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REVIEW 4 major objections 5 minor 298 references

The paper reports faint, concentric, planet-wide rings in Venus's polarized light and shows that 5-10% gas-density variations above the clouds, consistent with gravity waves, can produce them while leaving ordinary brightness unchanged.

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2026-08-01 20:35 UTC pith:NUOXJ7LI

load-bearing objection Candidate detection with an honest caveat: the rings are genuinely new in polarized flux, but whether they are Venusian waves or an instrument artifact is not settled, and the forward model is partly tuned to the observation. the 4 major comments →

arxiv 2607.16557 v1 pith:NUOXJ7LI submitted 2026-07-17 astro-ph.EP

Planet-wide, Concentric Density Waves in Venus's Upper Atmosphere Revealed through Polarimetry?

Gourav Mahapatra , Michiel Rodenhuis , Frans Snik , Daphne M. Stam , Lo\"ic Rossi , Christoph Keller This is my paper
classification astro-ph.EP
keywords Venuspolarimetrygravity wavesatmospheric density wavesradiative transferStokes parametersupper atmosphereplanetary atmospheres
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper describes a serendipitous 36-minute observation in 2010 in which faint concentric rings appeared in polarized light reflected from Venus, though not in simultaneous total-flux images. It argues that these rings are a physically plausible atmospheric signal: radiative-transfer simulations show that 5-10% variations in gas density above the cloud tops, such as a planet-wide gravity wave would produce, create exactly this kind of polarization pattern while leaving total flux nearly unaffected. The authors stop short of claiming a confirmed detection, because the instrument was dismantled before the rings were noticed and only this single data set exists. Their goal is to establish that the pattern is worthy of targeted polarimetric follow-up as a new observational window into Venus's upper atmosphere.

Core claim

The central discovery claim is that faint concentric rings in the linearly polarized flux of sunlight reflected by Venus, observed for 36 minutes through several visible-wavelength filters, can be produced by gaseous density perturbations of 5-10% in the atmosphere above the cloud and haze layers. Such perturbations are invisible in total-flux images because the bright cloud deck dominates brightness, but they alter the balance between singly scattered Rayleigh molecular light and multiply scattered light, shifting the degree of polarization by up to about 5e-4 relative to surroundings. The pattern's geometry, centered slightly downwind of the sub-solar point, its wavelength dependence, and

What carries the argument

The mechanism behind the signal is the high sensitivity of polarized reflected sunlight to small amounts of molecular (Rayleigh) scattering above Venus's bright cloud deck. Because singly scattered molecular light is highly polarized with a direction opposite to that from cloud aerosols, changing the gas column density by a few percent alters the degree of linear polarization while leaving total flux almost unchanged. The observational technique is dual-beam exchange double-differencing, which suppresses first-order instrumental polarization; the theoretical counterpart is an adding-doubling radiative-transfer code that computes the full Stokes vector for a layered model atmosphere with impo

Load-bearing premise

The load-bearing premise is that the concentric rings are a real signal from Venus's atmosphere and not an unknown artifact of the instrument or Earth's atmosphere; the paper itself acknowledges that the available data cannot fully exclude such an artifact because no re-observation is possible.

What would settle it

A repeat observation with an imaging polarimeter of comparable or better sensitivity, ideally at a phase angle near 90 degrees and in a blue or narrow visible filter, that either reproduces the ring pattern at the predicted amplitude and wavelength dependence or fails to find it. If the 2010 pattern were an instrument artifact, it would not move with Venus's orientation or phase angle across multiple nights; if it is atmospheric, the model's predicted strengthening near 90-degree phase angle and at shorter wavelengths should be readily detectable.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • If the rings are real, high-sensitivity imaging polarimetry can reveal density-wave activity in Venus's upper atmosphere that is completely invisible in ordinary brightness imaging.
  • The modeled sensitivity to density variations increases toward shorter wavelengths because Rayleigh scattering is stronger, so future polarimetric observations in blue or visible filters are the most promising for confirming the rings.
  • A ring pattern centered slightly downwind of the sub-solar point implies wave generation near the sub-solar region and transport by the strong zonal winds, so repeated observations could measure wave propagation speeds and constrain atmospheric dynamics.
  • The observed visibility in three filters and absence in later ones is explained by a combination of wavelength-dependent sensitivity and degraded seeing or airmass, meaning that the non-detections do not weaken the physical interpretation.

Where Pith is reading between the lines

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

  • Editorial inference: If the pattern is genuine, it suggests a previously unrecognized class of planet-wide, coherent density waves on Venus that couple the sub-solar heating region to the terminators; such waves could contribute to momentum transport and help explain the puzzling super-rotation of the atmosphere.
  • Editorial inference: The same polarimetric technique could be applied to other cloudy planets, including gas giants and exoplanets, to detect gravity waves or other density perturbations above cloud decks that leave no trace in photometry.
  • Editorial inference: The paper's model makes a sharp, testable prediction: the ring signal should be strongest at phase angles near 90 degrees and stronger in the blue; a single well-placed observation at such geometry would decisively confirm or refute the atmospheric interpretation.
  • Editorial inference: The required density amplitude of 5-10% is substantial for internal gravity waves at those altitudes, so if confirmed, it would imply either unusually strong wave forcing or an alternative explanation such as organized aerosol variations that happen to mimic the same polarization signature.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

4 major / 5 minor

Summary. The paper analyzes a unique, serendipitous 36-minute ExPo imaging-polarimetry sequence of Venus taken on 24 May 2010. It reports faint, concentric, planet-wide ring-like patterns in the polarized flux (Stokes U) in the first three filter observations (H-alpha, H-alpha continuum, Na), while the later Na-continuum, Sloan r, and Sloan i frames show no such pattern. The total-flux images show no corresponding ring modulation. The authors use an adding-doubling radiative-transfer model with a four-layer Venus atmosphere containing gas, cloud, and haze to show that a 5-10% sinusoidal perturbation in the gas column density of the top layer can produce polarized-flux rings of the observed type while leaving total flux nearly unchanged. They interpret this as plausible evidence for planet-wide gravity waves above the cloud tops, but explicitly caution that the data cannot exclude an unknown instrumental artefact and that no repeat observation exists.

Significance. If the rings are astrophysical, the paper identifies a new observational signature of upper-atmospheric density waves on Venus that is invisible in conventional brightness imaging and accessible only through high-precision imaging polarimetry. The radiative-transfer modeling is a strength: it uses a fully polarimetric adding-doubling algorithm, a realistic cloud/haze model, wavelength-dependent CO2 Rayleigh scattering, and it demonstrates that the proposed density perturbations naturally produce a polarization signal without altering total flux. The paper is also commendably cautious: the abstract and conclusions repeatedly flag the single-epoch nature, the instrument's dismantling, and the inability to exclude artefacts. The inclusion of phase-screen seeing simulations to explore contrast loss in later exposures is a useful first step. However, the observational evidence is thin in specific, quantifiable ways: no per-pixel errors are given, the ring contrast is near the instrument's claimed sensitivity limit but not demonstrated for this data set, and the forward model is not an independent fit—its input parameters are derived from the observed pattern. The central claim therefore

major comments (4)
  1. [Sect. 2, Table 1, Figs. 3-4] The wavelength-dependence argument is compromised by the Na-continuum non-detection. Na (589.4 nm, 5 nm wide) shows clear rings at airmass 3.003-3.097, while Na-continuum (580.0 nm, 5 nm wide), observed only ~10 minutes later at airmass 3.419-3.542, shows none. The paper attributes this to seeing/airmass, but no quantitative seeing estimate or per-exposure degradation model is provided. The phase-screen computations (Sect. 5, Figs. 10-11) are explicitly illustrative and not calibrated to the actual time sequence. As presented, the detect/non-detect sequence could equally be explained by a time-dependent instrumental state. The phrase 'qualitatively consistent with the model prediction that sensitivity increases toward shorter wavelengths' (Sect. 4) overstates the support from this observation. Please either provide a quantitative seeing/airmass model that reproduces the Na detection and
  2. [Sect. 4.1, Fig. 8, Sect. 5] The forward model is not a fit; it is a plausibility demonstration. The injected perturbation amplitude (10%), radial wavelength profile (100-900 km), and center (20 degrees downwind of the sub-solar point) are all chosen from the observed pattern (Fig. 8). The resulting match in polarized flux is therefore by construction. The paper acknowledges this in Sect. 4.1, but the abstract and conclusion state that simulations 'show that rings in polarization can arise due to density variations of 5 to 10%'—this should be rephrased as 'are consistent with' or 'can plausibly be produced by'. To make the claim more robust, the authors should demonstrate that the qualitative result (rings in U, no rings in F) is insensitive to the assumed radial wavelength profile, amplitude, and center location, or at least quantify the range of parameters that produce a similar signature.
  3. [Sect. 2, Fig. 2, Sect. 3.2] No per-pixel error bars or noise maps are presented for the observed polarized flux. The ring contrast is stated as ~5e-4 in units of F_peak (Sect. 2, Fig. 2), while the instrument's polarimetric sensitivity of 1e-4 is quoted from laboratory or other observations (Sect. 3.2). The absolute calibration offset of 1-2% is irrelevant to relative spatial structure, but the spatial flat-field accuracy and per-pixel photon noise are directly relevant. Without an estimate of the pixel-to-pixel noise, the statistical significance of the 5e-4 modulation cannot be assessed. This is a load-bearing gap because the rings are faint and could be an artefact of the reduction. Please include noise maps, flat-field residuals, or at least a robust estimate of the per-pixel uncertainty for the U images.
  4. [Sect. 2 and Abstract] The paper's own statement that 'the present data do not allow us to exclude an unknown artefact completely' (Sect. 2) is the central limitation. Because ExPo was dismantled and no re-observation exists, the astrophysical interpretation is untestable with current data. This is not a flaw in the RT modeling, but it means the paper cannot claim a detection, however cautious. The abstract's phrasing 'We report observations of faint, concentric, planet-wide rings...' is slightly stronger than the evidence supports; the body correctly calls them 'a candidate signal'. I recommend the abstract and title more explicitly label the finding as a candidate or potential detection, and that the conclusion emphasize that confirmation requires new polarimetric observations with a calibrated, operational instrument.
minor comments (5)
  1. [Abstract and Sect. 2] Inconsistency: the abstract says 'faint (10^-6)' rings, while Sect. 2 states the typical difference in polarized flux inside/outside the brightest ring is 5e-4. Please clarify which quantity is 10^-6 (e.g., polarized flux in absolute units?) and which is 5e-4 (relative to F_peak?).
  2. [Eq. (13)] The symbol N_L (Loschmidt's number) is not defined in the text. Please define it explicitly.
  3. [Fig. 3 caption] The caption says 'The time sequence of the observations is from top left to bottom right: 5-6-1-2-3-4.' This is confusing because the top row is labeled Sloan r and Sloan i (observations 5 and 6), but the panels are described in a nonintuitive order. Please label each panel with its filter and time clearly, or reorder the figure to match the chronological sequence.
  4. [References] There are two entries for Travis 1979 in the reference list with the same DOI (10.1117/12.957426), but different titles and page numbers. Please merge or differentiate them.
  5. [Table 1 caption] The caption contains a typo: 'T able 1' instead of 'Table 1'.

Circularity Check

1 steps flagged

Modeled rings are partly constructed from the observed ring pattern; total-flux and wavelength cross-checks remain independent.

specific steps
  1. fitted input called prediction [Section 4.1 and Fig. 8 caption]
    "A sinusoidal variation in the gas column number density was spatially introduced to model the effect of a density wave travelling through the upper atmosphere of Venus (see lower sub-plots of Fig. 8). The amplitude of this variation was 10 % of the computed column gas density pertaining to this top most atmospheric layer. ... The model wavelengths (for the rings) were chosen to span the full range of gravity wave scales observed in Venus’ atmosphere, varying from about 900 km near the sub-solar (sub-observer) point to 100 km near the terminator."

    The model's input is effectively the observed ring morphology: the sinusoidal density perturbation's amplitude (10%), radial wavelength profile (100–900 km), and center (near/20° downwind of sub-solar) are all set from the ExPo ring pattern. The simulation then returns rings in polarized flux because rings were placed into the input; this agreement is partly by construction and does not independently validate the wave interpretation. The paper candidly frames the calculation as a plausibility check ('not to demonstrate that the observed pattern must be atmospheric in origin'), but the abstract still presents 'density variations of 5 to 10%' as the model's showing, which is a fitted-input demonstration rather than an independent prediction. The total-flux invariance and the Rayleigh-scatter

full rationale

The main circular step is confined to the forward-modeling section. The sinusoidal gas-density perturbation placed in the top atmospheric layer is spatially tuned to the observed rings—amplitude, wavelength profile, and center are taken from the data—so the simulated rings in polarized flux largely re-display the input pattern. This reduces the strength of the claim that the simulations 'show' the rings can be explained by gravity waves: they show that an input shaped like the observations can reproduce them. However, the paper repeatedly limits its claim ('present data do not allow us to exclude an unknown artefact completely', 'candidate signal', 'purpose ... is not to demonstrate ... but to assess'), which softens the circularity. Independent content remains in the model: the near-invariance of total flux and the wavelength scaling of the polarization response are genuine outputs not encoded in the assumed density pattern, and the seeing simulations add a separate consistency test. The self-citations to ExPo instrument papers are ordinary instrument-characterization references, not a load-bearing uniqueness theorem or an ansatz smuggled via citation. Overall, one or more derived claims reduce partly by construction, so a partial-circularity score of 6 is appropriate.

Axiom & Free-Parameter Ledger

4 free parameters · 4 axioms · 0 invented entities

The central simulation is a forward model: it injects a density perturbation whose amplitude, radial wavelength profile, and center are chosen to reproduce the observed rings. The total-flux invariance is a genuine cross-check, but the model's agreement in polarized flux is partly by construction. All cloud/haze microphysical inputs are inherited from prior Venus models rather than fitted here.

free parameters (4)
  • Gas density perturbation amplitude (delta N_m / N_m in top layer) = 10% (paper cites 5-10%)
    Hand-chosen to produce a polarization modulation of the observed order; no independent constraint, and the paper says the simulation is not a fit.
  • Radial wavelength profile of the imposed density perturbation = ~900 km near sub-solar point to ~100 km near terminator
    Set empirically to match ring spacing in the observations and prior gravity-wave literature; not derived from wave dynamics.
  • Center of the imposed concentric density pattern = ~20 degrees downwind of sub-solar point (approx. 2100 km; ~13:00 local time)
    Taken from the observed ring geometry rather than predicted; the simulation places the rings around this point.
  • Atmospheric seeing parameter S in phase-screen simulations = 0.5 arcseconds and 1.5 arcseconds
    Illustrative only; authors state the simulations are not a reconstruction of actual turbulence conditions.
axioms (4)
  • standard math The adding-doubling algorithm (de Haan et al. 1987) correctly models multiple scattering including linear and circular polarization.
    The simulated ring contrast and total-flux invariance depend on this RT code; treated as reliable from the literature.
  • domain assumption The four-layer model atmosphere (cloud optical thickness ~30, haze ~0.02, gas columns in Table 3) adequately represents Venus's upper atmosphere for this purpose.
    Values are taken from earlier Venus models (Kawabata, Sato, Rossi) and not optimized to the current data; the paper explicitly does not fit clouds/hazes.
  • domain assumption Molecular (CO2) Rayleigh scattering in the top layer is the dominant source of the polarization response to gas-density variations above the clouds.
    The mechanism relies on the contrast between singly scattered molecular light (polarized perpendicular to the scattering plane) and the cloud/haze background; this is the paper's physical interpretation.
  • ad hoc to paper A 5-10% gas-density perturbation above the cloud tops is physically plausible for a gravity wave.
    The paper states consistency with a gravity wave but does not derive the amplitude from wave dynamics or observations; it is a premise of the interpretation.

pith-pipeline@v1.3.0-alltime-deepseek · 16591 in / 14226 out tokens · 141076 ms · 2026-08-01T20:35:19.834812+00:00 · methodology

0 comments
read the original abstract

We report observations of faint ($10^{-6}$), concentric, planet-wide rings in the polarized flux of sunlight that is reflected by Venus, obtained during a serendipitous, 36-minute run in 2010, with the highly sensitive Extreme Polarimeter (ExPo) on the William Herschel Telescope. The rings appear to be centered slightly downwind of the sub-solar point, are visible in different filters across the visible, and are not obvious in the simultaneous total flux observations. ExPo's dual-beam exchange and double-differencing design strongly suppresses first-order instrumental polarization, and we could not identify an instrumental cause of the observed pattern. Because ExPo was dismantled before the rings were identified in the data, this is the only set of observations of these rings. We are therefore careful in claiming the detection of a new atmospheric phenomenon on Venus. However, numerical radiative transfer simulations show that planet-wide rings in polarization can arise due to density variations of 5 to 10% in the gas above the clouds, consistent with a gravity wave. Our simulations also show that such density variations would not show up in total flux observations. By presenting our observations and numerical simulations, we hope to motivate new polarimetric observations of Venus that could confirm or refute the presence of such planet-wide waves.

Figures

Figures reproduced from arXiv: 2607.16557 by Christoph Keller, Daphne M. Stam, Frans Snik, Gourav Mahapatra, Lo\"ic Rossi, Michiel Rodenhuis.

Figure 1
Figure 1. Figure 1: Venus as observed in total flux F (left) and polarized flux U (right) through the H-alpha continuum filter (see [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Equatorial cut through the H–alpha continuum observation shown in [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: The polarized flux (p Q2 + U2) as measured through the six filters (see [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: The background (red-orange) shows the degree of polarization as a function of longitude with respect to the sub–observer point (horizontal axis) and the latitude from -30◦ to +30◦ on Venus (vertical axis) as measured in the various filters, with the time of observation increasing from top to bottom (see [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: The direction of polarization as measured using the H-alpha cont. filter (λ0 = 647.1 nm). The orientation of the red lines indicates the polarization direction (note that the direction is not shown for every pixel to avoid cluttering), and the line length indicates the local degree of polarization, which is predominantly determined by the polarization signal of the lower atmospheric layers that contain the… view at source ↗
Figure 6
Figure 6. Figure 6: ExPo’s dual-beam exchange polarimetry technique. Calling the two states A and B (see 6) and denoting the two beams by L and R, the polarised flux is found through the double difference of four measurements: Q = AL − AR − BL + BR (5) [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: The flux (left) and degree of linear polarization P (right) of incident unpolarized light that is singly scattered by the cloud particles, haze particles, and gaseous molecules (solid black line) at the central wavelengths of the filters. Note that the wavelength dependence of the molecular scattering (through the depolarization factor, see Eq. 10) is so small that we show only one line. All flux curves ar… view at source ↗
Figure 8
Figure 8. Figure 8: The total flux (left) (normalized such that at a phase angle of 0◦ , the disk–integrated flux equals the planet’s geometric albedo) and degree of linear polarization (right) along Venus’ equator in response to changes in the gas column number density N m of the upper atmospheric layer for wavelengths covered by the filters (see [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Numerical computations corresponding to the candidate pattern in the H–alpha filter (λ0 = 656 nm), for the total flux (left) and the polarized flux (right). The background polarization signal has been subtracted from the latter. The decrease in spatial resolution due to the Earth’s atmosphere is not included. The planetary atmosphere is assumed to be horizontally homogeneous except for the gas density vari… view at source ↗
Figure 10
Figure 10. Figure 10: Numerical computations of the polarized flux Q in our Venus model in the H–alpha filter (λ0 = 656 nm) after the introduction of atmospheric seeing S (arcseconds). An atmospheric phase screen is applied to the fluxes in orthogonally polarized states, which are then recombined to obtain F and Q; the signed degree of linear polarization is computed as Ps = −Q/F (Eq. 4). Panels 2 and 3 show the progressive bl… view at source ↗
Figure 11
Figure 11. Figure 11: Illustrative 1D numerical computations of the effect of Earth atmospheric seeing S (arcseconds) on the modeled signed degree of linear polarization Ps in the H–alpha filter (λ0 = 656 nm). The atmosphere is assumed to be horizontally homogeneous except for the imposed gas-density variations. Increasing S progressively attenuates the wave-like modulation in Ps. These calculations are intended to illustrate … view at source ↗

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Reference graph

Works this paper leans on

298 extracted references · 29 canonical work pages

  1. [1]

    1992, title A mechanism for the Venus thermospheric superrotation, Geophysical research letters, 19, 2207

    Alexander, M. 1992, title A mechanism for the Venus thermospheric superrotation, Geophysical research letters, 19, 2207

    1992

  2. [2]

    1993, title Local time asymmetries in the Venus thermosphere, Journal of Geophysical Research: Planets, 98, 10849

    Alexander, M., Stewart, A., Solomon, S., & Boucher, S. 1993, title Local time asymmetries in the Venus thermosphere, Journal of Geophysical Research: Planets, 98, 10849

    1993

  3. [3]

    J., Smith, G

    Belton, M. J., Smith, G. R., Schubert, G., & Del Genio, A. D. 1976, title Cloud patterns, waves and convection in the Venus atmosphere, Journal of the Atmospheric Sciences, 33, 1394

    1976

  4. [4]

    1997, title Upper atmosphere dynamics: global circulation and gravity waves, Venus II: Geology, Geophysics, Atmosphere, and Solar Wind Environment, 259

    Bougher, S., Alexander, M., & Mayr, H. 1997, title Upper atmosphere dynamics: global circulation and gravity waves, Venus II: Geology, Geophysics, Atmosphere, and Solar Wind Environment, 259

    1997

  5. [5]

    Buscher, D. F. 2016, title Simulating large atmospheric phase screens using a woofer-tweeter algorithm, Optics express, 24, 23566

    2016

  6. [6]

    2011, title Data-reduction techniques for high-contrast imaging polarimetry-Applications to ExPo, Astronomy & Astrophysics, 531, A102

    Canovas, H., Rodenhuis, M., Jeffers, S., Min, M., & Keller, C. 2011, title Data-reduction techniques for high-contrast imaging polarimetry-Applications to ExPo, Astronomy & Astrophysics, 531, A102

    2011

  7. [7]

    1980, title Zonal and meridional circulation of the lower atmosphere of Venus determined by radio interferometry, Journal of Geophysical Research: Space Physics, 85, 8026

    Counselman, C., Gourevitch, S., King, R., Loriot, G., & Ginsberg, E. 1980, title Zonal and meridional circulation of the lower atmosphere of Venus determined by radio interferometry, Journal of Geophysical Research: Space Physics, 85, 8026

    1980

  8. [8]

    F., Bosma , P

    de Haan , J. F., Bosma , P. B., & Hovenier , J. W. 1987, title The adding method for multiple scattering calculations of polarized light , , 183, 371

    1987

  9. [9]

    A., & van der Stap , C

    de Rooij , W. A., & van der Stap , C. C. A. H. 1984, title Expansion of Mie scattering matrices in generalized spherical functions , , 131, 237

    1984

  10. [10]

    J., Mumma, M

    Goldstein, J. J., Mumma, M. J., Kostiuk, T., et al. 1991, title Absolute wind velocities in the lower thermosphere of Venus using infrared heterodyne spectroscopy, Icarus, 94, 45

    1991

  11. [12]

    E., & Travis , L

    Hansen , J. E., & Travis , L. D. 1974, title Light scattering in planetary atmospheres , Space Science Reviews, 16, 527

    1974

  12. [13]

    C., Marcq, E., et al

    Helbert, J., Vandaele, A. C., Marcq, E., et al. 2019, title The VenSpec suite on the ESA EnVision mission to Venus, in Infrared remote sensing and instrumentation XXVII, Vol. 11128, SPIE, 18--32

    2019

  13. [14]

    M., Colin, L., Donahue, T

    Hunten, D. M., Colin, L., Donahue, T. M., & Moroz, V. I. 2022, Venus (University of Arizona Press)

    2022

  14. [15]

    I., Titov , D

    Ignatiev , N. I., Titov , D. V., Piccioni , G., et al. 2009, title Altimetry of the Venus cloud tops from the Venus Express observations , Journal of Geophysical Research (Planets), 114, 0, 10.1029/2008JE003320

    doi:10.1029/2008je003320 2009

  15. [16]

    2012, title Direct imaging of a massive dust cloud around R Coronae Borealis, Astronomy & Astrophysics, 539, A56

    Jeffers, S., Min, M., Waters, L., et al. 2012, title Direct imaging of a massive dust cloud around R Coronae Borealis, Astronomy & Astrophysics, 539, A56

    2012

  16. [17]

    1988, title Wavelike perturbations observed in the neutral thermosphere of Venus, Journal of Geophysical Research: Space Physics, 93, 11237

    Kasprzak, W., Hedin, A., Mayr, H., & Niemann, H. 1988, title Wavelike perturbations observed in the neutral thermosphere of Venus, Journal of Geophysical Research: Space Physics, 93, 11237

    1988

  17. [18]

    1980, title Cloud and haze properties from Pioneer Venus polarimetry, Journal of Geophysical Research: Space Physics, 85, 8129

    Kawabata, K., Coffeen, D., Hansen, J., et al. 1980, title Cloud and haze properties from Pioneer Venus polarimetry, Journal of Geophysical Research: Space Physics, 85, 8129

    1980

  18. [19]

    C., Henson , G

    Kemp , J. C., Henson , G. D., Steiner , C. T., & Powell , E. R. 1987, title The optical polarization of the sun measured at a sensitivity of parts in ten million , Nature, 326, 270

    1987

  19. [20]

    M., et al

    Kitahara, T., Imamura, T., Sato, T. M., et al. 2019, title Stationary features at the cloud top of Venus observed by Ultraviolet Imager onboard Akatsuki, Journal of Geophysical Research: Planets, 124, 1266

    2019

  20. [21]

    2012, title SPICAV IR acousto-optic spectrometer experiment on Venus Express , Planetary and Space Science, 65, 38, 10.1016/j.pss.2012.01.002

    Korablev , O., Fedorova , A., Bertaux , J.-L., et al. 2012, title SPICAV IR acousto-optic spectrometer experiment on Venus Express , Planetary and Space Science, 65, 38, 10.1016/j.pss.2012.01.002

    work page doi:10.1016/j.pss.2012.01.002 2012

  21. [22]

    J., Munoz, A., Choi, Y.-J., et al

    Lee, Y. J., Munoz, A., Choi, Y.-J., et al. 2024, title Long-term Monitoring Plan of Venus using Earth-orbiting CubeSats,

    2024

  22. [23]

    S., & Suomi, V

    Limaye, S. S., & Suomi, V. E. 1981, title Cloud motions on Venus: Global structure and organization, Journal of the Atmospheric Sciences, 38, 1220

    1981

  23. [24]

    1988, title Gravity waves in the upper atmosphere of Venus, Journal of Geophysical Research: Space Physics, 93, 11247

    Mayr, H., Harris, I., Kasprzak, W., Dube, M., & Varosi, F. 1988, title Gravity waves in the upper atmosphere of Venus, Journal of Geophysical Research: Space Physics, 93, 11247

    1988

  24. [25]

    2011, title Oxygen airglow emission on Venus and Mars as seen by VIRTIS/VEX and OMEGA/MEX imaging spectrometers, Planetary and Space Science, 59, 981

    Migliorini, A., Altieri, F., Zasova, L., et al. 2011, title Oxygen airglow emission on Venus and Mars as seen by VIRTIS/VEX and OMEGA/MEX imaging spectrometers, Planetary and Space Science, 59, 981

    2011

  25. [26]

    V., Canovas, H., et al

    Min, M., Jeffers, S. V., Canovas, H., et al. 2013, title The color dependent morphology of the post-AGB star HD 161796, Astronomy & Astrophysics, 554, A15

    2013

  26. [27]

    2009, title Venus cloud top winds from tracking UV features in Venus Monitoring Camera images, Journal of Geophysical Research: Planets, 114

    Moissl, R., Khatuntsev, I., Limaye, S., et al. 2009, title Venus cloud top winds from tracking UV features in Venus Monitoring Camera images, Journal of Geophysical Research: Planets, 114

    2009

  27. [28]

    2023, Telescope Simulator,, https://github.com/dmortimer101/Telescope_Simulator GitHub

    Mortimer, D. 2023, Telescope Simulator,, https://github.com/dmortimer101/Telescope_Simulator GitHub

    2023

  28. [29]

    C., Bruinsma, S., Marty, J.-C., & Svedhem, H

    M \"u ller-Wodarg, I. C., Bruinsma, S., Marty, J.-C., & Svedhem, H. 2016, title In situ observations of waves in Venus’s polar lower thermosphere with Venus Express aerobraking, Nature Physics, 12, 767

    2016

  29. [30]

    C., De Cock, R., et al

    Neefs, E., Vandaele, A. C., De Cock, R., et al. 2024, title VenSpec-H spectrometer on the ESA EnVision mission: Design, modeling, analysis,

    2024

  30. [31]

    J., & Patel, I

    Newman, M., Schubert, G., Kliore, A. J., & Patel, I. R. 1984, title Zonal winds in the middle atmosphere of Venus from Pioneer Venus radio occultation data, Journal of the atmospheric sciences, 41, 1901

    1984

  31. [32]

    2017, title Stationary waves and slowly moving features in the night upper clouds of Venus, Nature Astronomy, 1, 0187, 10.1038/s41550-017-0187

    Peralta, J., Hueso, R., S \' a nchez-Lavega, A., et al. 2017, title Stationary waves and slowly moving features in the night upper clouds of Venus, Nature Astronomy, 1, 0187, 10.1038/s41550-017-0187

    doi:10.1038/s41550-017-0187 2017

  32. [33]

    2015, Venus thermosphere densities as revealed by Venus Express torque and accelerometer data,

    Persson, M. 2015, Venus thermosphere densities as revealed by Venus Express torque and accelerometer data,

    2015

  33. [34]

    V., Sanchez-Lavega, A., et al

    Piccialli, A., Titov, D. V., Sanchez-Lavega, A., et al. 2014, title High latitude gravity waves at the Venus cloud tops as observed by the Venus Monitoring Camera on board Venus Express, Icarus, 227, 94

    2014

  34. [35]

    2012, title The extreme polarimeter: design, performance, first results and upgrades, in Ground-based and Airborne Instrumentation for Astronomy IV, Vol

    Rodenhuis, M., Canovas, H., Jeffers, S., et al. 2012, title The extreme polarimeter: design, performance, first results and upgrades, in Ground-based and Airborne Instrumentation for Astronomy IV, Vol. 8446, SPIE, 1413--1430

    2012

  35. [36]

    2008, title The Extreme Polarimeter (ExPo): design of a sensitive imaging polarimeter, in Ground-based and Airborne Instrumentation for Astronomy II, Vol

    Rodenhuis, M., Canovas, H., Jeffers, S., & Keller, C. 2008, title The Extreme Polarimeter (ExPo): design of a sensitive imaging polarimeter, in Ground-based and Airborne Instrumentation for Astronomy II, Vol. 7014, International Society for Optics and Photonics, 70146T

    2008

  36. [37]

    Rodenhuis , M., & Keller , C. U. 2007, title Design Options for the Extreme Polarimeter (ExPo) , in Proceedings of the conference In the Spirit of Bernard Lyot: The Direct Detection of Planets and Circumstellar Disks in the 21st Century. June 04 - 08, 2007. University of California, Berkeley, CA, USA. Edited by Paul Kalas., ed. P. Kalas , 43--+

    2007

  37. [38]

    2015, title Preliminary study of Venus cloud layers with polarimetric data from SPICAV/VEx, Planetary and Space Science, 113, 159

    Rossi, L., Marcq, E., Montmessin, F., et al. 2015, title Preliminary study of Venus cloud layers with polarimetric data from SPICAV/VEx, Planetary and Space Science, 113, 159

    2015

  38. [39]

    , & Stam, D

    Rossi, L. , & Stam, D. M. 2018, title Circular polarization signals of cloudy (exo)planets, A&A, 616, A117, 10.1051/0004-6361/201832619

    work page doi:10.1051/0004-6361/201832619 2018

  39. [40]

    1996, title Photopolarimetry Analysis of the Venus Atmosphere in Polar Regions , Icarus, 124, 569, 10.1006/icar.1996.0231

    Sato , M., Travis , L., & Kawabata , K. 1996, title Photopolarimetry Analysis of the Venus Atmosphere in Polar Regions , Icarus, 124, 569, 10.1006/icar.1996.0231

    arXiv 1996

  40. [41]

    2005, title Direct measurement of the Rayleigh scattering cross section in various gases , J

    Sneep , M., & Ubachs , W. 2005, title Direct measurement of the Rayleigh scattering cross section in various gases , J. Quant. Spectrosc. Radiative Transfer, 92, 293, 10.1016/j.jqsrt.2004.07.025

    doi:10.1016/j.jqsrt.2004.07.025 2005

  41. [42]

    1999, title Degree of linear polarization of light emerging from the cloudless atmosphere in the oxygen A band, Journal of Geophysical Research: Atmospheres, 104, 16843

    Stam, D., De Haan, J., Hovenier, J., & Stammes, P. 1999, title Degree of linear polarization of light emerging from the cloudless atmosphere in the oxygen A band, Journal of Geophysical Research: Atmospheres, 104, 16843

    1999

  42. [44]

    Travis, L. D. 1979, Imaging And Polarimetry With The Pioneer Venus Orbiter Cloud Photopolarimeter, 10.1117/12.957426

    work page doi:10.1117/12.957426 1979

  43. [45]

    Long-term Monitoring Plan of Venus using Earth-orbiting CubeSats , author=

  44. [46]

    , keywords =

    Determination of Rayleigh scattering cross sections and indices of refraction for Ar, CO _ 2 , SF _ 6 , and CH _ 4 using BBCES in the ultraviolet. , keywords =. doi:10.1016/j.jqsrt.2020.107224 , adsurl =

    arXiv 2020

  45. [47]

    Infrared Remote Sensing and Instrumentation XXXII , volume=

    Design of the VenSpec-U instrument: a double UV imaging spectrometer to analyze sulfured gases in the Venus’ atmosphere , author=. Infrared Remote Sensing and Instrumentation XXXII , volume=. 2024 , organization=

    2024

  46. [48]

    Infrared remote sensing and instrumentation XXVII , volume=

    The VenSpec suite on the ESA EnVision mission to Venus , author=. Infrared remote sensing and instrumentation XXVII , volume=. 2019 , organization=

    2019

  47. [49]

    Nature , volume=

    Variable oxygen airglow on Venus as a probe of atmospheric dynamics , author=. Nature , volume=. 1992 , publisher=

    1992

  48. [50]

    Icarus , volume=

    Photochemistry of the stratosphere of Venus: Implications for atmospheric evolution , author=. Icarus , volume=. 1982 , publisher=

    1982

  49. [51]

    Monthly Notices of the Royal Astronomical Society , volume=

    Chasing rainbows and ocean glints: Inner working angle constraints for the Habitable Worlds Observatory , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2023 , publisher=

    2023

  50. [52]

    Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray , volume=

    The science case for POLLUX: a high-resolution UV spectropolarimeter onboard LUVOIR , author=. Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray , volume=. 2018 , organization=

    2018

  51. [53]

    The Astronomy and Astrophysics Review , volume=

    Polarimetry of Solar System minor bodies and planets , author=. The Astronomy and Astrophysics Review , volume=. 2024 , publisher=

    2024

  52. [54]

    Icarus , volume=

    First ever in situ observations of Venus’ polar upper atmosphere density using the tracking data of the Venus Express Atmospheric Drag Experiment (VExADE) , author=. Icarus , volume=. 2012 , publisher=

    2012

  53. [55]

    VenSpec-H spectrometer on the ESA EnVision mission: Design, modeling, analysis , author=

  54. [56]

    Science , volume=

    How waves and turbulence maintain the super-rotation of Venus’ atmosphere , author=. Science , volume=. 2020 , publisher=

    2020

  55. [57]

    Astronomy and Astrophysics-A&A , volume=

    From exo-Earths to exo-Venuses: Flux and polarization signatures of reflected light , author=. Astronomy and Astrophysics-A&A , volume=

  56. [58]

    The Planetary Science Journal , volume=

    Polarimetry as a tool for observing orographic gravity waves on venus , author=. The Planetary Science Journal , volume=. 2021 , publisher=

    2021

  57. [59]

    Nature geoscience , volume=

    Variations of sulphur dioxide at the cloud top of Venus’s dynamic atmosphere , author=. Nature geoscience , volume=. 2013 , publisher=

    2013

  58. [60]

    Space Science Reviews , volume=

    Composition and chemistry of the neutral atmosphere of Venus , author=. Space Science Reviews , volume=. 2018 , publisher=

    2018

  59. [61]

    Icarus , volume=

    Temporal variability of ultraviolet cloud features in the Venus stratosphere , author=. Icarus , volume=. 1982 , publisher=

    1982

  60. [62]

    Spatial and temporal variability , author=

    Sulfur dioxide in the Venus Atmosphere: II. Spatial and temporal variability , author=. Icarus , volume=. 2017 , publisher=

    2017

  61. [63]

    Experimental Astronomy , volume=

    Venus: Key to understanding the evolution of terrestrial planets , author=. Experimental Astronomy , volume=. 2022 , publisher=

    2022

  62. [64]

    arXiv preprint arXiv:1703.09010 , year=

    EnVision: understanding why our most Earth-like neighbour is so different , author=. arXiv preprint arXiv:1703.09010 , year=

    Pith/arXiv arXiv

  63. [65]

    Space Science Reviews , volume=

    Clouds and hazes of Venus , author=. Space Science Reviews , volume=. 2018 , publisher=

    2018

  64. [66]

    Astronomy & Astrophysics , volume=

    Ocean signatures in the total flux and polarization spectra of Earth-like exoplanets , author=. Astronomy & Astrophysics , volume=. 2022 , publisher=

    2022

  65. [67]

    Space Science Reviews , volume=

    Synergies Between Venus & Exoplanetary Observations: Venus and Its Extrasolar Siblings , author=. Space Science Reviews , volume=. 2023 , publisher=

    2023

  66. [68]

    American Astronomical Society Meeting Abstracts\# 215 , volume=

    Transiting exoplanet survey satellite (tess) , author=. American Astronomical Society Meeting Abstracts\# 215 , volume=

  67. [69]

    Burgess, Ebenezer and Gangooly, Phanindralal , year=. S

  68. [70]

    Astronomy & Astrophysics , volume=

    The color dependent morphology of the post-AGB star HD 161796 , author=. Astronomy & Astrophysics , volume=. 2013 , publisher=

    2013

  69. [71]

    Astronomy & Astrophysics , volume=

    Direct imaging of a massive dust cloud around R Coronae Borealis , author=. Astronomy & Astrophysics , volume=. 2012 , publisher=

    2012

  70. [72]

    Ground-based and Airborne Instrumentation for Astronomy IV , volume=

    The extreme polarimeter: design, performance, first results and upgrades , author=. Ground-based and Airborne Instrumentation for Astronomy IV , volume=. 2012 , organization=

    2012

  71. [73]

    , author=

    Cosmotheoros: or, Conjectures concerning the inhabitants of the planets: Translated from the Latin of Christian Huygens.. , author=. 1762 , publisher=

  72. [74]

    Planetary and Space Science , volume=

    SPICAV IR acousto-optic spectrometer experiment on Venus Express , author=. Planetary and Space Science , volume=. 2012 , publisher=

    2012

  73. [75]

    Planetary and Space Science , volume=

    SPICAV on Venus Express: Three spectrometers to study the global structure and composition of the Venus atmosphere , author=. Planetary and Space Science , volume=. 2007 , publisher=

    2007

  74. [76]

    Journal of Geophysical Research: Planets , volume=

    Venus express mission , author=. Journal of Geophysical Research: Planets , volume=. 2009 , publisher=

    2009

  75. [77]

    Planetary and Space Science , volume=

    Venus Express—the first European mission to Venus , author=. Planetary and Space Science , volume=. 2007 , publisher=

    2007

  76. [78]

    Planetary and Space Science , volume=

    Scientific goals for the observation of Venus by VIRTIS on ESA/Venus Express mission , author=. Planetary and Space Science , volume=. 2007 , publisher=

    2007

  77. [79]

    Planetary and Space Science , volume=

    Venus Express science planning , author=. Planetary and Space Science , volume=. 2006 , publisher=

    2006

  78. [80]

    Journal of Geophysical Research: Planets , volume=

    Analysis of temporal variations of the polarization of Venus observed by Pioneer Venus Orbiter , author=. Journal of Geophysical Research: Planets , volume=. 1998 , publisher=

    1998

  79. [81]

    Journal of Atmospheric Sciences , volume=

    Planetary-scale waves and the cyclic nature of cloud top dynamics on Venus , author=. Journal of Atmospheric Sciences , volume=

  80. [82]

    Journal of Geophysical Research: Space Physics , volume=

    Structure and circulation of the Venus atmosphere , author=. Journal of Geophysical Research: Space Physics , volume=. 1980 , publisher=

    1980

Showing first 80 references.