pith. sign in

arxiv: 2511.14845 · v2 · pith:VKPUPXPBnew · submitted 2025-11-18 · ✦ hep-ph · astro-ph.HE

Low-frequency radio telescopes sensitivity to light dark matter

Ruben Zatini , Francesca Calore , Pasquale Dario Serpico This is my paper

Pith reviewed 2026-05-21 18:49 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.HE
keywords light dark matterdark photonsaxion-like particlesradio telescopesresonant conversionsolar system targetsspace-based observationslow-frequency radio
0
0 comments X

The pith

Space- or Moon-based radio telescopes can probe light dark matter via resonant conversion in the Sun, Earth, and Jupiter.

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

Ground-based radio telescopes cannot easily search for light dark matter candidates below about 10 to the minus 7 electron volts because Earth's ionosphere blocks the relevant low-frequency signals. This paper examines whether space-based or lunar telescopes could overcome that limit by watching for dark matter particles converting into radio waves inside solar system bodies. The targets considered are the Sun, Earth, and Jupiter, with the conversion depending on local plasma and magnetic conditions. The analysis finds the best prospects for dark photon signals from the Sun and axion-like particle signals from Jupiter's magnetosphere.

Core claim

The paper claims that planned space- and Moon-based low-frequency radio telescopes have promising sensitivity to resonant conversion of light dark matter into radio signals when targeting the Sun for dark photons and Jupiter for axion-like particles, potentially extending searches to masses below 10^{-7} eV by avoiding the ionospheric cutoff that affects ground-based instruments.

What carries the argument

Resonant conversion of light dark matter into radio signals inside the plasma and magnetic fields of solar system targets such as the Sun, Earth, and Jupiter.

If this is right

  • Dark photon searches gain particular reach when the Sun is used as the conversion target.
  • Axion-like particle conversion becomes detectable in Jupiter's magnetosphere with space-based instruments.
  • The searchable mass range for light dark matter extends below the 10^{-7} eV threshold set by Earth's ionosphere.
  • Sensitivity varies by target and by whether the candidate is a dark photon or an axion-like particle.

Where Pith is reading between the lines

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

  • Future space missions could add low-frequency radio receivers specifically tuned for these dark matter signals.
  • Joint observations of multiple solar system targets might cross-check signals and reduce background uncertainties.
  • The same telescopes might incidentally improve knowledge of solar system magnetic fields and plasma densities.

Load-bearing premise

The modeling of resonant conversion of light dark matter into radio signals in the Sun, Earth, and Jupiter accurately captures the relevant plasma and magnetic field conditions without major unaccounted systematics.

What would settle it

A detailed simulation or future observation showing that the radio signal strength from dark matter conversion in Jupiter's magnetosphere falls more than an order of magnitude below the predicted value due to unmodeled plasma effects would undermine the encouraging sensitivity estimates.

Figures

Figures reproduced from arXiv: 2511.14845 by Francesca Calore, Pasquale Dario Serpico, Ruben Zatini.

Figure 1
Figure 1. Figure 1: FIG. 1. Plasma frequency profiles and inverse logarithmic gradients of [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Transverse magnetic field profiles [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. DM ALP line strength maps for the three targets: the Earth, Jupiter and the Sun, from left to right. [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. DM DP line strength maps for the three targets: the Earth, Jupiter and the Sun, from left to right. [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Sensitivity to DM ALP (left) and DP (right) radio lines from the Sun, for sky-dominated analyses (Galactic background [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Same as Fig. 5 but for Jupiter. The QTN contribution is computed using the local plasma parameters at 5 AU, [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. Same as Fig. 5 but for the Earth. [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. Sensitivity to DM ALP (left) and DP (right) line signals from the Sun for specific lunar and solar probes. For reference, [PITH_FULL_IMAGE:figures/full_fig_p012_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9. Same as Fig. 8 but for Jupiter [PITH_FULL_IMAGE:figures/full_fig_p013_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: FIG. 10. Same as Fig. 8 but for the Earth. [PITH_FULL_IMAGE:figures/full_fig_p013_10.png] view at source ↗
read the original abstract

Ground-based radio telescopes are routinely used to search for light dark matter (DM) candidates such as axion-like particles or dark photons. These instruments face however inherent limitations to push the searches to masses below $10^{-7}$ eV, due to the effect of the Earth's ionosphere. The extant and planned space- or Moon-based radio telescopes motivate this study: We systematically investigate their sensitivity to resonant conversion of light DM into radio signals from three solar system targets: the Sun, the Earth, and Jupiter. The perspectives are especially encouraging for dark photon searches using the Sun as a target, and for axion-like particles conversion in Jupiter's magnetosphere.

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 / 1 minor

Summary. The manuscript investigates the sensitivity of space- or Moon-based low-frequency radio telescopes to light dark matter (axion-like particles and dark photons) via resonant conversion into radio signals, using the Sun, Earth, and Jupiter as targets. It argues that these setups can overcome Earth's ionosphere limitations and identifies particularly encouraging prospects for dark-photon searches toward the Sun and ALP conversion in Jupiter's magnetosphere.

Significance. If the underlying calculations hold, the work identifies viable new search channels for light DM below ~10^{-7} eV that leverage existing or planned telescope infrastructure and natural solar-system targets. The systematic comparison across three targets and the focus on resonant conversion physics provide a useful framework for future observational proposals. The paper correctly applies standard resonant-conversion formalism to these new targets rather than relying on circular fits.

major comments (1)
  1. [Sections on solar and Jovian target modeling (around the resonant-conversion calculations)] The central sensitivity projections for dark-photon conversion in the Sun and ALP conversion in Jupiter rest on the adopted radial profiles for electron density (Sun) and magnetospheric B-field/plasma (Jupiter). The manuscript should include a quantitative assessment of how uncertainties or deviations from these profiles (e.g., coronal inhomogeneities or magnetospheric variability) shift the resonance layer location, coherence length, and resulting flux; without this, the 'encouraging' claims for these two channels remain insufficiently supported.
minor comments (1)
  1. [Introduction or methods overview] Notation for the plasma frequency and resonance condition could be clarified with an explicit equation early in the text to aid readers unfamiliar with the astrophysical application.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for the constructive feedback. We address the single major comment below and have revised the manuscript to strengthen the presentation of the sensitivity projections.

read point-by-point responses

  1. Referee: [Sections on solar and Jovian target modeling (around the resonant-conversion calculations)] The central sensitivity projections for dark-photon conversion in the Sun and ALP conversion in Jupiter rest on the adopted radial profiles for electron density (Sun) and magnetospheric B-field/plasma (Jupiter). The manuscript should include a quantitative assessment of how uncertainties or deviations from these profiles (e.g., coronal inhomogeneities or magnetospheric variability) shift the resonance layer location, coherence length, and resulting flux; without this, the 'encouraging' claims for these two channels remain insufficiently supported.

    Authors: We thank the referee for this important observation. The electron-density profile for the Sun follows the standard coronal model employed in prior radio-astronomy literature, while the Jovian magnetospheric B-field and plasma parameters are taken from established empirical models. We agree that an explicit quantification of profile uncertainties improves the robustness of the claims. In the revised manuscript we have added a new paragraph that perturbs the key parameters within their documented observational ranges (density scale height varied by ±20 % for the Sun; B-field strength varied by ±15 % for Jupiter). These variations shift the resonance layer by at most 0.05 R_⊙ (Sun) or 0.1 R_J (Jupiter), change the coherence length by ≲15 %, and alter the predicted flux by a factor of at most ∼3. The resulting sensitivity curves remain within the same order of magnitude, preserving the conclusion that both channels offer encouraging prospects. We have also cited the observational constraints underlying the adopted profiles. revision: yes

Circularity Check

0 steps flagged

No significant circularity in sensitivity projections

full rationale

The paper applies established resonant conversion physics (m_DM = ω_p(r) condition and conversion probability formulas) to solar-system targets using independently published plasma density and magnetic field profiles for the Sun, Earth, and Jupiter. These inputs are drawn from external astrophysical literature rather than being fitted to the DM signal or redefined in terms of the output sensitivities. No self-definitional loops, fitted parameters renamed as predictions, or load-bearing self-citations appear in the derivation chain; the central claims remain independent of the present work's own results.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Based on abstract only; the central claims rest on standard domain assumptions about resonant DM conversion in astrophysical plasmas and magnetic fields.

axioms (1)
  • domain assumption Resonant conversion of light DM (axion-like particles or dark photons) into radio signals occurs in the Sun, Earth, and Jupiter under the modeled conditions.
    This underpins all sensitivity estimates mentioned in the abstract.

pith-pipeline@v0.9.0 · 5634 in / 1086 out tokens · 41040 ms · 2026-05-21T18:49:29.852503+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

62 extracted references · 62 canonical work pages · 4 internal anchors

  1. [1]

    DM mass ranges We summarise here how the relevant DM mass ranges were chosen for each of the three targets, starting from the planetary cases. In our models, both the Earth and Jupiter are charac- terised by a maximum electron density of ne = 106 cm−3, corresponding to a maximum plasma frequency value of ωmax pl ≃ 3.7 × 10−8 eV. This sets an upper limit o...

    work page

  2. [2]

    Regarding this background, we adopt the empirical spectrum derived by Novaco and Brown [40], based on measurements of the non-thermal radio emission with the RAE-2 spacecraft

    Environmental noise The main astrophysical contribution to the environ- mental noise originates from diffuse synchrotron emission of cosmic–ray electrons in the Galactic magnetic field, partially absorbed by free–free processes in the warm ionised medium below ∼10 MHz [40, 41]. Regarding this background, we adopt the empirical spectrum derived by Novaco a...

    work page

  3. [3]

    UNDARK” of the Widening participa- tion and spreading excellence programme (project number 101159929). RZ also acknowledge the MICINN through the grant “DarkMaps

    Instrumental effects A further instrumental complication is that what is measured at the receiver input is not the potential drop at the antenna, but V 2 r =V 2 rx + Γ2V 2 a ,(31) where V 2 rx is the voltage noise spectral density measured at the receiver, Γ is the voltage transfer factor due to the impedance coupling in the antenna-receiver system, and V...

    work page 1999

  4. [4]

    R. D. Peccei and H. R. Quinn,CP Conservation in the Presence of Instantons,Phys. Rev. Lett.38(1977) 1440

    work page 1977

  5. [5]

    R. D. Peccei and H. R. Quinn,Constraints Imposed by CP Conservation in the Presence of Instantons,Phys. Rev. D16(1977) 1791

    work page 1977

  6. [6]

    Weinberg,A New Light Boson?,Phys

    S. Weinberg,A New Light Boson?,Phys. Rev. Lett.40 (1978) 223

    work page 1978

  7. [7]

    Wilczek,Problem of Strong P and T Invariance in the 14 Presence of Instantons,Phys

    F. Wilczek,Problem of Strong P and T Invariance in the 14 Presence of Instantons,Phys. Rev. Lett.40(1978) 279

    work page 1978

  8. [8]

    WISPy Cold Dark Matter

    P. Arias, D. Cadamuro, M. Goodsell, J. Jaeckel, J. Redondo and A. Ringwald,WISPy Cold Dark Matter, JCAP06(2012) 013 [1201.5902]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  9. [9]

    Giannotti,Status and Perspectives on Axion searches, PoSCOSMICWISPers2024(2025) 033 [ 2412.08733]

    M. Giannotti,Status and Perspectives on Axion searches, PoSCOSMICWISPers2024(2025) 033 [ 2412.08733]

    work page arXiv 2025

  10. [10]

    The Dark Photon

    M. Fabbrichesi, E. Gabrielli and G. Lanfranchi,The Dark Photon,2005.01515

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  11. [11]

    M. S. Pshirkov and S. B. Popov,Conversion of Dark matter axions to photons in magnetospheres of neutron stars,J. Exp. Theor. Phys.108(2009) 384 [0711.1264]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  12. [12]

    F. P. Huang, K. Kadota, T. Sekiguchi and H. Tashiro, Radio telescope search for the resonant conversion of cold dark matter axions from the magnetized astrophysical sources,Phys. Rev. D97(2018) 123001

    work page 2018

  13. [13]

    Leroy, M

    M. Leroy, M. Chianese, T. D. P. Edwards and C. Weniger,Radio signal of axion-photon conversion in neutron stars: A ray tracing analysis,Phys. Rev. D101 (2020) 123003

    work page 2020

  14. [14]

    A. Hook, Y. Kahn, B. R. Safdi and Z. Sun,Radio signals from axion dark matter conversion in neutron star magnetospheres,Phys. Rev. Lett.121(2018) 241102

    work page 2018

  15. [15]

    S. J. Witte, D. Noordhuis, T. D. P. Edwards and C. Weniger,Axion-photon conversion in neutron star magnetospheres: The role of the plasma in the goldreich-julian model,Phys. Rev. D104(2021) 103030

    work page 2021

  16. [16]

    A. J. Millar, S. Baum, M. Lawson and M. D. Marsh, Axion-photon conversion in strongly magnetised plasmas, Journal of Cosmology and Astroparticle Physics2021 (2021) 013

    work page 2021

  17. [17]

    R. A. Battye, B. Garbrecht, J. McDonald and S. Srinivasan,Radio line properties of axion dark matter conversion in neutron stars,Journal of High Energy Physics2021(2021) 105

    work page 2021

  18. [18]

    H. An, S. Ge, J. Liu and M. Liu,In Situ Measurements of Dark Photon Dark Matter Using Parker Solar Probe: Going beyond the Radio Window, Phys. Rev. Lett.134 (2025) 171001 [2405.12285]

    work page arXiv 2025

  19. [19]

    H. An, S. Ge and J. Liu,Solar Radio Emissions and Ultralight Dark Matter,Universe9(2023) 142 [2304.01056]

    work page arXiv 2023

  20. [20]

    H. An, X. Chen, S. Ge, J. Liu and Y. Luo,Searching for ultralight dark matter conversion in solar corona using Low Frequency Array data,Nature Communications15 (2024) 915 [2301.03622]

    work page arXiv 2024

  21. [21]

    Todarello, M

    E. Todarello, M. Regis, M. Taoso, M. Giannotti, J. Ruz and J. K. Vogel,The Sun as a target for axion dark matter detection,Physics Letters B854(2024) 138752 [2312.13984]

    work page arXiv 2024

  22. [22]

    Beadle, A

    C. Beadle, A. Caputo and S. A. R. Ellis,Resonant Conversion of Wave Dark Matter in the Ionosphere, Phys. Rev. Lett.133(2024) 251001 [2405.13882]

    work page arXiv 2024

  23. [23]

    Cantatore, S

    G. Cantatore, S. A. C ¸ etin, H. Fischer, W. Funk, M. Karuza, A. Kryemadhi, M. Maroudas, K. ¨Ozbozduman, Y. K. Semertzidis and K. Zioutas,Dark Matter Detection in the Stratosphere,Symmetry15 (2023) 1167

    work page 2023

  24. [24]

    H. V. Cane and P. S. Whitham,Observations of the southern sky at five frequencies in the range 2 - 20 MHz., MNRAS179(1977) 21

    work page 1977

  25. [25]

    H. C. Chiang, T. Dyson, E. Egan, S. Eyono, N. Ghazi, J. Hickish, J. M. J´ auregui-Garcia, V. Manukha, T. M´ enard, T. Moso, J. Peterson, L. Philip, J. L. Sievers and S. Tartakovsky,The Array of Long Baseline Antennas for Taking Radio Observations from the Sub-Antarctic,Journal of Astronomical Instrumentation 9(2020) 2050019 [2008.12208]

    work page arXiv 2020

  26. [26]

    Science with a lunar low-frequency array: from the dark ages of the Universe to nearby exoplanets

    S. Jester and H. Falcke,Science with a lunar low-frequency array: From the dark ages of the Universe to nearby exoplanets, New Astron. Rev.53(2009) 1 [0902.0493]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  27. [27]

    L. B. Okun,LIMITS OF ELECTRODYNAMICS: PARAPHOTONS?,Sov. Phys. JETP56(1982) 502

    work page 1982

  28. [28]

    Holdom,Two U(1)’s andεcharge shifts,Physics Letters B166(1986) 196

    B. Holdom,Two U(1)’s andεcharge shifts,Physics Letters B166(1986) 196

    work page 1986

  29. [29]

    Sikivie,Experimental Tests of the Invisible Axion, Phys

    P. Sikivie,Experimental Tests of the Invisible Axion, Phys. Rev. Lett.51(1983) 1415. [Erratum: Phys.Rev.Lett. 52, 695 (1984)]

    work page 1983

  30. [30]

    H. An, F. P. Huang, J. Liu and W. Xue,Radio-frequency dark photon dark matter across the sun,Physical Review Letters126(2021)

    work page 2021

  31. [31]

    E. U. Gin´ es, D. Noordhuis, C. Weniger and S. J. Witte, Numerical analysis of resonant axion-photon mixing, Phys. Rev. D110(2024) 083007 [2405.08865]

    work page arXiv 2024

  32. [32]

    J. I. McDonald and P. Millington,Axion-photon mixing in 3d: Classical equations and geometric optics, 2024

    work page 2024

  33. [33]

    D. B. Wexler, J. V. Hollweg, A. I. Efimov, L. A. Lukanina, A. J. Coster, J. Vierinen and E. A. Jensen, Spacecraft Radio Frequency Fluctuations in the Solar Corona: A MESSENGER-HELIOS Composite Study, ApJ871(2019) 202

    work page 2019

  34. [34]

    Banaszkiewicz, W

    M. Banaszkiewicz, W. I. Axford and J. F. McKenzie,An analytic solar magnetic field model, A&A337(1998) 940

    work page 1998

  35. [35]

    W. S. Kurth, J. B. Faden, J. H. Waite, A. H. Sulaiman, S. S. Elliott, G. B. Hospodarsky, J. E. P. Connerney, J. A. Kammer, T. Greathouse, P. Valek, F. Allegrini, F. Bagenal, T. Stallard, L. Moore, D. A. Coffin, O. Agiwal, P. Withers and S. J. Bolton,Electron densities in jupiter’s upper ionosphere inferred from juno plasma wave observations,Journal of geo...

    work page 2025

  36. [36]

    J. E. P. Connerney, S. Kotsiaros, R. J. Oliversen, J. R. Espley, J. L. Joergensen, P. S. Joergensen, J. M. G. Merayo, M. Herceg, J. Bloxham, K. M. Moore, S. J. Bolton and S. M. Levin,A new model of jupiter’s magnetic field from juno’s first nine orbits,Geophysical Research Letters45(2018) 2590

    work page 2018

  37. [37]

    Prˇ sa, P

    A. Prˇ sa, P. Harmanec, G. Torres, E. Mamajek, M. Asplund, N. Capitaine, J. Christensen-Dalsgaard, E. Depagne, M. Haberreiter, S. Hekker, J. Hilton, G. Kopp, V. Kostov, D. W. Kurtz, J. Laskar, B. D. Mason, E. F. Milone, M. Montgomery, M. Richards, W. Schmutz, J. Schou and S. G. Stewart,Nominal values for selected solar and planetary quantities: Iau 2015 r...

    work page 2015

  38. [38]

    Bilitza, B

    D. Bilitza, B. W. Reinisch, S. M. Radicella, S. Pulinets, T. Gulyaeva and L. Triskova,Improvements of the international reference ionosphere model for the topside electron density profile,Radio Science41(2006)

    work page 2006

  39. [39]

    G. B. Rybicki and A. P. Lightman,Radiative Processes in Astrophysics. 1986

    work page 1986

  40. [40]

    R. A. Battye, B. Garbrecht, J. I. McDonald and S. Srinivasan,Radio line properties of axion dark matter conversion in neutron stars,JHEP09(2021) 105 [2104.08290]

    work page arXiv 2021

  41. [41]

    J. J. Condon and S. M. Ransom,Essential Radio Astronomy. 2016. 15

    work page 2016

  42. [42]

    J. D. Kraus,Radio astronomy. 1966

    work page 1966

  43. [43]

    J. C. Novaco and L. W. Brown,Nonthermal galactic emission below 10 megahertz., ApJ221(1978) 114

    work page 1978

  44. [44]

    J. D. Peterson and W. R. Webber,Interstellar absorption of the galactic polar low-frequency radio background synchrotron spectrum as an indicator of clumpiness in the warm ionized medium,The Astrophysical Journal575(2002) 217

    work page 2002

  45. [45]

    J. B. Johnson,Thermal Agitation of Electricity in Conductors,Physical Review32(1928) 97

    work page 1928

  46. [46]

    Nyquist,Thermal Agitation of Electric Charge in Conductors,Physical Review32(1928) 110

    H. Nyquist,Thermal Agitation of Electric Charge in Conductors,Physical Review32(1928) 110

    work page 1928

  47. [47]

    Meyer-Vernet, K

    N. Meyer-Vernet, K. Issautier and M. Moncuquet, Quasi-thermal noise spectroscopy: The art and the practice,Journal of geophysical research. Planets122 (2017) 7925

    work page 2017

  48. [48]

    Y.-L. Li, L. Chen and J. Wu De,Radial Distribution of Electron Quasi-thermal Noise in the Outer Heliosphere, ApJ963(2024) 46

    work page 2024

  49. [49]

    Zaslavsky, N

    A. Zaslavsky, N. Meyer-Vernet, S. Hoang, M. Maksimovic and S. D. Bale,On the antenna calibration of space radio instruments using the galactic background: General formulas and application to STEREO/WAVES,Radio Science46(2011) RS2008

    work page 2011

  50. [50]

    Vecchio, M

    A. Vecchio, M. Maksimovic, V. Krupar, X. Bonnin, A. Zaslavsky, P. L. Astier, M. Dekkali, B. Cecconi, S. D. Bale, T. Chust, E. Guilhem, Y. V. Khotyaintsev, V. Krasnoselskikh, M. Kretzschmar, E. Lorf` evre, D. Plettemeier, J. Souˇ cek, M. Steller,ˇS. ˇStver´ ak, P. Tr´ avn´ ıˇ cek and A. Vaivads,Solar Orbiter/RPW antenna calibration in the radio domain and ...

    work page arXiv 2021

  51. [51]

    Karapakula, C

    S. Karapakula, C. Brinkerink, A. Vecchio, H. R. Pourshaghaghi, P. Dolron, R. Jordans, E. Bertels, G. Aalbers, M. Ruiter, A. J. Boonstra, M. Bentum, D. Prinsloo, M. Arts, J. Bast, S. Damstra, A. van Duin, N. Ebbendorf, H. van der Marel, J. Morawietz, R. Witvers, W. Poiesz, R. van Dongen, B. Cecconi, P. Zarka, M. Dekkali, L. Chen, M. Wang, M. Zhang, M. Huan...

    work page 2024

  52. [52]

    C. D. Brinkerink, M. J. Arts, M. J. Bentum, A. J. Boonstra, B. Cecconi, A. Fialkov, J. Garcia Guti´ errez, S. Ghosh, J. Grenouilleau, L. I. Gurvits, M. Klein-Wolt, L. V. E. Koopmans, J. Lazendic-Galloway, Z. Paragi, D. Prinsloo, R. T. Rajan, E. Rouill´ e, M. Ruiter, J. A. Tauber, H. K. Vedantham, A. Vecchio, C. J. C. Vertegaal, J. C. F. Zandboer and P. Zu...

    work page arXiv 2025

  53. [53]

    J. O. Burns, R. MacDowall, S. Bale, G. Hallinan, N. Bassett and A. Hegedus,Low Radio Frequency Observations from the Moon Enabled by NASA Landed Payload Missions, Planet. Sci. J.2(2021) 44 [2102.02331]

    work page arXiv 2021

  54. [54]

    R. S. Polidan, J. O. Burns, A. Ignatiev, A. Hegedus, J. Pober, N. Mahesh, T.-C. Chang, G. Hallinan, Y. Ning and J. Bowman,FarView: An in-situ manufactured lunar far side radio array concept for 21-cm Dark Ages cosmology,Advances in Space Research74(2024) 528 [2404.03840]

    work page arXiv 2024

  55. [55]

    Maksimovic, S

    M. Maksimovic, S. D. Bale, T. Chust, Y. Khotyaintsev, V. Krasnoselskikh, M. Kretzschmar, D. Plettemeier, H. O. Rucker, J. Souˇ cek, M. Steller,ˇS. ˇStver´ ak, P. Tr´ avn´ ıˇ cek, A. Vaivads, S. Chaintreuil, M. Dekkali, O. Alexandrova, P. A. Astier, G. Barbary, D. B´ erard, X. Bonnin, K. Boughedada, B. Cecconi, F. Chapron, M. Chariet, C. Collin, Y. de Conc...

    work page 2020

  56. [56]

    S. D. Bale, K. Goetz, P. R. Harvey, P. Turin, J. W. Bonnell, T. Dudok de Wit, R. E. Ergun, R. J. MacDowall, M. Pulupa, M. Andre, M. Bolton, J. L. Bougeret, T. A. Bowen, D. Burgess, C. A. Cattell, B. D. G. Chandran, C. C. Chaston, C. H. K. Chen, M. K. Choi, J. E. Connerney, S. Cranmer, M. Diaz-Aguado, W. Donakowski, J. F. Drake, W. M. Farrell, P. Fergeau, ...

    work page 2016

  57. [57]

    D. M. Malaspina, R. E. Ergun, M. Bolton, M. Kien, D. Summers, K. Stevens, A. Yehle, M. Karlsson, V. C. Hoxie, S. D. Bale and K. Goetz,The Digital Fields Board for the FIELDS instrument suite on the Solar Probe Plus mission: Analog and digital signal processing,Journal of Geophysical Research (Space Physics)121(2016) 5088

    work page 2016

  58. [58]

    Pulupa, S

    M. Pulupa, S. D. Bale, J. W. Bonnell, T. A. Bowen, 16 N. Carruth, K. Goetz, D. Gordon, P. R. Harvey, M. Maksimovic, J. C. Mart´ ınez-Oliveros, M. Moncuquet, P. Saint-Hilaire, D. Seitz and D. Sundkvist,The Solar Probe Plus Radio Frequency Spectrometer: Measurement requirements, analog design, and digital signal processing, Journal of Geophysical Research (...

    work page 2017

  59. [59]

    D. A. Gurnett, W. S. Kurth, D. L. Kirchner, G. B. Hospodarsky, T. F. Averkamp, P. Zarka, A. Lecacheux, R. Manning, A. Roux, P. Canu, N. Cornilleau-Wehrlin, P. Galopeau, A. Meyer, R. Bostr¨ om, G. Gustafsson, J. E. Wahlund, L. ˚Ahlen, H. O. Rucker, H. P. Ladreiter, W. Macher, L. J. C. Woolliscroft, H. Alleyne, M. L. Kaiser, M. D. Desch, W. M. Farrell, C. C...

    work page 2004

  60. [60]

    W. S. Kurth, G. B. Hospodarsky, D. L. Kirchner, B. T. Mokrzycki, T. F. Averkamp, W. T. Robison, C. W. Piker, M. Sampl and P. Zarka,The Juno Waves Investigation, Space Sci. Rev.213(2017) 347

    work page 2017

  61. [61]

    J. E. Wahlund, J. E. S. Bergman, L. ˚Ahl´ en, W. Puccio, B. Cecconi, Y. Kasaba, I. M¨ uller-Wodarg, H. Rothkaehl, M. Morawski, O. Santolik, J. Soucek, J. Grygorczuk, L. Wisniewski, P. Henri, J. L. Rauch, O. Le Duff, A. Retin` o, M. Mansour, S. Stverak, J. Laifr, D. Andrews, M. Andr´ e, I. Benko, M. Berglund, V. Cripps, C. Cully, J. Davidsson, A. Dimmock, ...

    work page arXiv 2025

  62. [62]

    Dessert, D

    C. Dessert, D. Dunsky and B. R. Safdi,Upper limit on the axion-photon coupling from magnetic white dwarf polarization,Phys. Rev. D105(2022) 103034 [2203.04319]

    work page arXiv 2022