal of Geophysical Research; Space Physics, 125, e2019JA027693. The Allegrini team was focused on the aurora activity and did not track UV at specific wavelengths. I believe that this is why they did not see the UV loss at wavelengths 165 nm to 180 nm in the regions of the aurorae.
Jupiter's temperature story involves heat due to friction with the differential flows of debris on top of the ice shell. This heat maintains a thin water layer between the ice shell and the outer swirling debris... according to the model I assert.
To be clear, the trusted professors of space science do not even entertain the idea that Jupiter could have an ice shell. Even though Scott Bolton, the lead investigator of the Juno mission said that Jupiter is a whole new planet from what we thought, the team is still, for the most part, using the same models that they were prior to Juno's insertion into its planetary orbits.
Anyway, I thought that some of my fellow Asterisk participants might be interested in some of this info, Please forgive me if I have stepped out of bounds to bring up a nonstandard interpretation of data observations.
I sign off with my favorite image of Jupiter in infrared light, from the far side of Jupiter.
[img2]https://s3.amazonaws.com/ipostersessions-agu/b5757a24-aed5-4651-a152-392331e0382d.jpg[/img2]