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arxiv: 2605.22793 · v1 · pith:M3MJGN4Rnew · submitted 2026-05-21 · 🌌 astro-ph.EP · physics.ao-ph· physics.flu-dyn

Variation of Venusian Gravity Wave Absolute Momentum Fluxes and Drag as Retrieved from the Akatsuki Mission

Erdal Yi\u{g}it , Emilia Sloan This is my paper

Pith reviewed 2026-05-22 02:54 UTC · model grok-4.3

classification 🌌 astro-ph.EP physics.ao-phphysics.flu-dyn
keywords gravity wavesVenus atmospheremomentum fluxwave dragAkatsukiradio occultationmiddle atmosphereatmospheric dynamics
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The pith

Akatsuki radio occultation data yield the first estimates of gravity wave momentum fluxes and drags in Venus's middle atmosphere.

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

The paper establishes quantitative values for the horizontal momentum carried by gravity waves and the resulting drag they exert on the background flow, derived from temperature fluctuations measured between 40 and 95 km altitude. These fluxes reach 10-30 m² s⁻² while the associated drags span 0.003-0.03 m s⁻², values that set a lower bound on total wave-driven acceleration. A sympathetic reader would care because such transport and dissipation help determine whether waves can sustain Venus's rapid zonal winds and overall circulation patterns. The analysis shows flux growing exponentially at lower altitudes before attenuating where dissipation occurs, with drag appearing at those same levels. Patterns hold across latitudes and local times, supplying direct observational limits for models that simulate wave-mean flow interactions.

Core claim

Using temperature retrievals from Akatsuki radio occultation measurements, gravity wave activity is characterized as a function of vertical wavenumber and altitude, and for the first time absolute horizontal momentum fluxes of 10-30 m² s⁻² and wave drags of 0.003-0.03 m s⁻² are estimated in the Venusian middle atmosphere between 40-95 km. Momentum flux increases exponentially below approximately 50-60 km, then peaks and attenuates at higher altitudes, while wave drag becomes prominent where momentum flux decreases as a consequence of wave dissipation. Both quantities exhibit multiple altitude-localized maxima consistent with upward propagation followed by dissipation at different altitudes,,

What carries the argument

Conversion of observed temperature perturbation amplitudes into absolute horizontal momentum fluxes and wave drag via linear gravity wave theory applied to radio occultation profiles

If this is right

  • Momentum flux grows exponentially with altitude below 50-60 km before attenuating higher up as waves dissipate.
  • Wave drag appears precisely where momentum flux begins to decrease, quantifying the local acceleration of the mean flow.
  • Multiple localized maxima in flux and drag indicate that waves of different vertical wavelengths dissipate at distinct altitudes.
  • Nonlinear interactions provide the dominant damping that limits amplitude and flux growth with height.
  • The derived values supply observational constraints that numerical models can use to quantify wave-mean flow interactions.

Where Pith is reading between the lines

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

  • The reported drags may contribute to sustaining Venus's superrotating zonal winds, an implication left implicit in the middle-atmosphere focus.
  • Application of the same radio-occultation technique to other planets would enable direct comparison of gravity-wave momentum transport across solar-system atmospheres.
  • Higher-vertical-resolution profiles from future missions could tighten the separation between wave signals and background variability.

Load-bearing premise

Temperature perturbations observed in the radio occultation profiles are produced by atmospheric gravity waves rather than other sources such as thermal tides or instrument noise, and the conversion from temperature amplitude to momentum flux uses a valid linear wave theory without large biases from nonlinear effects or background wind uncertainties.

What would settle it

Independent in-situ wind or temperature measurements at overlapping altitudes that show momentum fluxes or drags differing by more than an order of magnitude from the reported ranges, or high-resolution simulations reproducing the same temperature perturbations without gravity waves, would falsify the estimates.

Figures

Figures reproduced from arXiv: 2605.22793 by Emilia Sloan, Erdal Yi\u{g}it.

Figure 1
Figure 1. Figure 1: Each of these panels plots data from all radio occultation temperature profiles used. (a) Latitude is plotted on the x-axis, altitude on the y-axis for each profile. (b) Longitude is plot￾ted on the x-axis, altitude on the y-axis for each profile. Profiles plotted in red represent daytime observations, profiles plotted in blue represent nighttime observations. (c) Local time is plotted on the x-axis, altit… view at source ↗
Figure 2
Figure 2. Figure 2: The top panel is an ingress observation during orbit 216, with latitudes ranging from 32.26◦ –35.60◦N, longitudes ranging from 196.99–197.05◦ , and solar zenith angle ranging from 42.626◦ – 44.754◦ . The bottom panel is an ingress observation during orbit 118, with lati￾tudes ranging from 32.92 − 45.12◦S, longitudes ranging from 67.48◦ –71.23◦ , and solar zenith angle ranging from 22.121– 32.317◦ . (a, c) … view at source ↗
Figure 3
Figure 3. Figure 3: (a, c) Derived from Orbit 216, 34◦N profiles. (b, d) Derived from Orbit 118, 39◦S profiles. (a, d) Brunt-V¨ais¨al¨a frequency squared, N 2 . (b, e) Background density relative to the source density, ρ0/ρ(z) representing wave growth. (c, f) Amplitude of temperature perturbations, |T ′ | (K), as a function of altitude and vertical wavelength λz. Vertical wavelength is derived from the wavenumber, m. The harm… view at source ↗
Figure 4
Figure 4. Figure 4: Gravity wave absolute momentum flux (upper panels a,b) and absolute horizontal gravity wave drag (lower panels c,d) as a function of altitude and vertical wavelength for the northern midlatitude (left panels a and c; Orbit 216, 34◦N) and southern midlatitude (right pan￾els b and d; Orbit 118, 39◦S). Vertical wavelength bin edges are [ 1 m+1 , 1 m ]. –27– [PITH_FULL_IMAGE:figures/full_fig_p027_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Altitude variations of the total gravity wave absolute horizontal momentum flux (upper panels) and total absolute horizontal gravity wave drag (lower panels) at the two midlat￾itudes shown in Figures 2–4. There is a secondary x-axis for drag in m s−1 day−1 for compari￾son with Earth, where one day is 24 hours. –28– [PITH_FULL_IMAGE:figures/full_fig_p028_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Total absolute gravity wave horizontal momentum flux is plotted as a function of altitude. Red lines represent daytime profiles (SZA < 90◦ ) and blue lines represent nighttime profiles (SZA > 90◦ ). Curves are grouped by latitude: (a) Northern hemisphere low latitudes (0◦ –30◦N), 15 daytime profiles, 11 nighttime profiles; (b) Northern hemisphere middle latitudes (30◦N–60◦N), 8 daytime profiles, 8 nighttim… view at source ↗
Figure 7
Figure 7. Figure 7: Total absolute horizontal gravity wave drag in m s−2 is plotted as a function of altitude. Red lines represent daytime profiles (SZA < 90◦ ) and blue lines represent nighttime profiles (SZA > 90◦ ). Curves are grouped by latitude: (a) Northern hemisphere low latitudes (0◦ –30◦N); (b) Northern hemisphere middle latitudes (30◦ –60◦N); (c) Northern hemisphere high latitudes (60◦ –90◦N); (d) Southern hemispher… view at source ↗
Figure 8
Figure 8. Figure 8: Mean gravity wave amplitude, absolute momentum flux, and absolute drag as a function of vertical wavelength and altitude, derived from Monte Carlo simulations using the southern hemisphere profile from [PITH_FULL_IMAGE:figures/full_fig_p031_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Standard deviation of the wave amplitude, absolute momentum flux, and absolute drag as a function of vertical wavelength and altitude, derived from Monte Carlo simulations using the southern hemisphere profile from [PITH_FULL_IMAGE:figures/full_fig_p032_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Retrieved total gravity wave absolute momentum flux (a–c) and absolute drag (d–f) as a function of altitude, with ±1σ uncertainty bounds derived from Monte Carlo simula￾tions using the southern hemisphere profile from [PITH_FULL_IMAGE:figures/full_fig_p033_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: The variation of the gravity wave absolute momentum flux and absolute drag for the λz =7.5–15 km wavelength bin as a function of horizontal wavelength and altitude. The profile used to derive the momentum flux and drag is the same southern hemisphere profile used in 2. (a) shows the variation of absolute momentum flux with horizontal wavelength. (b) shows the variation of absolute wave drag with horizonta… view at source ↗
read the original abstract

Using temperature retrievals from Akatsuki radio occultation measurements, we characterize gravity wave activity as a function of vertical wavenumber and altitude and, for the first time, estimate the absolute horizontal momentum fluxes and the magnitude of the associated gravity wave drag (i.e., wave acceleration), which quantify the potential effects of these waves in the Venusian middle atmosphere between 40--95 km. Observed temperature perturbations, which are indicative of atmospheric gravity wave activity, reach amplitudes of approximately $\pm$10 K, and significant momentum flux (10--30 m$^2$ s$^{-2}$) and wave drag (0.003--0.03 m s$^{-2}$) are detected across all analyzed profiles. The inferred wave drag represents a lower bound on the total gravity wave-induced drag in the Venusian atmosphere. Momentum flux tends to increase exponentially with altitude below approximately 50--60 km, then peaks and attenuates at higher altitudes. Wave drag becomes prominent where momentum flux begins to decrease, which is a consequence of wave dissipation. Both quantities exhibit multiple altitude-localized maxima, which is consistent with upward wave propagation followed by dissipation at different altitudes for different vertical wavelengths. Damping due to gravity wave nonlinear interactions is likely to play the major role in limiting the growth of wave amplitudes and fluxes with height. These features are observed across a range of latitudes and local times. Overall, the results provide observational constraints on gravity wave momentum transport and dissipation in the Venusian middle atmosphere and could guide numerical models in their effort to quantify wave-mean flow interactions in Venus's atmosphere.

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

2 major / 2 minor

Summary. The paper uses temperature retrievals from Akatsuki radio occultation measurements to characterize gravity wave activity in the Venusian middle atmosphere (40-95 km) as a function of vertical wavenumber and altitude. It provides the first estimates of absolute horizontal momentum fluxes (10-30 m² s⁻²) and associated wave drag (0.003-0.03 m s⁻²), showing exponential growth of flux below ~50-60 km followed by attenuation, with drag prominent where flux decreases due to dissipation. Multiple altitude-localized maxima are reported, attributed to upward propagation and dissipation at different vertical wavelengths, with nonlinear interactions likely dominating damping. The inferred drag is presented as a lower bound on total gravity wave-induced drag, offering observational constraints for models of wave-mean flow interactions across latitudes and local times.

Significance. If the central estimates hold, the work supplies the first direct observational quantification of gravity wave momentum transport and drag in the Venus middle atmosphere, addressing a key gap in understanding superrotation and circulation. The use of Akatsuki radio occultation data to derive these quantities across a range of conditions provides reproducible, falsifiable inputs that can guide numerical models. The reported altitude dependence and multiple dissipation levels add empirical detail to wave propagation and breaking processes on Venus.

major comments (2)
  1. [Section 3.2] Section 3.2 (momentum flux derivation): The conversion of temperature perturbations (±10 K) to absolute horizontal momentum flux via linear polarization relations requires accurate background wind, stability, and horizontal wavenumber; however, no uncertainty propagation or sensitivity tests from the assumed zonal wind profile are presented, directly scaling the reported 10-30 m² s⁻² fluxes and 0.003-0.03 m s⁻² drags.
  2. [Section 4] Section 4 (results and drag lower-bound claim): The assertion that observed perturbations are dominated by gravity waves (rather than thermal tides or noise) and that the derived drag is a lower bound lacks explicit data selection/exclusion criteria, validation against independent measurements, or quantitative assessment of nonlinear saturation biases, which are load-bearing for the central observational claim.
minor comments (2)
  1. [Abstract] Abstract: The momentum flux and drag ranges are stated without accompanying error bars or statistical measures; adding these would improve clarity of the reported significance.
  2. [Figures] Figure captions (e.g., those showing altitude profiles): Some panels lack explicit indication of the number of profiles averaged or the vertical resolution used, which would aid reproducibility.

Simulated Author's Rebuttal

2 responses · 1 unresolved

We thank the referee for their constructive and detailed review. The comments identify important areas for strengthening the robustness and transparency of our analysis, particularly regarding uncertainties in the momentum flux derivation and the justification for interpreting the signals as gravity-wave dominated. We respond to each major comment below.

read point-by-point responses

  1. Referee: [Section 3.2] Section 3.2 (momentum flux derivation): The conversion of temperature perturbations (±10 K) to absolute horizontal momentum flux via linear polarization relations requires accurate background wind, stability, and horizontal wavenumber; however, no uncertainty propagation or sensitivity tests from the assumed zonal wind profile are presented, directly scaling the reported 10-30 m² s⁻² fluxes and 0.003-0.03 m s⁻² drags.

    Authors: We agree that the absolute momentum flux and drag values are sensitive to the choice of background zonal wind and that a quantitative uncertainty analysis is required. In the revised manuscript we will add sensitivity tests in Section 3.2 in which the zonal wind profile is perturbed by ±10 m s⁻¹ (reflecting the range reported by prior observations and models). We will also implement uncertainty propagation through the linear polarization relations, combining temperature retrieval errors with the wind and stability uncertainties, and will report the resulting ranges on the quoted flux and drag values. revision: yes

  2. Referee: [Section 4] Section 4 (results and drag lower-bound claim): The assertion that observed perturbations are dominated by gravity waves (rather than thermal tides or noise) and that the derived drag is a lower bound lacks explicit data selection/exclusion criteria, validation against independent measurements, or quantitative assessment of nonlinear saturation biases, which are load-bearing for the central observational claim.

    Authors: We will revise Section 4 to include explicit data-selection criteria: profiles are retained only when the vertical wavenumber spectrum is consistent with gravity-wave scales (wavelengths 1–20 km) after removal of large-scale trends, and profiles showing dominant tidal signatures are excluded. We will also expand the discussion of the lower-bound nature of the drag by adding a qualitative assessment of nonlinear saturation effects, noting that the linear-theory assumption may underestimate drag where wave amplitudes approach saturation. Direct validation against independent measurements is not feasible at present because no concurrent, co-located observations of momentum flux exist for the Venus middle atmosphere; we will therefore limit the comparison to published model results and earlier indirect estimates. revision: partial

standing simulated objections not resolved
  • Direct validation of the derived momentum fluxes and drags against independent observational datasets, as no such concurrent measurements currently exist for the Venusian middle atmosphere.

Circularity Check

0 steps flagged

No circularity: observational retrieval from Akatsuki data using standard linear theory

full rationale

The paper derives momentum flux and wave drag estimates directly from observed temperature perturbations in radio occultation profiles by applying established linear gravity-wave polarization relations. This is an empirical retrieval chain, not a closed theoretical loop or self-referential derivation. No steps reduce by construction to fitted inputs, self-citations, or ansatzes imported from the authors' prior work; the reported ranges (10-30 m² s⁻² fluxes, 0.003-0.03 m s⁻² drags) are presented as lower-bound inferences from data rather than predictions forced by the method itself. The derivation remains self-contained against external benchmarks of linear wave theory.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review; no explicit free parameters, axioms, or invented entities are identifiable. The conversion from temperature amplitude to momentum flux implicitly relies on linear gravity-wave polarization relations and an assumed background atmosphere, but these are not quantified here.

pith-pipeline@v0.9.0 · 5826 in / 1280 out tokens · 37585 ms · 2026-05-22T02:54:56.326258+00:00 · methodology

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