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REVIEW 3 major objections 3 minor 88 references

Exploration of new experimental strategies for the detection of ultralight dark matter : laboratory searches on ground and in space

T0 review · 3 major / 3 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read A spherical dish antenna will not focus all dark-photon power at its center; the received power can be only a few percent of the emitted power.

desk verdict A genuinely useful thesis whose central new result — the dish-antenna power correction — is plausible but needs a full-wave check before the field adopts it. read the letter →

arxiv 2411.14128 v1 pith:CFYYJ5N5 submitted 2024-11-21 hep-ph gr-qc

Jordan Gué This is my paper · ORCID
classification hep-phgr-qc
keywords ultralightdarkmatterphotondishantennaKirchhoffintegralequivalenceprincipleatominterferometryLISAaxion-photoncoupling
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

Ultralight dark matter candidates below 1 eV produce small oscillating signals—electric fields, mass oscillations, or polarization rotation—that existing detectors may be able to see with the right modeling. This thesis builds theoretical models for several of those detectors and derives sensitivity estimates. Its sharpest result is that the standard assumption for dish antennas, namely that all power emitted by a spherical dish is focused at the curvature center, is too optimistic. Using a Kirchhoff propagation calculation, the thesis finds that the received power depends on the dark photon Compton frequency and can be only a few percent of the emitted power even when the dish radius is more than ten times the wavelength. The same framework also yields phase-shift formulas for optical cavities and fibers, a Rydberg-atom microwave-cavity scheme for dark photons, and a Bayesian analysis for distinguishing ultralight dark matter from gravitational waves in LISA.

What carries the argument

The central object is the Kirchhoff integral with a Dirichlet Green function, used to propagate the electric field emitted by a spherical dish: the dish is treated as a thin optical element that imprints a phase factor $e^{ikf(\rho)}$ on the field (Eq. (11.7)), and the field is then propagated from the closing plane to the receiver via Eq. (11.15). This two-step decomposition makes an analytical calculation possible, since no Dirichlet Green function for a portion of a sphere is known. Supporting machinery includes the dilaton and axion 'charges' that relate atomic mass and frequency oscillations to couplings, and the quadratic Stark effect in Rydberg atoms used to measure the squared total field in the cavity scheme.

What would settle it

Build a tabletop spherical reflector with radius $r$ an order of magnitude larger than the wavelength and a source at its curvature center, then measure the power at the receiver at several frequencies; matching the full-focus formula of the standard assumption rather than the Kirchhoff prediction of Eq. (11.15) would falsify the thesis's dish result.

Watch

Extended reading notes

Core claim

The central claim is that the standard full-focus assumption for dish-antenna dark photon searches is wrong. The thesis derives, in Chapter 11, the electric field at a receiver placed at the curvature center of a spherical dish by propagating the field in two steps: first from the dish to a closing plane with the thin optical element approximation, then from that plane to the receiver with an exact Kirchhoff integral and a Dirichlet Green function. The result, Eq. (11.15), shows that the focused power is a strong function of the dark photon Compton frequency; for dish radii well above the wavelength it can fall to a few percent of the emitted power. The thesis also establishes complementary results: an optical-cavity phase shift from axion birefringence that is independent of laser frequency and resonantly enhanced at even modes, a microwave-cavity signal linear in the dark photon kinetic mixing and amplified near odd resonances, and concrete sensitivity projections for atom interferometry, equivalence-principle tests, and LISA.

Load-bearing premise

The load-bearing premise is that the dish can be treated as a thin optical element, requiring its radius to be much smaller than its curvature radius and transverse field modes to be much smaller than the longitudinal wavevector; if a realistic spherical dish violates these conditions, the few-percent focusing result may change.

Editorial extensions

If this is right

  • Dish-antenna exclusion limits that assume full focusing will need revision; the true sensitivity is frequency-dependent and may be worse by more than an order of magnitude in the affected mass range.
  • The proposed Rydberg-atom microwave-cavity experiment can scan a continuous band of dark photon masses by sweeping the applied field frequency, with the signal enhanced by the cavity quality factor near odd resonances.
  • For axion-photon searches, the optical-cavity phase-shift formula gives a signal independent of the laser frequency, so the same cavity can probe a broad range of axion masses near even modes rather than a single resonant frequency.
  • In LISA, a Bayesian likelihood that discriminates oscillating-mass dark matter signals from gravitational waves yields realistic sensitivity limits on scalar and vector couplings, including cases where the two signals overlap.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Editorial extension: if the dish result holds, reanalysing past dish-antenna limits with the Kirchhoff efficiency curve would be a direct test of whether any excluded dark-photon parameter space actually remains open.
  • Editorial extension: the same two-step Kirchhoff method could be applied to other curved emitters, such as parabolic dishes or lens-coupled receivers, where the thin optical element approximation may be better or worse controlled.
  • Editorial extension: a tabletop radio-frequency analogue with a point source and spherical reflector would measure the focusing efficiency as a function of $R/r$ and wavelength, giving a clean laboratory check of the few-percent prediction.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 3 minor

Summary. This PhD thesis investigates experimental strategies for detecting ultralight dark matter (ULDM), focusing on three phenomenologies: dark-photon kinetic mixing with electromagnetism (probed with cavities, Rydberg atoms, and dish antennas), scalar/axion couplings that oscillate atomic masses and transition frequencies (probed with equivalence-principle tests, atom interferometry, and LISA), and axion-photon coupling effects such as vacuum birefringence and dichroism (probed with optical cavities, fibers, and LISA). The manuscript derives signal amplitudes and estimates sensitivities for these schemes. Its most distinctive new claim, developed in Chapter 11, is that for dish antennas the dark-photon-induced field is not fully focused at the curvature center: the power received there can be only a few percent of the emitted power, even when the dish radius exceeds the wavelength by more than an order of magnitude. This is presented as a correction to the standard assumption quoted from Ref. [10] that the emitted power is entirely focused at the curvature center.

Significance. If correct, the dish-antenna result would materially affect the design and sensitivity projections of dish-based dark-photon searches, including experiments of the SHUKET/FUNK type. The thesis also contains useful derivations for optical-cavity and fiber searches for axion-photon coupling, a Rydberg-atom microwave-cavity detection scheme for dark photons, and a framework for LISA-based searches. Strengths include the explicit statement of approximations, the use of standard astrophysical inputs (local density, velocity distribution, coherence time, stochastic amplitude correction), and forward sensitivity projections rather than fits. However, the central dish claim rests on a two-step approximate Green-function calculation whose validity is not independently established, and the sensitivity chapters and appendices were not available in the provided text, so the projected sensitivity curves could not be checked.

major comments (3)
  1. [Section 11.2, Eqs. (11.7), (11.10), (11.15)] The chapter's central claim—that the power received at the curvature center is only a few percent of P_emit even for r/λ>10—is obtained by replacing the spherical dish with a thin phase screen (Eq. (11.7), stated in Section 11.2.2 to be valid only for r<<R) and then propagating from the fictional plane using the Dirichlet Green function of an infinite plane (Eqs. (11.10)-(11.15)). The second step is equivalent to diffraction by an aperture in an opaque screen: the field on the fictional plane outside the projected disk is set to zero. There is no physical screen in the actual setup, and the boundary condition is only on the dish surface. The manuscript itself states in Section 11.2.1 that no exact analytical solution for the spherical geometry exists, and realistic dish antennas can have r comparable to R, outside the stated validity of the phase-screen approximation. The stress-test concern about the opaque-plane model is partly legitimate: while the phase factor e^{ikf} in Eq. (11.7) preserves the constant optical path to the curvature center in the paraxial limit, the artificial zero boundary condition on the fictional plane outside the disk is an unvalidated modeling choice that can alter the diffracted field and the power coupled into the receiver. I therefore ask for an independent quantitative validation (for example, a full-wave or boundary-integral calculation for a spherical cap with the relevant f-number) and for an assessment of how much the sensitivity projections in Chapter 18 change under this modeling uncertainty.
  2. [Chapters 15-18 and Appendices A-E] The text made available for review stops at Section 11.3.1. The sensitivity estimates in Chapter 18 and the supporting derivations in Appendices A-E, including the phase-shift derivation leading to Eq. (9.7) and the cavity-field derivation leading to Eq. (10.12), are therefore not checkable from the provided material. Since those sensitivity projections are a central output of the thesis, the complete manuscript should be supplied, and every equation used to produce a sensitivity curve should be derivable either in the main text or in an appendix.
  3. [Section 11.1 and Section 11.3] The phrase "power received at the curvature center" is not precisely defined in the available text. Section 11.1 defines emitted power P_emit (Eq. (11.2)), and Section 11.3 begins a mode-overlap calculation for a horn antenna, but the relation between the electric field from Eq. (11.15), the total power crossing a detector plane, and the power actually coupled into the antenna mode is not stated. The chapter's headline correction to Ref. [10] ("only a few percent of emitted power") depends on this relation; without it, the reader cannot tell whether the suppression is a propagation effect, a detection-efficiency effect, or both.
minor comments (3)
  1. [Section 11.2.2, after Eq. (11.8)] The notation Δx, Δy for the dish extent is introduced without definition; the order-of-magnitude estimate p~q~1/Δx~1 m^-1 should be stated in terms of the dish radius r and the angular aperture r/R.
  2. [Eq. (9.7)] As typeset, the fraction containing sqrt(1−2r^2 cos(2ω_aℓ/c)+r^4) and sin^2(ω_aℓ/(2c)) is ambiguous; please check the equation image in the arXiv source.
  3. [Fig. 11.1 and Section 11.2.1] The caption states that the closing surfaces A2 and A3 are chosen so that their contributions vanish at the curvature center; since Eq. (11.15) is used for general receiver positions, the text should explain why those contributions can be neglected at the receiver location actually considered.

Circularity Check

0 steps flagged · score 0.0 of 10

Self-contained forward sensitivity calculations; no circular step identified.

full rationale

The thesis is a forward-calculation pipeline. Couplings such as chi, g_agamma, d_e, and d_g are free parameters that are scanned, not fitted to the target signals. The amplitudes of the ULDM fields are fixed by the stated local density and velocity distribution (Eqs. 7.17 and 7.26), which are external inputs, and the signals are then propagated through Maxwell and Klein-Gordon equations in standard ways. The sensitivity estimates in Chapters 17-18 compare predicted signal power spectral densities to experimental noise models, so the 'predictions' are not obtained by construction from the fitted parameters. The self-citations that appear, notably the published versions of the cavity and dish proposals, are pointers to the same derivations presented in the thesis and are not load-bearing justifications. The strongest new claim, the dish-antenna result of Chapter 11, rests on the thin optical element approximation of Eq. (11.7) and the Dirichlet Green function propagation of Eq. (11.15); these are stated approximations with stated validity conditions (p,q << k and r << R), and the resulting few-percent power estimate follows from integrating the assumed source field rather than by circular reduction. The thesis itself acknowledges that no exact analytical solution exists for the spherical dish, which is a legitimate model-risk caveat, but it is not a circularity. Overall, the derivation chain is self-contained and no specific step reduces to its own inputs.

Assumptions & free parameters 3 free parameters · 4 assumptions · 0 invented entities

The paper introduces no new particles; it reuses dark photons, axions, and dilatons from prior literature. The listed inputs are externally fitted parameters and stated modeling assumptions. The main cost is the monochromatic-field approximation and the thin-element dish approximation.

free parameters (3)
  • Local dark matter energy density rho_DM = 0.4 GeV/cm^3
    From McMillan 2011 (cited as [37]); sets the ULDM field amplitude in Eq. (7.17) and therefore all signal amplitudes and sensitivity curves.
  • Galactic dark matter mean velocity v_DM and velocity dispersion sigma_v = v_DM = 3e5 m/s; sigma_v = 1.5e5 m/s
    From Evans et al. 2019 (cited as [39]); determines the coherence time in Eq. (5.11), frequency broadening, and gradient projections used in sensitivity estimates.
  • Stochastic amplitude correction factor for T_obs much less than tau = 1.51 at 68% confidence
    Taken from Centers et al. 2021 (cited as [45]); the thesis applies this to monochromatic signals and notes in a footnote that gradient couplings require case-by-case treatment.
assumptions (4)
  • domain assumption The ULDM field oscillates as a classical coherent field with amplitude fixed by rho_DM and behaves as cold dark matter.
    Section 7.3 derives the energy density and pressure; the identification rho = rho_DM is used in all sensitivity chapters.
  • domain assumption The field is monochromatic and spatially homogeneous over each experiment; velocity dispersion is neglected except through the coherence time.
    Sections 5.3.3 and 7.4 state this simplification and give the validity condition in Eq. (7.28).
  • ad hoc to paper For the dish calculation, the spherical dish can be treated as a thin optical element with transverse modes much smaller than the longitudinal wavevector and radius much smaller than curvature radius.
    Section 11.2.2 introduces Eq. (11.7) under these conditions because no exact analytical Kirchhoff solution exists for a spherical dish (Section 11.2.1).
  • domain assumption The scalar and axion couplings to matter are described by the low-energy linear Lagrangians Eq. (8.1) and Eq. (8.16), with atom charge tables computed in the cited literature.
    Chapter 8 builds all phenomenology from these Lagrangians and from the Damour-Donoghue and Kim-Perez results.

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Pith. "Pith review of Exploration of new experimental strategies for the detection of ultralight dark matter : laboratory searches on ground and in space." pith.science (2026). https://pith.science/paper/CFYYJ5N5

@misc{pith2026241114128,
  author       = {Pith},
  title        = {Pith review of: Exploration of new experimental strategies for the detection of ultralight dark matter : laboratory searches on ground and in space},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/CFYYJ5N5}},
  note         = {Machine review of arXiv:2411.14128}
}
read the original abstract

Ultralight dark matter (ULDM), as a class of low mass (< 1 eV) dark matter (DM) candidates, is a compelling alternative to historically dominant models such as WIMPs and has recently gained significant attention in the scientific community. In this thesis, we study various experimental schemes for the direct detection of ULDM, both on ground and in space. More precisely, we propose a theoretical modeling of current and futuristic experiments, and we derive an estimation of their respective sensitivity. We mainly concentrate on three distinct phenomenologies. The first one is the coupling between a DM U(1) field, known as the dark photon (DP), and electromagnetism, which induces a small electric field oscillating at the DP Compton frequency. We study how to detect this electric field using atoms inside a cavity and through dish antennas. The second main phenomenology considered in this thesis is the oscillation of rest mass and transition frequencies of atoms and test masses. These oscillations could be produced by the non-universal coupling of standard matter with a scalar ULDM candidate (dilaton or axion-like particle). We study how to detect such couplings in classical tests of the universality of free fall (UFF), atom interferometry and using LISA. Finally, we study the effect of vacuum birefringence and dichroism induced by the coupling between axions and photons, and how it could be detected with optical cavities, fibers, and LISA.

Figures

Figures reproduced from arXiv: 2411.14128 by the authors.

Figure 4.1
Figure 4.1. All fundamental particles of the Standard Model (with the hypothetical graviton), [PITH_FULL_IMAGE:figures/full_fig_p019_4_1.png] view at source ↗
Figure 5.1
Figure 5.1. Velocity profile of the NGC 6503 galaxy (from [ [PITH_FULL_IMAGE:figures/full_fig_p022_5_1.png] view at source ↗
Figure 5.2
Figure 5.2. Composite image of the bullet cluster, where the blue area shows the gravita [PITH_FULL_IMAGE:figures/full_fig_p023_5_2.png] view at source ↗
Figures from the paper (31 more)
Figure 5.3
Figure 5.3. Figure 5.3: Mass scale of DM candidates, from massive primordial black holes to the light [PITH_FULL_IMAGE:figures/full_fig_p024_5_3.png]
Figure 10.1
Figure 10.1. Figure 10.1: Experimental scheme that we propose for the search of the DP-photons coupling [PITH_FULL_IMAGE:figures/full_fig_p073_10_1.png]
Figure 10.2
Figure 10.2. Figure 10.2: Signal contribution Eq. (10.12a) (arb. units) as function of 𝜔𝑈 , 𝜔𝐴, both presented in units of 𝑐/𝐿. The resonance peaks appear clearly when both frequencies correspond to an odd mode of the cavity. plots of the signal contribution Eq. (10.12a) as function of the a…
Figure 11.1
Figure 11.1. Figure 11.1: The oscillating standing DP electric field [PITH_FULL_IMAGE:figures/full_fig_p083_11_1.png]
Figure 11.2
Figure 11.2. Figure 11.2: To compute the electric field induced by the dish at a location [PITH_FULL_IMAGE:figures/full_fig_p085_11_2.png]
Figure 11.3
Figure 11.3. Figure 11.3: Rectangular horn antenna and definition of its physical surface aperture. Therefore, in a coordinate system with the 𝑧-axis perpendicular to the surface aperture of the an￾tenna, as shown in [PITH_FULL_IMAGE:figures/full_fig_p088_11_3.png]
Figure 13.1
Figure 13.1. Figure 13.1: On the left, scheme of the two photon Raman transition considered in the present [PITH_FULL_IMAGE:figures/full_fig_p100_13_1.png]
Figure 13.2
Figure 13.2. Figure 13.2: The various phase contributions along the AI path : in orange are the propagation [PITH_FULL_IMAGE:figures/full_fig_p101_13_2.png]
Figure 13.3
Figure 13.3. Figure 13.3: Simple scheme on the com￾putation of the time of emission of pho￾tons from both lasers. To compute the laser phase, we need to know the different times 𝑡𝑖 of emission of photons. For a given interaction time 𝑡int, they are given by (see [PITH_FULL_IMAGE:figures/ful…
Figure 13.4
Figure 13.4. Figure 13.4: Spacetime diagram of a single photon transition, as proposed in [ [PITH_FULL_IMAGE:figures/full_fig_p112_13_4.png]
Figure 13.5
Figure 13.5. Figure 13.5: Spacetime diagram of a gradiometer, where two interferometers as shown in [PITH_FULL_IMAGE:figures/full_fig_p113_13_5.png]
Figure 13.6
Figure 13.6. Figure 13.6: Simplified setup for the SPID experiment. For the sake of simplicity, we assume two different isotopes with respective transition frequencies 𝑓1 = 𝑓tr = 1014 Hz, 𝑓2 = 𝑓tr + 𝑓EOM = (1 + 10−5 ) × 1014 Hz. The laser is locked on the transition frequency of isotope 1 an…
Figure 14.1
Figure 14.1. Figure 14.1: LISA constellation heliocentric orbit (from [4]). 14.2 LISA, the first european space-based gravitational waves detector After the success of the ground-based GW detectors such as LIGO and VIRGO, one of the next important mission aiming at detecting GW is LISA (Lase…
Figure 15.1
Figure 15.1. Figure 15.1: Amplitude of transfer functions of TDI 𝑋 combinations for both scalar ULDM (in blue) and GW (in orange) from Eqs. (15.8) and (15.16a) respectively. For this plot, we neglected the impact of the geometric factors. where 𝑤ℓ = ±1 respectively for ℓ = 3, 2. One can simp…
Figure 15.2
Figure 15.2. Figure 15.2: Results of the fit of a galactic binary signal by a galactic binary model. The [PITH_FULL_IMAGE:figures/full_fig_p139_15_2.png]
Figure 15.3
Figure 15.3. Figure 15.3: GW signal PSD (in lime) com￾pared to LISA noise PSD of the TDI 𝐴 combi￾nation (in red) in Fourier domain. The signal is well above the noise. We also show the 𝑟GW,GW residuals power in grey, which are below the noise. 10 3 10 2 × 10 3 3 × 10 3 4 × 10 3 6 × 10 3 2 f …
Figure 15.5
Figure 15.5. Figure 15.5: Results of the fit of the DM signal by a DM model. The yellow lines indicate [PITH_FULL_IMAGE:figures/full_fig_p144_15_5.png]
Figure 15.6
Figure 15.6. Figure 15.6: DM signal PSD (in lime) com￾pared to LISA noise PSD of TDI 𝐴 combina￾tion (in red) in Fourier domain (as in [PITH_FULL_IMAGE:figures/full_fig_p146_15_6.png]
Figure 15.8
Figure 15.8. Figure 15.8: Joint likelihood ℒ(𝑣 𝑀 DM, 𝜀 𝑀) for the data parameters shown in [PITH_FULL_IMAGE:figures/full_fig_p151_15_8.png]
Figure 16.1
Figure 16.1. Figure 16.1: Simplified optical benches in LISA spacecrafts. The two optical benches 𝐴 and 𝐵 are inside two different spacecrafts (shown as the light green cube) and exchange light between each other. The optical elements are shown in blue, the light polarization in red and the …
Figure 16.2
Figure 16.2. Figure 16.2: Two optical benches are present in each spacecraft which permits six individual interference measurements at each time. Fol￾lowing our arbitrary choice on light polariza￾tion in [PITH_FULL_IMAGE:figures/full_fig_p155_16_2.png]
Figure 16.3
Figure 16.3. Figure 16.3: Modified optical bench inside LISA spacecraft, compared to the original one presented in [PITH_FULL_IMAGE:figures/full_fig_p159_16_3.png]
Figure 16.4
Figure 16.4. Figure 16.4: LISA proposed modified constellation for the search of vac￾uum birefringence, as a consequence of [PITH_FULL_IMAGE:figures/full_fig_p161_16_4.png]
Figure 18.1
Figure 18.1. Figure 18.1: Current constraints on all the dilatonic couplings of interest in this thesis : [PITH_FULL_IMAGE:figures/full_fig_p182_18_1.png]
Figure 18.2
Figure 18.2. Figure 18.2: On the left, we show the sensitivity of LISA to the general coupling 𝜀min when the velocity is assumed fixed (blue curve) and when it is a free parameter (orange curve). One can notice a deterioration of the sensitivity when the velocity is a free parameter of the B…
Figure 18.3
Figure 18.3. Figure 18.3: Current lab constraints on 1/ 𝑓𝑎 axion coupling [40–43] (from [44]) (the constraint from [42] has been rescaled for consistent value of local DM energy density) (shown in solid lines). The new sensitivity estimates resulting from this thesis are shown in dashed line…
Figure 18.4
Figure 18.4. Figure 18.4: Current laboratory constraints on the axion-photon coupling [PITH_FULL_IMAGE:figures/full_fig_p189_18_4.png]
Figure 18.5
Figure 18.5. Figure 18.5: Expected sensitivity of DAMNED (red curve) and a 86 km long fiber (blue curve) to 𝑔𝑎𝛾. Compared to already existing exper￾iments (see [PITH_FULL_IMAGE:figures/full_fig_p190_18_5.png]
Figure 18.6
Figure 18.6. Figure 18.6: Dark photons-photons kinetic mixing coupling [PITH_FULL_IMAGE:figures/full_fig_p192_18_6.png]
Figure 18.7
Figure 18.7. Figure 18.7: Efficiency coefficient 𝛾(𝑓 , Δ𝑧)AF as function of the frequency 𝑓 and Δ𝑧, in the frequency range 𝑓 ∈ [6, 18] GHz, of the horn antenna [20] and for distances |Δ𝑧| ≫ 𝑟. The efficiency coefficient increases for low fre￾quencies and short distances and presents a local …
Figure 18.8
Figure 18.8. Figure 18.8: Preliminary constraint (95% confidence level) of a second run of [PITH_FULL_IMAGE:figures/full_fig_p200_18_8.png]

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    Computenumericallythefieldonthedish ®𝑈test 𝐷 (®𝑥)from®𝑈𝑃(®𝑥′)usingKirchhoffintegral theorem Eq. (11.6),

  79. [95]

    Compute the relative error between®𝑈𝐷(®𝑥) and®𝑈test 𝐷 (®𝑥). We consider the plane located at𝑧′ = 𝑅−𝑎, then the field at a point(𝜌′,𝜙′,𝑧′) on the plane going towards the dish, located at𝑧≥ 𝑧′, is given by ®𝑈P→D(𝜌′,𝜙′,𝑧′)=𝑖𝜒𝜔𝑈𝑒−𝑖𝑘𝑓(𝜌′)®𝑌∥,𝐷(𝜌′,𝜙′, 𝑓(𝜌′)+ 𝑧′). (E.1) Notice the ch...

  80. [2027]

    url: https://hal.archives-ouvertes.fr/jpa- 00248106

    doi: 10.1051/jp2:1994103 . url: https://hal.archives-ouvertes.fr/jpa- 00248106

    doi

Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.