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Juno: Looking Deep into Jupiter’s Atmosphere

We’re learning more about the composition of Jupiter’s atmosphere, and in particular, the amount of water therein, as a result of data from the Juno mission. The data come in the 1.25 to 22 GHz range from Juno’s microwave radiometer (MWR), depicting the deep atmosphere in the equatorial region. Here, water (considered in terms of its component oxygen and hydrogen) makes up about 0.25 percent of the molecules in Jupiter’s atmosphere, almost three times the percentage found in the Sun. All of this gets intriguing when compared to the results from Galileo.

You’ll recall that the Galileo probe descended into the Jovian atmosphere back in 1995, sending back spectrometer measurements of the amount of water it found down to almost 120 kilometers, where atmospheric pressure reached 320 pounds per square inch (22 bar). Unlike Juno, Galileo showed that Jupiter might be dry compared to the Sun — there was in fact ten times less water than expected — but it also found water content increasing even as it reached its greatest depth, an oddity given the assumption that mixing in the atmosphere would create a constant water content. Did Galileo run into some kind of meteorological anomaly?

A new paper in Nature Astronomy looks at the matter as part of its analysis of the Juno results, which also depict an atmosphere not well mixed:

The findings of the Galileo probe were puzzling because they showed that where ammonia and hydrogen sulfide become uniformly mixed occurs at a level much deeper (~10 bar) than what was predicted by an equilibrium thermochemical model. The concentration of water was subsolar and still increasing at 22 bar, where radio contact with the probe was lost, although the concentrations of nitrogen and sulfur stabilized at ~3 times solar at ~10 bar. The depletion of water was proposed to be caused by meteorological effects at the probe location. The observed water abundance was assumed not to represent the global mean water abundance on Jupiter, which is an important quantity that distinguishes planetary formation models and affects atmospheric thermal structure.

Now Juno has found water content greater than what Galileo measured. But the fact that Galileo showed a water concentration that was still increasing when the probe no longer could send data makes its results inconclusive. The matter is important for those interested in planet formation because as the likely first planet to form, Jupiter would have contained the great bulk of gas and dust that did not go into the composition of the Sun. Thus planet formation models are keyed to factors like the amount of water the young planet would have assimilated. Scott Bolton, Juno principal investigator at the Southwest Research Institute in San Antonio, comments:

“Just when we think we have things figured out, Jupiter reminds us how much we still have to learn. Juno’s surprise discovery that the atmosphere was not well mixed even well below the cloud tops is a puzzle that we are still trying to figure out. No one would have guessed that water might be so variable across the planet.”

Image: The JunoCam imager aboard NASA’s Juno spacecraft captured this image of Jupiter’s southern equatorial region on Sept. 1, 2017. The image is oriented so Jupiter’s poles (not visible) run left-to-right of frame. Credit: NASA/JPL-Caltech/SwRI/MSSS/Kevin M. Gill.

The research team, led by Cheng Li (JPL/Caltech) used data from Juno’s first eight science flybys, focusing on the equatorial region first because the atmosphere appears to be better mixed there than in other regions. Juno’s microwave radiometer can measure the absorption of microwave radiation by water at multiple depths at the same time. Using these methods, Juno could collect data from deeper in the atmosphere than Galileo, where pressures reach about 480 psi (33 bar). The next move will be to compare this with other regions, giving us a picture of water abundance as Juno coverage extends deeper into Jupiter’s northern hemisphere. Of particular interest will be what Juno will find at the planet’s poles.

From the paper:

We have shown that the structure of Jupiter’s EZ [equatorial zone] is steady, relatively uniform vertically and close to a moist adiabat [a region where heat does not enter or leave the system]; from this we have derived its water abundance. The thermal structure outside of the equator is still ambiguous owing to the non-uniform distribution of ammonia gas, for which we do not know the physical origin. Deriving the thermal structure outside of the equator in the future not only hints about the water abundance on Jupiter at other latitudes but also places constraints on the atmospheric circulation model for giant planets in the Solar System and beyond.

Image: Thick white clouds are present in this JunoCam image of Jupiter’s equatorial zone. These clouds complicate the interpretation of infrared measurements of water. At microwave frequencies, the same clouds are transparent, allowing Juno’s Microwave Radiometer to measure water deep into Jupiter’s atmosphere. The image was acquired during Juno’s flyby of the gas giant on Dec. 16, 2017. Credit: NASA/JPL-Caltech/SwRI/MSSS/Kevin M. Gill.

The authors add that Juno has already revealed a deep atmosphere that is surprisingly variable as a function of latitude, highlighting the need to tread cautiously before making any assumptions about the planet’s overall water abundance. Extending these observations into other regions of the planet will be useful because oxygen is the most common element after hydrogen and helium in Jupiter’s atmosphere, and as water ice may thus have been the primary condensable in the protoplanetary disk. Consider this a deep probe into planet formation.

The paper is Li et al., “The water abundance in Jupiter’s equatorial zone,” Nature Astronomy 10 February 2020 (abstract).


Comments on this entry are closed.

  • djlactin February 23, 2020, 7:17

    Here’s an idea: beam an EM ray of appropriate wavelength to arrive as Juno passes behind Jupiter. Juno records what it detects, then returns the information. The spectral difference would encode useful information about the absorptivity spectrum of the Jovian atmosphere. Consolidation of results from “a few” passes might yield a CAT scan of the atmosphere.

  • Harold Shaw February 23, 2020, 19:20

    There are visitors to this site much better qualified to explain the instruments aboard Juno, but hopefully I can offer a useful response.

    The Sun is a powerful source of EM radiation and Juno would use that naturally occurring source the same way you propose it use a man made source. It would look at what the Jovian atmosphere absorbed of the Sun’s EM spectrum. It could also do absorption analysis from directly above the atmosphere by emitting a source of EM radiation and measuring what is absorbed versus what is reflected back.

    • Mike Serfas February 25, 2020, 9:25

      I was thinking the same way when I read this two days ago… but I just saw this article: https://phys.org/news/2020-02-photon-silencing-sun.html Apparently it is possible to use a subset of photons in a specific state (Quantum Parametric Mode Filtering) and detect (nearly) only those photons, not the natural photons, eliminating background light. I haven’t even tried to understand how this works yet, let alone whether it can be done with a new or existing spacecraft, but conceptually it sounds like some form of laser-and-probe approach could be interesting. (The length/depth of the path through the atmosphere is another question: see https://solarsystem.nasa.gov/resources/17394/bent-rings/ )

  • Geoffrey Hillend February 23, 2020, 20:42

    I don’t think that Galileo ran into some kind of meteorological anomaly. It says in this article that Galileo used a spectrometer which I assume is in the visible, or infra red spectrum which has a shorter wavelength than the Juno probes 1.25 to 22 GHZ radio frequency range. Consequently a the Juno probes can penetrate deeper into the atmosphere because microwaves are of a longer wavelength than those used in a spectrometer with are of shorter wave EMR. The spectrometer is more blind to the water vapor in the deeper layers of the atmosphere. The reason being is that shorter wavelengths are closer to the size of the water molecules so they get blocked more easily and the longer wavelengths can bend around the molecules and pass more easily between them.

    The Juno radiometer is a passive radiometer with receives the microwaves which are the thermal heat coming through the clouds of Jupiter in the thermal micro wave EM spectrum which can pass more easily through the clouds than the shorter wavelengths detected by a spectrometer . https://www.youtube.com/watch?v=iakQRb3e0Zg