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arxiv: 2606.01893 · v1 · pith:IL6GH2EEnew · submitted 2026-06-01 · 🌌 astro-ph.SR

Visualizing the Magnetic Structure in Interplanetary Coronal Mass Ejections with ATHARV

Vivek Menon , Jyoti Sheoran , Vaibhav Pant , Dipankar Banerjee This is my paper

Pith reviewed 2026-06-28 12:44 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords interplanetary coronal mass ejectionsmagnetic flux ropesin-situ observationsmultipoint measurementsspace weathermagnetic structureATHARV
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The pith

ATHARV remaps spacecraft time series of an ICME into spatial maps showing coherent flux-rope rotation with mesoscale differences between two points.

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

The paper presents ATHARV as a tool that converts in-situ magnetic field measurements from spacecraft into spatial coordinates by accounting for the expansion of the coronal mass ejection and the motion of the observing platforms. When applied to data from STEREO-A and Wind for the April 2023 event, the reconstructed sheath shows disordered fields while the magnetic ejecta displays a consistent right-handed SWN flux-rope rotation at both locations. Differences in field magnitude profiles, rotation details, and inferred sizes between the two spacecraft indicate that the magnetic structure varies on mesoscales. The work shows how single-point sampling limits inference of three-dimensional structure and why multipoint observations matter for ICME studies.

Core claim

The reconstructed magnetic ejecta shows a coherent rotation consistent with a right-handed SWN flux-rope configuration at both spacecraft, while differences in magnitude profiles, rotation signatures, and inferred sizes indicate mesoscale inhomogeneity within the ICME magnetic structure.

What carries the argument

ATHARV, the Analysis Tool for Heliospheric Arrangement of Remapped Vectors, which remaps time-series magnetic measurements into spatial coordinates assuming self-similar expansion along three orthogonal directions or using measured velocities as proxies for plasma motion.

If this is right

  • The magnetic ejecta can be visualized as a flux rope with coherent rotation from multipoint data.
  • Single-spacecraft data alone cannot reveal mesoscale inhomogeneities inside the structure.
  • Hodograms and field-orientation angles provide additional checks on magnetic coherence after remapping.
  • The publicly available tool supplies a consistent way to analyze other ICME events with expansion effects included.

Where Pith is reading between the lines

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

  • Applying the remapping to more multipoint events could show whether mesoscale variations are typical or rare in ICMEs.
  • If such inhomogeneities alter the overall field orientation, single-point estimates of geomagnetic impact may need revision.
  • Testing the method on simulated ICMEs with known internal structure would check how well the expansion assumption holds.

Load-bearing premise

The ICME expands self-similarly with possibly different rates along three orthogonal directions, allowing time series to be converted into spatial positions.

What would settle it

A third spacecraft observation or independent remote-sensing image that shows a rotation direction or size profile contradicting the remapped structures from the two points would falsify the reconstruction.

Figures

Figures reproduced from arXiv: 2606.01893 by Dipankar Banerjee, Jyoti Sheoran, Vaibhav Pant, Vivek Menon.

Figure 1
Figure 1. Figure 1: Schematic illustration of a self-similarly expanding one-dimensional structure (blue rectangle) at the reference time t0 (top panel) and at a later time t (bottom panel), propagating toward increasing coordinate values (to the right). The structure evolves from size l0(t0) centered at rcm(t0) to size l(t) centered at rcm(t). The spacecraft (black triangle) performing in-situ measurements is located at rsc(… view at source ↗
Figure 2
Figure 2. Figure 2: Time series of magnetic-field and plasma parameters observed by (i) STEREO-A and (ii) Wind during the ICME event of 23–24 April 2023. The panels show: (a) magnetic-field components (BR, BT , BN ) and total magnitude (|B|); (b) proton velocity components (VR, VT , VN ) and bulk speed (Vp); (c) proton number density (Np); (d) proton temperature (Tp, blue) and the expected temperature (Texp, red) derived from… view at source ↗
Figure 3
Figure 3. Figure 3: Three-dimensional reconstruction of the ICME magnetic field structure along the spacecraft trajectories during the ICME event of 2023 April 23–24 for (i) STEREO-A and (ii) Wind, generated using the ATHARV tool. Arrows indicate the magnetic field direction, with length and color representing |B| in the R0T0N0 frame at the initial ICME encounter time t0. The arrow tails trace the remapped spacecraft trajecto… view at source ↗
Figure 4
Figure 4. Figure 4: Top panels: Magnetic-field hodograms (BT –BN ) for the ICME event of 2023 April 23–24 observed at (i) STEREO-A and (ii) Wind. Data points and connecting lines are col￾or-coded by observation time. The white triangle marks the ICME onset, and the gold star indicates the onset of the ME. Bottom panels: Temporal evolution of the magnetic-field vector angle with respect to the T-axis at (iii) STEREO-A and (iv)… view at source ↗
read the original abstract

Interplanetary coronal mass ejections (ICMEs) are major drivers of space weather, and their geoeffectiveness is strongly governed by the structure and orientation of their internal magnetic field. However, in-situ observations provide only 1D sampling along a spacecraft trajectory, limiting direct inference of the ICME 3D magnetic structure. We introduce the Analysis Tool for Heliospheric Arrangement of Remapped Vectors (ATHARV), which remaps in-situ time-series measurements into spatial coordinates while accounting for ICME expansion and spacecraft motion. ATHARV assumes self-similar expansion with different expansion rates along three orthogonal directions, while more general cases use measured velocities as proxies for plasma motion. The framework also incorporates complementary diagnostics, including hodograms and magnetic-field orientation angles, to assess magnetic coherence and field rotation within ICMEs. We demonstrate ATHARV using multipoint observations of an ICME detected near 1 au by STEREO-A and Wind on 2023 April 23--24. The reconstructed sheath exhibits disordered and variable magnetic fields, whereas the magnetic ejecta (ME) shows a coherent rotation consistent with a right-handed SWN flux-rope configuration at both spacecraft. However, differences in magnetic-field magnitude profiles, rotation signatures, and inferred ME sizes indicate mesoscale inhomogeneity within the ICME magnetic structure, possibly associated with a writhed or distorted flux rope. This event highlights the limitations of interpreting ICME magnetic configurations from single-point measurements and demonstrates the importance of multipoint observations for investigating their 3D structure and evolution. ATHARV provides a consistent framework for interpreting in-situ ICME observations and investigating their spatial structure and evolution, and is publicly available to the heliophysics community.

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 / 2 minor

Summary. The paper introduces ATHARV, a tool that remaps in-situ time-series magnetic field data from ICMEs into spatial coordinates assuming self-similar expansion along three orthogonal axes (or velocity proxies for plasma motion). Applied to the 2023 April 23–24 ICME observed by both STEREO-A and Wind near 1 au, the reconstruction shows disordered fields in the sheath but coherent right-handed SWN flux-rope rotation in the magnetic ejecta (ME) at both spacecraft; differences in |B| profiles, rotation signatures, and inferred ME sizes are interpreted as evidence of mesoscale inhomogeneity, possibly from a writhed flux rope. The tool and its diagnostics (hodograms, orientation angles) are made publicly available.

Significance. If the remapping assumptions hold, ATHARV offers a reproducible framework for converting 1D trajectories into spatial visualizations of ICME magnetic structure, directly supporting the claim that single-spacecraft data are insufficient for 3D inference. The public code release and the concrete multipoint demonstration on a recent event are clear strengths that enable follow-on work.

major comments (1)
  1. [§3] §3 (ATHARV method description): the central claim of mesoscale inhomogeneity rests on the time-to-space remapping; the self-similar expansion with independent rates along three orthogonal directions (or velocity proxies) is stated but no sensitivity analysis, comparison between the two options, or independent validation of the chosen rates is shown for the 2023 April 23–24 event. This leaves open whether the reported differences in ME size and |B| profiles between STEREO-A and Wind could arise from the mapping choice rather than intrinsic structure.
minor comments (2)
  1. Figure captions and axis labels in the remapped spatial plots should explicitly state the expansion rates adopted for each direction so readers can reproduce the coordinate transformation.
  2. [§4] The abstract and §4 refer to 'inferred ME sizes' without quoting the numerical values or the exact formula used to convert the remapped intervals into physical lengths; adding these would strengthen the inhomogeneity claim.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the constructive review and the recommendation for minor revision. The single major comment is addressed point-by-point below.

read point-by-point responses

  1. Referee: [§3] §3 (ATHARV method description): the central claim of mesoscale inhomogeneity rests on the time-to-space remapping; the self-similar expansion with independent rates along three orthogonal directions (or velocity proxies for plasma motion) is stated but no sensitivity analysis, comparison between the two options, or independent validation of the chosen rates is shown for the 2023 April 23–24 event. This leaves open whether the reported differences in ME size and |B| profiles between STEREO-A and Wind could arise from the mapping choice rather than intrinsic structure.

    Authors: We agree that an explicit sensitivity test would strengthen the interpretation. In the revised manuscript we will add a dedicated subsection in §3 that (i) compares the self-similar expansion solution against the velocity-proxy solution for the 2023 April 23–24 event, (ii) reports the expansion rates adopted and the observational constraints used to select them, and (iii) shows that the reported differences in ME size, |B| profile shape, and rotation signatures remain qualitatively unchanged when the rates are varied within the range permitted by the in-situ velocity and density data. These additions will demonstrate that the mesoscale inhomogeneity conclusion is robust to reasonable choices of the remapping parameters. revision: yes

Circularity Check

0 steps flagged

No significant circularity in ATHARV derivation chain

full rationale

The paper presents ATHARV as a remapping framework that takes the self-similar expansion assumption (with independent rates along three axes or velocity proxies) as an explicit external input, then applies it to observed time series from STEREO-A and Wind to produce spatial vectors and diagnostics such as hodograms. The reported right-handed SWN flux-rope rotation and mesoscale inhomogeneity are direct outputs of this remapping applied to the data; no equation or step reduces the handedness, rotation signatures, or size differences back to a fitted parameter of the output itself. No self-citation is invoked as load-bearing justification for the central claims, and the method does not rename or smuggle in prior results by construction. The chain is therefore self-contained.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim depends on the self-similar expansion assumption and the choice of three orthogonal expansion rates; no new particles or forces are postulated.

free parameters (1)
  • expansion rates along three orthogonal directions
    Chosen to account for anisotropic self-similar expansion when remapping time series to spatial coordinates.
axioms (1)
  • domain assumption ICMEs undergo self-similar expansion
    Invoked to convert spacecraft time series into spatial maps while accounting for spacecraft motion.

pith-pipeline@v0.9.1-grok · 5855 in / 1276 out tokens · 25489 ms · 2026-06-28T12:44:00.106731+00:00 · methodology

discussion (0)

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Reference graph

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