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arxiv: 2606.29594 · v1 · pith:HQFZ4J5Hnew · submitted 2026-06-28 · 🌌 astro-ph.SR

Radio Wave Propagation as a Probe of the Solar Corona and Solar Wind

K. Sasikumar Raja , Prasad Subramanian , Susanta Kumar Bisoi , Janardhan Padmanabhan , Eduard Kontar , Anshu Kumari This is my paper

Pith reviewed 2026-06-30 01:43 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords radio wave propagationsolar coronasolar windinterplanetary scintillationangular broadeningturbulencedensity fluctuationsSKA
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The pith

Radio waves distorted by the solar corona and wind reveal turbulence strength, heating rates, and magnetic topology.

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

This review shows that radio waves passing through the solar corona and solar wind acquire phase deviations from density fluctuations, producing measurable effects such as angular broadening of sources and intensity scintillation. These effects allow extraction of the phase structure function, turbulence amplitude, density modulation index, heating rates, magnetic field topology, and dissipation scales. The current scarcity of suitable radio sources near the ecliptic limits the reach of such measurements. Future arrays are projected to supply many more sources, enabling systematic tracking of how the derived quantities vary with distance from the Sun and across the solar cycle.

Core claim

Radio waves propagating through an inhomogeneous, turbulent medium such as the solar corona and solar wind become distorted, causing the initially plane wavefronts to become corrugated and acquire an RMS phase deviation across the wavefront. This leads to observable effects such as angular broadening of radio sources or intensity scintillation. Such observations enable the study of several key properties, such as the phase structure function, amplitude of turbulence, density modulation index, solar wind heating rates, magnetic field topology, and dissipation scales.

What carries the argument

Wavefront corrugation and RMS phase deviation produced by density fluctuations, observed through angular broadening and interplanetary scintillation.

Load-bearing premise

Future radio arrays will detect a significantly larger number of radio sources near the ecliptic.

What would settle it

Observations with the new arrays that fail to increase the number of usable sources near the ecliptic or that yield turbulence parameters inconsistent with independent solar-wind models.

Figures

Figures reproduced from arXiv: 2606.29594 by Anshu Kumari, Eduard Kontar, Janardhan Padmanabhan, K. Sasikumar Raja, Prasad Subramanian, Susanta Kumar Bisoi.

Figure 1
Figure 1. Figure 1: The schematic diagram shows the geometry of Crab nebula occultation; ‘PQ’ indicates the projected path of the Crab nebula during the month of June every year. The closest point of ‘PQ’ to ‘S’ is ≈ 5 𝑅⊙. The radiation from ‘C’ passes through the effective turbulent medium ‘AB’ at a solar elongation of ‘𝜖’ as viewed from ‘E’. density irregularities in the solar wind leads to an increase in its apparent angul… view at source ↗
Figure 2
Figure 2. Figure 2: The upper panel shows the solar disk view of the Crab nebula occultation technique. The filled red colored circle represents the Sun, while the green circles indicate the positions of the Crab nebula relative to the Sun on different dates. Here, ΔR.A. and ΔDec denote the offset distances of the Crab nebula from the Sun in right ascension and declination, respectively. The innermost concentric circle around… view at source ↗
Figure 3
Figure 3. Figure 3: A log-log plot of 𝐶 2 𝑁 vs the heliocentric distance (in 𝑅⊙) derived from observations in 2013. We used 𝛼 = 3 and the inner scale is the proton inertial length. The fit to 𝐶 2 𝑁 (𝑅) = 𝐴 𝑅−𝛾 yields 𝛾 = 3.4 and 𝐴 = 4 × 105 cm−6 . The correlation between 𝛾 and the sunspot number indicates that the scattering strength falls off faster with heliocentric distance when solar activity increases. This might be beca… view at source ↗
Figure 4
Figure 4. Figure 4: The top panel and middle panel show 𝛾 and 𝐴 (𝑐𝑚−6 ) as a function of time. The ‘circles’ and ‘squares’ indicate the proton inertial and proton gyroradius inner scale models respectively with 𝛼 = 3. For the proton gyroradius model, a temperature of 105 K was used. The solid line in the bottom panel shows the yearly averaged sunspot number and the ‘*’ represents the year in which the Crab occultation measure… view at source ↗
Figure 5
Figure 5. Figure 5 [PITH_FULL_IMAGE:figures/full_fig_p012_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Heliocentric dependence of the proton heating rate in different years is shown. The markers ‘circle’ and ‘square’ indicate proton heating rates that are derived using the proton inertial length and proton gyroradius model, respectively. 𝛿𝑣𝑘𝑖 (𝑅) = [PITH_FULL_IMAGE:figures/full_fig_p013_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: (top) Solar cycle dependence of the modulation index averaged over the heliocentric distance 5−45 𝑅⊙. (middle) Solar cycle dependence of the proton heating rate averaged over the heliocentric distance 5−45 𝑅⊙. The measurements for various inner scale models, i.e., proton inertial length and proton gyroradius models are indicated with the symbols ‘circle’ and ‘square’, respectively. (bottom) The solid line … view at source ↗
Figure 8
Figure 8. Figure 8: The circles indicate 𝐷obs(𝑠)/𝐷obs(𝑠𝑟 ) for the Crab Nebula observed on 18 June 2016, the radio image. The solid line represents 𝐷th (𝑠)/𝐷th (𝑠𝑟 ) (Eq 17) for 𝛼 = 3 and the dissipation scale 𝑙𝑖 = 560 m. The average rms error between the model fit (solid line) and the visibility data (circles) is 3.67% 19 [PITH_FULL_IMAGE:figures/full_fig_p019_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: The dissipation length (𝑙𝑖) of density turbulence in the solar wind as a function of projected heliocentric distance in units of 𝑅⊙. The red circles indicates the dissipation scale lengths derived from the observations. The solid line indicates the prediction of proton inertial length model. The dashed line indicates the proton gyroradius computed using a temperature of 105 K and the Parker spiral magnetic… view at source ↗
Figure 10
Figure 10. Figure 10: The left panel shows the SOHO/LASCO C3 image of the solar corona (inverted grey scale image) observed on 17 June 2016 at 06:30 UT. The innermost black circle depicts the solar disk (radius = 1 𝑅⊙). The next concentric circle is the occulting disk of the coronagraph and its radius is 3.5 𝑅⊙. The outermost circle marks a heliocentric distance of 30 𝑅⊙. In both the images, the black features are coronal stre… view at source ↗
Figure 11
Figure 11. Figure 11: The image on 12 June 2016 shows the angular broadened Crab nebula at a heliocentric distance of 10.18 𝑅⊙ during its ingress into the inner solar wind. The images on 17 June 2016 (at 10.2 𝑅⊙), 17 (9.41 𝑅⊙) and 18 June 2017 (12.61 𝑅⊙) depict the angular broadened Crab nebula observed through coronal streamers during its egress from the solar wind. The arrows depict the sunward direction on each day. The maj… view at source ↗
Figure 12
Figure 12. Figure 12: Peak flux density of the Crab nebula on different days of June 2016 is shown in red circles and 2017 in blue squares. The red and blue data points shown in the shaded area show instances when the Crab nebula was observed through a streamer in 2016 and 2017 respectively. 9 Observations through CMEs Low-frequency radio observations of the occultation of the Crab Nebula by the slow Coronal Mass Ejection even… view at source ↗
Figure 13
Figure 13. Figure 13: The variation of the density modulation index (red circles) and the solar wind proton heating rate (blue squares) with projected heliocentric distance. We note that the proton heating rate is correlated with the density modulation index. range of 2–16 𝑅⊙. The observed angular broadening is anisotropic, with axial ratios ranging from 2 to 16. Larger axial ratios are preferentially detected at smaller solar… view at source ↗
Figure 14
Figure 14. Figure 14: Radio map of the Crab nebula obtained on 1997 June 4 with the CME is in the foreground at a heliocentric distance of 41𝑅⊙. 25 [PITH_FULL_IMAGE:figures/full_fig_p025_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Sample radio maps of different sources observed using VLA in A-configuration. the tracking of solar wind electron density variations with scale sizes ≤ 103 km over heliocentric distances of 0.26 to 0.82 AU in the inner heliosphere (Pramesh Rao et al., 1974). IPS observations have been instrumental in measuring solar wind velocity (Coles, 1996; Manoharan and Ananthakr￾ishnan, 1990; Kojima and Kakinuma, 199… view at source ↗
read the original abstract

Radio waves propagating through an inhomogeneous, turbulent medium such as the solar corona and solar wind become distorted, causing the initially plane wavefronts becomes corrugated and acquire an RMS phase deviation across the wavefront. This leads to observable effects such as angular broadening of radio sources or intensity scintillation. Such waves can be used to probe the solar wind through various techniques, including angular broadening and interplanetary scintillation observations. Such observations enable the study of several key properties, such as the phase structure function, amplitude of turbulence, density modulation index, solar wind heating rates, magnetic field topology, and dissipation scales. These phenomena provide critical insights into the physical processes governing the solar corona and solar wind and its interaction with radio waves, offering valuable constraints on both coronal and solar wind turbulence and coronal magnetic field configurations. Currently, the limited number of radio sources near the ecliptic restricts our observations. However, the SKA-Low and SKA-Mid are expected to detect a significantly larger number of radio sources, thereby providing deeper insights into the solar corona, solar wind, and heliosphere. Long-term observations will be crucial to understanding how the above-mentioned parameters vary with heliocentric distance and over the solar cycle.

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

0 major / 1 minor

Summary. The manuscript is a review summarizing how radio waves propagating through the inhomogeneous solar corona and solar wind are distorted, producing observable effects such as angular broadening of sources and intensity scintillation. It states that angular broadening and interplanetary scintillation (IPS) observations can be used to study the phase structure function, turbulence amplitude, density modulation index, solar wind heating rates, magnetic field topology, and dissipation scales. The text notes the current restriction from the limited number of radio sources near the ecliptic and projects that SKA-Low and SKA-Mid will detect significantly more sources, enabling deeper insights into the corona, solar wind, and heliosphere, while emphasizing the value of long-term observations to track variations with heliocentric distance and solar cycle.

Significance. If the synthesis is accurate, the paper provides a concise overview of established radio-propagation techniques for heliospheric studies and highlights the prospective role of SKA observations. Its value is primarily as a literature compilation rather than an advance containing new data, derivations, or quantitative error analysis.

minor comments (1)
  1. [Abstract] Abstract: the clause 'the initially plane wavefronts becomes corrugated' contains a subject-verb agreement error ('becomes' should be 'become').

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their review and positive assessment of the manuscript as a concise overview of radio-propagation techniques. No specific major comments were provided in the report, so we have no points requiring direct response or revision at this stage. The manuscript is intended as a literature synthesis highlighting established methods and the prospective role of SKA observations, consistent with the referee's description.

Circularity Check

0 steps flagged

No significant circularity; review of established techniques

full rationale

This is a review paper summarizing established radio-propagation methods (angular broadening, IPS) and their standard applications to derive quantities such as phase structure function, turbulence amplitude, density modulation index, heating rates, magnetic topology, and dissipation scales. These follow directly from cited observables in the external literature with no internal derivation chain, fitted parameters renamed as predictions, or self-citation load-bearing steps that reduce to the paper's own inputs by construction. The SKA sensitivity projection is a straightforward extrapolation with no hidden self-reference. The manuscript is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a review/overview paper; no new free parameters, axioms, or invented entities are introduced in the provided abstract. All content draws from established radio astronomy and solar physics concepts.

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