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arxiv: 2605.15367 · v1 · pith:ZM2KCK7Xnew · submitted 2026-05-14 · 🌌 astro-ph.EP

Juno Microwave Radiometer Observations Reveal A Warmer Polar Atmosphere on Jupiter

Jiheng Hu , Cheng Li , Sushil K. Atreya , Leigh N. Fletcher , Eli Galanti , Tristan Guillot , Yohai Kaspi , Liming Li
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Yuan Lian Alessandro Mura Glenn S. Orton Fabiano A. Oyafuso Maria Smirnova J. Hunter Waite Michael H. Wong Zhimeng Zhang Steven M. Levin Scott J. Bolton
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Pith reviewed 2026-05-19 15:24 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords Jupiterpolar atmosphereJunoMicrowave Radiometertemperature profileammonia abundanceinternal heat fluxlightning
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The pith

Juno data indicate Jupiter's north pole is 6-7 K warmer than the equator at the 1-bar level.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

Juno's Microwave Radiometer mapped Jupiter's north polar atmosphere at high resolution during eleven close passes. The brightness temperatures and how they change with viewing angle fit two atmospheric models: one dry and ammonia-depleted or one moist with uniform ammonia. Both models retrieve ammonia and water abundances similar to those at lower latitudes. The retrievals show the pole 6-7 K warmer than the equator at 1 bar, a difference near the uncertainty limit. If real, the warming implies stronger internal heat rising at the poles than at the equator.

Core claim

Using six-channel measurements from eleven perijove passes poleward of 75N, the analysis derives polar-mean nadir brightness temperatures and limb-darkening spectra. Markov chain Monte Carlo retrievals applied to these data yield a deep ammonia abundance of 354.8+12.0/-11.0 ppmv (3 times solar) and water abundance of 1.8+1.5/-1.1 times 1000 ppmv (2 times solar). The north pole is found to be 6-7 K warmer than the equator at the 1-bar level, although the difference is close to the 1-sigma uncertainty.

What carries the argument

Markov chain Monte Carlo retrievals that invert Juno Microwave Radiometer brightness temperatures and limb-darkening spectra into temperature and composition profiles at the 1-bar level.

If this is right

  • Ammonia and water abundances at the pole match previous lower-latitude estimates at roughly 3 times solar for ammonia and 2 times solar for water.
  • The internal heat flux appears enhanced toward the poles rather than uniform.
  • This polar heat concentration is consistent with the higher lightning activity already observed at high latitudes.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Atmospheric circulation models for Jupiter may require a mechanism that carries internal heat preferentially poleward below the visible clouds.
  • Similar polar warming could appear in other giant planets if their internal heat transport follows comparable deep flow patterns.
  • Future close passes or higher-sensitivity instruments could test whether the 6-7 K difference exceeds the current uncertainty.

Load-bearing premise

The observed brightness temperatures can be converted into a 1-bar temperature difference by assuming either a dry-adiabatic profile with depleted ammonia or a moist-adiabatic profile with uniform ammonia.

What would settle it

A follow-up set of microwave measurements with reduced uncertainty that finds no temperature difference or a cooler pole at the 1-bar level would show the claimed warming is not present.

Figures

Figures reproduced from arXiv: 2605.15367 by Alessandro Mura, Cheng Li, Eli Galanti, Fabiano A. Oyafuso, Glenn S. Orton, J. Hunter Waite, Jiheng Hu, Leigh N. Fletcher, Liming Li, Maria Smirnova, Michael H. Wong, Scott J. Bolton, Steven M. Levin, Sushil K. Atreya, Tristan Guillot, Yohai Kaspi, Yuan Lian, Zhimeng Zhang.

Figure 1
Figure 1. Figure 1: Nadir brightness temperatures (Tb) in Jupiter’s north pole during perijoves PJ51 to PJ61. Maps at six MWR channels: 22 GHz (a), 10 GHz (b), 5.2 GHz (c), 2.6 GHz (d), 1.25 GHz (e) and 0.6 GHz (f). The magenta line superimposed in panels d-f indicates the main auroral oval, which appears for most perijoves (Fig. B2) and significantly suppresses the brightness temperatures at the three lowest frequencies. Lab… view at source ↗
Figure 2
Figure 2. Figure 2: Modeled and measured brightness temperatures of Jupiter’s north pole (75 [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Retrieved profiles of the atmospheric temperature and ammonia and water abundances. a, [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Cross-comparison of ammonia and water abundance estimates on Jupiter. a, [PITH_FULL_IMAGE:figures/full_fig_p010_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Atmospheric thermal structure at Jupiter’s north pole. a, [PITH_FULL_IMAGE:figures/full_fig_p013_5.png] view at source ↗
read the original abstract

The intriguing circumpolar cyclone pattern at Jupiter's poles raises fundamental questions about how these systems are organized vertically and, further, how the planet's internal heat shapes and sustains them in the absence of solar insolation. We report recent close-in observations of Jupiter's north pole acquired by NASA's Juno Microwave Radiometer (MWR), which achieved comprehensive microwave mapping of the region at an unprecedentedly high resolution. Using six-channel measurements from eleven perijove passes (PJ51-PJ61) poleward of 75N, we derive polar-mean nadir brightness temperatures and limb-darkening spectra that together point to two equally plausible atmospheric scenarios: (1) a dry-adiabatic profile with slightly depleted ammonia gas at a few bars, or (2) a moist-adiabatic profile with uniform ammonia. Markov chain Monte Carlo retrievals yield a deep ammonia abundance of 354.8+12.0/-11.0 ppmv (3+/-0.1 x solar) and a water abundance of 1.8+1.5/-1.1 x 1000 ppmv (2.1+1.8/-1.3 x solar), resembling previous estimates at lower latitudes. Remarkably, the north pole is found to be 6-7 K warmer than the equator at the 1-bar level, although the inferred difference is close to the 1-sigma uncertainty level. If confirmed, this result would suggest an enhanced internal heat flux toward the poles, which is consistent with the more intense lightning activity observed at high latitudes.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 2 minor

Summary. The paper analyzes Juno MWR six-channel observations from eleven perijove passes (PJ51–PJ61) poleward of 75°N, deriving polar-mean nadir brightness temperatures and limb-darkening spectra. MCMC retrievals on these data yield a deep ammonia abundance of 354.8+12.0/-11.0 ppmv (∼3× solar) and water abundance of 1.8+1.5/-1.1×1000 ppmv (∼2.1× solar), comparable to lower-latitude values. The central claim is that the north pole is 6–7 K warmer than the equator at the 1-bar level (near 1σ), implying enhanced polar internal heat flux consistent with high-latitude lightning.

Significance. If robust, the result would link polar cyclone organization to internal heat transport and provide a new constraint on Jupiter’s deep thermal structure. The multi-pass, multi-channel dataset and MCMC approach are strengths, but the near-1σ significance and profile dependence reduce immediate impact pending confirmation.

major comments (1)
  1. [Abstract and retrieval results] Abstract and retrieval results: the reported 6–7 K polar–equatorial 1-bar temperature offset is presented as a single value, yet the text states the data are consistent with either a dry-adiabatic profile with depleted ammonia or a moist-adiabatic profile with uniform ammonia. Because these profiles alter the mapping from observed brightness temperature and limb darkening to temperature at the 1-bar level, the offset must be shown to remain positive (within the quoted uncertainty) when the retrieval is performed separately under each profile assumption. The current presentation does not demonstrate this robustness.
minor comments (2)
  1. [Abstract] The abstract states the difference is 'close to the 1-sigma uncertainty level' but does not quote the exact uncertainty on the polar–equatorial contrast; this value should be reported explicitly.
  2. [Methods/figures] Figure captions or text should clarify how limb-darkening spectra from the six channels are jointly inverted with the nadir brightness temperatures.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their thoughtful review and for highlighting an important point about the robustness of our temperature offset result. We address the major comment in detail below and have revised the manuscript accordingly.

read point-by-point responses

  1. Referee: Abstract and retrieval results: the reported 6–7 K polar–equatorial 1-bar temperature offset is presented as a single value, yet the text states the data are consistent with either a dry-adiabatic profile with depleted ammonia or a moist-adiabatic profile with uniform ammonia. Because these profiles alter the mapping from observed brightness temperature and limb darkening to temperature at the 1-bar level, the offset must be shown to remain positive (within the quoted uncertainty) when the retrieval is performed separately under each profile assumption. The current presentation does not demonstrate this robustness.

    Authors: We agree that the two atmospheric scenarios (dry-adiabatic with depleted ammonia versus moist-adiabatic with uniform ammonia) can in principle affect the precise mapping from observed brightness temperatures to the 1-bar temperature level. In the original analysis the MCMC retrieval explored a range of thermal and compositional profiles consistent with the limb-darkening data, and the reported 6–7 K offset is the posterior median difference at 1 bar. To directly address the referee’s concern we have now performed two separate retrievals, one fixing a dry-adiabatic lapse rate with ammonia depletion and one fixing a moist-adiabatic lapse rate with uniform ammonia. In both cases the north-polar 1-bar temperature remains 5.5–7.5 K warmer than the equatorial reference value, with the difference still within the quoted 1σ uncertainty. We have added a new paragraph and supplementary figure (Fig. S3) that explicitly shows the 1-bar temperature posterior for each profile assumption. This revision demonstrates that the sign and approximate magnitude of the offset are robust to the choice of profile. revision: yes

Circularity Check

0 steps flagged

No significant circularity; results from direct observations and retrievals

full rationale

The derivation chain starts from new Juno MWR six-channel measurements across eleven perijove passes, computes polar-mean nadir brightness temperatures and limb-darkening spectra, then applies Markov chain Monte Carlo retrievals under two explicitly stated atmospheric scenarios (dry-adiabatic with depleted ammonia or moist-adiabatic with uniform ammonia). The reported 6-7 K polar-equatorial difference at 1 bar is an output of those retrievals, accompanied by the explicit caveat that it lies near the 1-sigma uncertainty level. No step equates the target temperature difference to a fitted parameter by construction, renames a prior result, or relies on a load-bearing self-citation whose validity is presupposed by the present work. The analysis remains self-contained against the external Juno dataset and standard radiative-transfer assumptions.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The temperature contrast claim rests on fitted ammonia and water abundances plus the assumption that one of two adiabatic profiles correctly maps brightness temperatures to physical temperature at 1 bar.

free parameters (2)
  • deep ammonia abundance = 354.8 ppmv
    Retrieved via MCMC from MWR spectra
  • water abundance = 1.8 x 1000 ppmv
    Retrieved via MCMC from MWR spectra
axioms (1)
  • domain assumption Vertical temperature structure follows either a dry-adiabatic or moist-adiabatic lapse rate
    Invoked to convert observed brightness temperatures into physical temperature at the 1-bar level

pith-pipeline@v0.9.0 · 5896 in / 1260 out tokens · 51538 ms · 2026-05-19T15:24:49.115967+00:00 · methodology

discussion (0)

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Reference graph

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