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REVIEW 4 major objections 8 minor 61 references

Latitudinal dependence of the solar wind during periods of high and low activity through interplanetary scintillation

T0 review · 4 major / 8 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read At solar minimum, the solar wind's latitudinal density profile is a steep sigmoid with an equator-to-south-pole reduction ratio of 1.62±0.02, while in the active phase it is consistent with spherical symmetry.

desk verdict A genuinely large IPS dataset and a plausible qualitative result, but the headline numbers—the sigmoid shape and the 1.62 reduction ratio—need to survive a model comparison and a line-of-sight smearing analysis before I'd trust them. read the letter →

arxiv 2506.14155 v1 pith:WBLPWFF4 submitted 2025-06-17 astro-ph.SR

A. Waszewski , J. S. Morgan , R. Ekers , M. Johnston-Hollitt , M. C. M. Cheung , N. D. R. Bhat , R. Chhetri , S. C. Fu This is my paper · ORCID
classification astro-ph.SR
keywords interplanetaryscintillationsolarwindcyclelatitudinaldependenceminimummaximumg-levelMurchisonWidefieldArray
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

This paper uses interplanetary scintillation (IPS) observations from the Murchison Widefield Array to measure how the solar wind's density-turbulence level varies with solar latitude at two extremes of the solar cycle. Its central claim is that during the 2019 minimum between cycles 24 and 25, the g-level, a measure of scintillation enhancement over a spherically symmetric reference wind, falls with southern latitude along a steep sigmoid, with the main drop between about -25 and -40 degrees and an equator-to-south-pole reduction ratio of 1.62±0.02 at 108–123 solar radii. For the active ascending phase of cycle 25 in 2023, the same measurement shows no latitude dependence, consistent with a spherically symmetric solar wind. A sympathetic reader would care because it implies that the large-scale shape of the inner heliosphere is strongly solar-cycle-dependent and that IPS-based solar wind models need a steeper-than-elliptical transition at solar minimum.

What carries the argument

The central object is the g-level, the ratio of a source's observed scintillation to the scintillation expected for a point source in a spherically symmetric solar wind, after dividing out source angular size through the normalized scintillation index. This isolates the density-turbulence enhancement along each line of sight. Latitude is assigned by tracing each line-of-sight piercepoint back to the Sun's centre (the effective Carrington latitude), an assumption of radial outflow. The argument is carried by fitting a logistic function $y = l + u/(1+e^{-k(x-x_0)})$ to g-level versus latitude in three elongation bins; the parameters $l$ and $u$ define the reduction ratio $(u+l)/l$, while $k$ and $x_0$ quantify the steepness and midpoint of the latitudinal transition.

What would settle it

Measure the same three elongation bins with an independent IPS telescope, or perform a tomographic inversion that solves for density turbulence in three dimensions without assuming radial outflow, and fit the same logistic function; if the fitted midpoint ($x_0\approx-24.8^\circ$) and steepness ($k\approx0.14$) do not reproduce within errors, the sigmoid and the $1.62\pm0.02$ reduction ratio are artifacts of the latitude assignment.

Watch

Extended reading notes

Core claim

The central discovery is that the latitude dependence of the solar wind's density turbulence at 162 MHz switches between two states over the solar cycle. During the 2019 sunspot-minimum period, the g-level as a function of effective Carrington latitude in the southern hemisphere is well described by a logistic function, with a sharp transition around $-24.8^\circ$ and most of the drop occurring between $-25^\circ$ and $-40^\circ$. The fitted equator-to-pole reduction ratio, $(u+l)/l$, is $1.67\pm0.04$ at $90$–$108\,R_\odot$, $1.62\pm0.02$ at $108$–$123\,R_\odot$, and $1.51\pm0.01$ at $123$–$138\,R_\odot$, decreasing with heliospheric distance. During the 2023 active period, the g-level distributions stay flat across latitude at elevated values, matching a spherically symmetric solar wind. The sigmoid contrasts with the smoother elliptical transition favored by earlier IPS studies at similar distances.

Load-bearing premise

The load-bearing premise is that each measurement can be tied to a single solar latitude by tracing the closest-approach point of the line of sight back to the Sun's centre, which assumes purely radial solar wind flow and ignores solar rotation; if the flow is non-radial or the sensitive region of the line of sight lies elsewhere, the fitted sigmoid and the quoted 1.62 ratio would be systematically biased.

Editorial extensions

If this is right

  • At solar minimum, IPS-based models of the solar wind at 90–140 solar radii should replace elliptical or spherical latitude profiles with a sigmoid having a transition near -25 to -40 degrees.
  • The equator-to-south-pole reduction ratio of 1.62±0.02 at 108–123 solar radii is larger than some earlier values reported at similar elongations, suggesting cycle-to-cycle variation in the sharpness of the polar-equator boundary.
  • During the active ascending phase, treating the solar wind as spherically symmetric is sufficient to describe g-level variations at these distances.
  • The decline of the reduction ratio from 1.67 to 1.51 across the three elongation bins indicates that the latitudinal contrast in density turbulence relaxes as the wind moves outward.
  • The steep sigmoid implies the boundary between equatorial and polar wind structure sits at a higher southern latitude than the smoother elliptical transition used in earlier models.

Reading between the lines

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

  • If the sigmoid is a generic feature of solar minima, the midpoint and steepness could be cycle-specific diagnostics; applying this fit to the other MWA epochs (2020, 2024) would test whether the boundary shifts with cycle strength.
  • A steep density-turbulence gradient near -25 to -40 degrees at these distances implies pulsar timing and dispersion-measure solar wind models will see larger scattering changes just below the equator than elliptical models predict.
  • The flat 2023 profile may partly reflect line-of-sight averaging with transient events present; repeating the analysis after removing identified CMEs, which the paper says was not done, would test whether a hidden latitude dependence remains.
  • An independent check would compare the fitted logistic profile to a tomographic IPS reconstruction that does not assume radial outflow, hardening or refuting the 1.62 ratio.
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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

4 major / 8 minor

Summary. This paper uses Murchison Widefield Array interplanetary scintillation (IPS) observations at 162 MHz from the 2019 solar minimum and the early-2023 ascending phase of cycle 25 to study the latitudinal dependence of the g-level. After restricting to the southern hemisphere and to elongations 25–40 degrees, the authors bin the data by elongation and latitude and fit a logistic function (Eq. 4) to the 2019 profiles, obtaining a reduction ratio (Eq. 5) of 1.62±0.02 for the 30–35 degree elongation bin (108–123 R_sun). The 2023 data are interpreted as consistent with a spherically symmetric active solar wind. The results are compared with prior IPS studies and discussed in terms of solar-cycle variation of the density-fluctuation environment.

Significance. If the results are robust, this paper provides the highest-density IPS source sample to date in the 90–140 R_sun range and would be the first MWA-based claim that the solar-minimum latitude profile is steeper than the elliptical form found in earlier IPS work. The paper is explicit about its definitions, reports parameter errors for the logistic fit, and honestly labels the reduction ratio as derived from fitted parameters rather than as a prediction. The main value is observational: a large, homogeneous IPS dataset that can test and constrain solar-wind models at heliocentric distances that complement coronagraph and in-situ measurements. The central claims, however, rest on two assumptions that are acknowledged but not quantitatively validated: the localization of a line-of-sight-integrated measurement to a single piercepoint latitude, and the interpretation of visual inspection as statistical evidence for flatness in 2023.

major comments (4)
  1. [Section 2.2 and Section 3, Eq. (4)-(5)] The latitude assigned to each g-level is obtained by tracing the line-of-sight piercepoint back to the Sun's center, but Section 2.2 explicitly states that IPS is a weighted line-of-sight integration and that the method assumes radial flow and neglects solar rotation. The paper claims that the adopted 'Carrington' latitude partially mitigates line-of-sight effects, but no quantitative estimate of the remaining latitude smearing is given. For the MWA geometry, the half-power region at nearly constant heliocentric distance can span tens of degrees in heliographic latitude, which is comparable to the claimed transition width in Figure 5. This systematic can bias the fitted logistic steepness k, the midpoint x0, and therefore the reduction ratio in Eq. (5), and it is not included in the quoted statistical errors. Please provide a quantitative assessment, for example by forward-modeling the line-of-sight integral for a trial latitude profile and comparing the recovered logistic parameters, or otherwise demonstrate that the piercepoint assignment is unbiased for the actual weighting function.
  2. [Section 3, Figure 4] The claim that the 2023 observing period is consistent with a spherically symmetric solar wind is based on visual inspection of the g-level distributions. No quantitative test of flatness is reported: there is no fit of a constant or latitude-independent model, no upper limit on a latitude gradient, and no goodness-of-fit statistic. Because the 2019-versus-2023 contrast is a central conclusion of the paper, please add a statistical test (e.g., fitting a constant to the binned means or medians with uncertainties and reporting a confidence interval on any slope) to support the spherical-symmetry statement.
  3. [Section 3, Figure 5; Abstract] The paper states that a logistic/sigmoid function better represents the 2019 data than the elliptical function used by Manoharan (1993), but no model comparison is performed. Only the logistic function is fitted in Figure 5. Please fit the elliptical functional form (or another published alternative) to the same binned data and compare the models using an appropriate criterion (e.g., AIC/BIC, residual scatter, or a nested test) before concluding that the sigmoid is required. As written, the claim that the sigmoid is 'more exaggerated' than an ellipse is not supported by the analysis presented.
  4. [Section 2.2.1 and Section 4.1] The 2023 analysis deliberately does not remove transient events such as CMEs or stream interaction regions, and the text acknowledges that removal of such events 'may potentially' change the 2023 results. Since the 2023 flatness claim is based on elevated and broadened g-level distributions that could be influenced by a small number of large transients, please perform a sensitivity analysis—for example, excluding clearly enhanced measurements, using robust statistics such as the median, or identifying and removing obvious events—to demonstrate that the spherical-symmetry conclusion is not driven by transient contamination.
minor comments (8)
  1. [Section 2.2.1] The phrase 'refereed to simply' should be 'referred to simply'.
  2. [Section 4.2] The heading 'F uture W ork' contains stray spaces; please correct.
  3. [References] The reference list contains apparent typos: 'Crammer' is likely 'Cranmer' for the 2017 solar wind origins paper, and 'actiivty' in the McIntosh et al. reference should be 'activity'.
  4. [Section 3] The fitting procedure for the logistic function is not described: the minimization method, the treatment of outliers, and the way parameter uncertainties were computed are not stated. Please add this information so the reported parameters and errors are reproducible.
  5. [Section 3, Figure 4] The caption says that outliers above 4 sigma were removed from the figure; please clarify whether the statistics and fits use the full data or only the outlier-clipped data, since this affects the reported means and the logistic fit.
  6. [Section 2.2] The term 'Carrington latitude' is used for a latitude obtained by tracing the piercepoint to the Sun's center, which is nonstandard; please define this coordinate more carefully and distinguish it from helioprojective latitude throughout the paper.
  7. [Table 2] The 'Source Count' column lists values (e.g., 1265 for the 30–35 degree bin) that are much smaller than the population sizes stated in Section 3 (5578 for the same bin); please clarify whether these are unique sources rather than individual measurements, and how they were obtained.
  8. [Abstract and Section 4] The sentence in the abstract that an elliptical function 'better represents' the transition while a sigmoid is 'required' is confusing and appears to contradict the body of the paper; please rephrase to state clearly that the paper finds a sigmoid provides a better description than an ellipse.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the central latitude profile and reduction ratio are data-derived fits, not predictions from their own inputs.

full rationale

The paper's central claims are empirical fits to MWA IPS data, and none of the load-bearing results reduce by construction to the analysis inputs. The m_pt normalization in Eq. (2) does assume a spherically symmetric solar wind and fixes b=1.6 from Readhead (1971), an independent external IPS measurement, not a parameter fitted to the present dataset. This normalization provides an isotropic baseline, but the 2019 latitude dependence is detected as residual variation of g-level with latitude after that normalization; Eq. (2) contains no latitude term, so it cannot generate the observed latitude profile. The 2023 'spherically symmetric' conclusion is supported by the observed flatness of the g-level distributions across latitude bins, not merely by the normalization; the measured g-levels are elevated above 1 during activity, showing that the normalization does not force g=1. The headline reduction ratio of 1.62±0.02 is read directly from the fitted logistic parameters l and u via Eq. (5), and the paper explicitly labels this as a fit summary in Table 2 rather than an out-of-sample prediction. The logistic function in Eq. (4) is chosen and fitted to the data; references to Coles et al. (1995) and Manoharan (1993) are external comparisons used for context, not load-bearing self-citations. The self-citations that appear (Morgan et al. 2019, 2022; Waszewski et al. 2023; Chhetri et al. 2018) are methodological, data-processing, or source-calibration references; the NSI values are independently measured source properties and no cited 'uniqueness' theorem is invoked to forbid alternative models. The Section 2.2 piercepoint-latitude mapping relies on an unvalidated assumption of radial flow and neglect of solar rotation, which is a legitimate systematic-accuracy concern, but it is not circular: the fitted latitude profile is not defined by that mapping in a way that makes the output equal to the input. Overall, the derivation chain is self-contained against independent external calibrations and the paper's numerical claims are honest fits to the data, so no significant circularity is present.

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

The central result depends on the spherical normalization m_pt with b=1.6 (a fitted value imported from Readhead 1971), the four fitted parameters of the logistic function that directly produce the reduction ratio, and the choice of three elongation bins, since the ratio varies by bin. The latitude mapping assumes radial flow and the g-level proxy assumes piercepoint-dominated line-of-sight weighting. No new physical entities are introduced.

free parameters (3)
  • Radial dependence index b = 1.6
    Taken from Readhead (1971) and used in Eq. (2) to normalize g-level; the central latitudinal result depends on this normalization choice.
  • Logistic parameters for 30 to 35 degree bin = l=0.63, u=0.39, k=0.14, x0=-24.8 degrees
    Best-fit parameters of Eq. (4) for the 30 to 35 degree elongation bin; the reduction ratio (u+l)/l = 1.62 derives from these fitted values.
  • Elongation bin boundaries = 25 to 30, 30 to 35, 35 to 40 degrees
    Chosen to mitigate residual elongation effects; the reduction ratio varies across bins (1.67, 1.62, 1.51), so the reported value depends on bin choice.
assumptions (4)
  • domain assumption Weak scattering regime holds for elongations above 15 degrees at 162 MHz, so the m_pt formula (Eq. 2) is valid.
    Section 2.2 states Eq. (2) applies only to the weak scattering regime, above roughly 15 degrees; data are at 25 to 40 degrees, but Section 4.1 notes a gradual transition toward strong scintillation near the equator, which would bias g-level low.
  • domain assumption Solar wind flows radially so the piercepoint latitude can be mapped by a straight line to the Sun's center, ignoring solar rotation.
    Section 2.2 explicitly states this assumption and says Carrington longitude is not computed because it requires solar wind speed.
  • domain assumption The radial dependence of Delta N_e^2, proportional to R^{-(2b+1)} with b constant, does not vary with solar activity or latitude.
    Section 2.2, Eq. (1), cites prior IPS literature; if b varies with latitude or activity, the inferred g-level latitude trend would be distorted.
  • domain assumption g-level is a valid proxy for electron density fluctuations along the line of sight, dominated by the piercepoint.
    Section 2.2 notes IPS is a weighted line-of-sight integration, not a point measurement; the analysis assigns each g-level to a single latitude.

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Pith. "Pith review of Latitudinal dependence of the solar wind during periods of high and low activity through interplanetary scintillation." pith.science (2026). https://pith.science/paper/WBLPWFF4

@misc{pith2026250614155,
  author       = {Pith},
  title        = {Pith review of: Latitudinal dependence of the solar wind during periods of high and low activity through interplanetary scintillation},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/WBLPWFF4}},
  note         = {Machine review of arXiv:2506.14155}
}
abstract

We present a study of the solar wind over different periods of the solar cycle, specifically focussing on the minimum between solar cycles 24 and 25, and the active, ascending phase of solar cycle 25. With the use of interplanetary scintillation (IPS) data taken by the Murchison Widefield Array (MWA) from mid-2019 and early 2023, we have sampled over a wide range of solar latitudes and elongations, probing a large section of the surrounding heliosphere from $\sim$90 to 140R$_\odot$. The MWA observations provide the highest density of sampled IPS radio sources to date, allowing for an investigation into the latitudinal dependence of the scattering effect caused by the solar wind on a radio source as observed throughout the solar cycle. We find our measurements during periods of heightened solar activity are consistent with a spherically symmetric solar wind. On the other hand, with a reduction in solar activity we find the solar wind density inherits a latitudinal dependence. As is consistent with prior studies, an elliptical function better represents the transition from poles to equator, although we find a more exaggerated sigmoid shaped curve is required to represent the low- to mid-latitude transition region during the minimum of solar cycle 24. We find for a heliospheric distance range of 108 - 123R$_{\odot}$ the reduction ratio between the equator and the southern pole is 1.62$\pm$0.02.

Figures

Figures reproduced from arXiv: 2506.14155 by the authors.

Figure 1
Figure 1. Daily sunspot total, with the smoothed monthly sunspot number over solar cycles 24 and 25. Highlighted are the date ranges for both observing pe￾riods selected as part of this study (2019: pink, 2023: green). Sunspot numbers are taken from the World Date Center SILSO. As part of the MWA IPS survey, both observing pe￾riods were passed through a calibration and imaging pipeline. For the full processing methodology as … view at source ↗
Figure 2
Figure 2. The half-power region where IPS measure [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. An example g-map for a day in observing pe [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: Distribution of g-levels in the elongation range of 30 [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 5
Figure 5. Figure 5: Best fit logistic function (coloured, full lines) [PITH_FULL_IMAGE:figures/full_fig_p007_5.png]

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