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arxiv: 2606.31440 · v1 · pith:LC7D2D4Rnew · submitted 2026-06-30 · 🌌 astro-ph.SR · physics.space-ph

Role of SKA in Advancing Remote Measurements of Magnetic Fields of Solar Coronal Mass Ejections

Devojyoti Kansabanik , Surajit Mondal , Shaheda Begum Shahik , Peijin Zhang , Puja Majee , Angelos Vourlidas , John Morgan , Divya Oberoi
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Anshu Kumari Alec Thomson Bin Chen Carl Shneider Hariharan Krishnan Kamen Kozarev Sneha Pandit Vanessa Moss
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Pith reviewed 2026-07-01 03:17 UTC · model grok-4.3

classification 🌌 astro-ph.SR physics.space-ph
keywords coronal mass ejectionsmagnetic fieldsradio observationsspace weatherSquare Kilometre Arrayremote sensingFaraday rotationsolar corona
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The pith

The Square Kilometre Array will enable routine remote radio measurements of the magnetic fields carried by solar coronal mass ejections.

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

Coronal mass ejections drive space weather, yet their vector magnetic fields remain difficult to measure directly because visible-light observations yield only geometry and speed. Radio observations across MHz to GHz frequencies can sense these fields remotely through polarization effects, but current instruments lack the sensitivity, bandwidth, and frequency span needed to track evolving structures reliably. The paper reviews results from SKA precursors that have already demonstrated the techniques and identifies the hardware shortfalls that have limited them. It concludes that the SKA's improvements will remove those shortfalls and let the measurements constrain space-weather models.

Core claim

Radio observations spanning MHz to GHz frequencies provide a remote-sensing approach for measuring CME magnetic fields from the ground; recent work with SKA precursors has shown the potential of these techniques, but current instruments are limited by sensitivity, bandwidth, and frequency coverage. The higher sensitivity, wider instantaneous bandwidth, and broader frequency coverage of the SKA will open a new observational window, enabling these techniques to be fully exploited for constraining space-weather models and improving predictive accuracy, although the observations are non-standard and require special consideration in scheduling, calibration, and imaging.

What carries the argument

Radio remote-sensing techniques that use polarization and Faraday rotation across a wide frequency range to determine the strength and topology of CME magnetic fields.

If this is right

  • CME magnetic-field data will provide direct constraints on space-weather models that currently rely on indirect inferences.
  • Predictive accuracy for the geoeffectiveness of Earth-directed CMEs will increase.
  • Non-standard radio observations of CMEs will require dedicated scheduling, calibration, and imaging pipelines on the SKA.
  • Results from SKA precursors will guide the design of those pipelines and demonstrate their feasibility.

Where Pith is reading between the lines

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

  • The same wide-band data could be combined with visible-light coronagraph images to produce three-dimensional magnetic-field maps of individual events.
  • Routine measurements would allow statistical studies of how CME magnetic fields evolve with distance from the Sun rather than single-event case studies.
  • Improved remote magnetic diagnostics might reduce dependence on sparse in-situ measurements from spacecraft at L1.

Load-bearing premise

The main barriers to radio measurements of CME magnetic fields are the sensitivity, bandwidth, and frequency coverage of existing instruments, and that the SKA will overcome these barriers without creating new insurmountable problems in scheduling, calibration, or imaging.

What would settle it

A set of SKA observations of a well-observed CME that fails to yield usable vector magnetic-field measurements because of calibration or imaging difficulties that persist despite the instrument's improved hardware specifications.

Figures

Figures reproduced from arXiv: 2606.31440 by Alec Thomson, Angelos Vourlidas, Anshu Kumari, Bin Chen, Carl Shneider, Devojyoti Kansabanik, Divya Oberoi, Hariharan Krishnan, John Morgan, Kamen Kozarev, Peijin Zhang, Puja Majee, Shaheda Begum Shahik, Sneha Pandit, Surajit Mondal, Vanessa Moss.

Figure 1
Figure 1. Figure 1: A schematic depicts the current approach of CME magnetic field prediction for space weather forecasting. The left panel shows the photospheric magnetic field measurements, the middle panel shows white-light observations used to constrain geometric and dynamical properties, and the right panel shows the swarm of spacecraft used for in-situ measurements. 3 [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Direct and indirect radio observables that enable measurements of CME magnetic fields in the corona and inner heliosphere using ground-based radio observations. The background illustration highlights the imaging capabilities provided by the combined instrument suites onboard the STEREO-A (Ahead) and STEREO-B (Behind) spacecraft. The central panel presents a composite image that merges extreme ultraviolet (… view at source ↗
Figure 3
Figure 3. Figure 3: Left panel: A type-II radio burst showing multi-lane emission in the solar dynamic spectrum observed using the Learmonth solar radio spectrograph. Right panel: A type-IV radio burst observed with the Learmonth solar radio spectrograph. 2.1.1 Magnetic Field at CME Shocks using Type-II Radio Bursts Type-II solar radio bursts (type-IIs) are produced by the coherent plasma emission mechanism when energetic non… view at source ↗
Figure 4
Figure 4. Figure 4: The first detection of gyrosynchrotron emission from CME plasma using Nançay Radio Heliograph. The left panel shows the gyrosynchrotron radio emission from the CME, with white arcs marking the white￾light CME, which is shown in the right panel. The right panel shows the CME observed at the closest time using the white-light LASCO C2 coronagraph (Reproduced from Bastian et al. (2001)). 2.1.4 Gyrosynchrotron… view at source ↗
Figure 5
Figure 5. Figure 5: Left panel: The first detection of gyrosynchrotron emission from a slow CME. Cyan contours indicate the radio emission superimposed on the white-light LASCO C2 coronagraph image. Spectra have been extracted and modeled in the blue circle regions. (Reproduced from Mondal et al. (2020)). Right panel: Gyrosynchrotron emissions detected from two CMEs, marked by green and magenta boxes, at the highest heliocent… view at source ↗
Figure 6
Figure 6. Figure 6: Science verification observation on 10 June 2024 using MeerKAT observed an erupting CME. The top panels show MeerKAT radio images overlaid on 195 Å EUV images. The bottom left panel displays the 629 MHz brightness temperature map during the CME, with a point-spread-function (PSF, shown in the bottom left corner inside the white marked box) sized region highlighted, while the bottom right panel shows spectr… view at source ↗
Figure 7
Figure 7. Figure 7: Top panels: Gyrosynchrotron emission detected from a CME on 31 December 2023 using OVRO￾LWA at multiple timestamps during its propagation through the middle corona. The background in each panel shows the 48 MHz image, with overlaid contours at 34, 43, 48, 57, 71, 80, and 85 MHz, plotted at 10% of the peak brightness temperature. Point spread functions for each frequency are shown in the bottom left of each… view at source ↗
Figure 8
Figure 8. Figure 8: The solid blue curve shows the expected variation of relative rotation measure (RRM) of CMEs with heliocentric distance, with the light blue band indicating an order-of-magnitude uncertainty. Horizontal lines mark the achievable RRM precision for ∼15 minutes of integrations across different instruments and observing bands: solid for SKA precursors, dashed for SKA pathfinders, and dot–dashed for SKA bands. … view at source ↗
Figure 9
Figure 9. Figure 9: The top row shows three stages of helioschedule for ASKAP heliopolarimetry observation of a CME, and the bottom row shows the MWA observation of the same event, both triggered by helioschedule. The left panels illustrate CME detection by SEEDS using near-real-time coronagraph data, the middle panels display the calculated pointing configuration, and the right panels present the final telescope pointings us… view at source ↗
Figure 10
Figure 10. Figure 10: Rotation measure contribution from different heliospheric and ionospheric media. (Reproduced from Oberoi and Lonsdale (2012)). from enhanced UV coverage, and its extensive overall frequency range will together enable transfor￾mative advances in CME magnetic field measurements and in our understanding of CME physics. Realizing this potential, however, will require robust calibration, sophisticated data pro… view at source ↗
read the original abstract

Coronal Mass Ejections (CMEs) are large expulsions of magnetized plasma from the Sun into interplanetary space and are the primary drivers of extreme space weather variations. The strength and topology of CME magnetic fields largely determine their impact on Earth. Although visible-light coronagraphs routinely observe CMEs and provide their geometric and kinematic properties, they cannot directly measure CME vector magnetic fields. These fields evolve from initiation through the inner heliosphere due to interactions with other CMEs, coronal structures, and the ambient solar wind, leading to significant structural deformation. Such evolution complicates predictions of the CME magnetic field at Earth. Accurate measurements of CME magnetic fields in the corona and heliosphere are therefore essential for advancing space weather forecasting. Radio observations spanning MHz to GHz frequencies provide a powerful remote-sensing approach for measuring CME magnetic fields from the ground. Recent observations with Square Kilometre Array (SKA) precursors and pathfinder instruments, as well as other new-generation facilities, have demonstrated the potential of these radio techniques for CME magnetic-field diagnostics. At the same time, these studies have highlighted several limitations of current instruments. The higher sensitivity, wider instantaneous bandwidth, and broader frequency coverage of the SKA will open a new observational window, enabling these techniques to be fully exploited for constraining SpWx models and improving predictive accuracy. However, such observations are non-standard and require special consideration in scheduling, calibration, and imaging. Developments achieved with SKA precursors and pathfinders are paving the way for robust CME magnetic-field measurements with the SKA.

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

2 major / 1 minor

Summary. The manuscript argues that CME vector magnetic fields, which determine space-weather impacts and evolve during propagation, cannot be measured by visible-light coronagraphs but can be remotely sensed via radio techniques spanning MHz to GHz. Recent observations with SKA precursors and pathfinders have demonstrated the potential of these methods while exposing limitations in sensitivity, bandwidth, and frequency coverage. The paper asserts that the SKA's higher sensitivity, wider instantaneous bandwidth, and broader frequency coverage will overcome these limitations and enable the techniques to be fully exploited for constraining space-weather models, although the observations are non-standard and will require special scheduling, calibration, and imaging considerations. Precursor developments are said to pave the way for robust SKA measurements.

Significance. If the central assertion holds, the paper would usefully frame the SKA as a key facility for advancing direct remote measurements of CME magnetic fields, thereby supporting improved space-weather model constraints and predictive accuracy. It correctly identifies the observational gap left by coronagraphs and credits precursor instruments for initial demonstrations. The significance is limited, however, by the absence of any quantitative projections, error budgets, or feasibility analysis showing that SKA hardware gains will translate into usable vector B-field diagnostics.

major comments (2)
  1. [Abstract] Abstract: The claim that SKA sensitivity, bandwidth, and frequency improvements 'will open a new observational window, enabling these techniques to be fully exploited' is not supported by quantitative assessment. No error budgets, simulated imaging fidelity, or calibration-stability requirements derived from precursor studies are provided to show that the mentioned non-standard calibration and imaging challenges can be met at the level needed for vector B-field diagnostics such as Faraday rotation or gyrosynchrotron.
  2. [Abstract] Abstract: The text states that 'such observations are non-standard and require special consideration in scheduling, calibration, and imaging' yet offers no analysis or reference to SKA-specific mitigation strategies. This operational premise is load-bearing for the downstream claim of improved predictive accuracy but is asserted rather than demonstrated.
minor comments (1)
  1. [Abstract] The abbreviation 'SpWx' appears without definition; expand on first use for clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed comments, which help clarify the scope and limitations of our perspective manuscript. We address each major comment below and have revised the text to better reflect the current state of the field.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The claim that SKA sensitivity, bandwidth, and frequency improvements 'will open a new observational window, enabling these techniques to be fully exploited' is not supported by quantitative assessment. No error budgets, simulated imaging fidelity, or calibration-stability requirements derived from precursor studies are provided to show that the mentioned non-standard calibration and imaging challenges can be met at the level needed for vector B-field diagnostics such as Faraday rotation or gyrosynchrotron.

    Authors: We agree that the original phrasing was too assertive for a perspective article without accompanying quantitative analysis. The manuscript's intent is to synthesize recent precursor results and identify the observational gap rather than to deliver a full feasibility study. We will revise the abstract to adopt more measured language (e.g., 'is expected to open' and 'has the potential to enable') and will add citations to recent precursor papers that quantify sensitivity gains and discuss the remaining calibration challenges for Faraday rotation and gyrosynchrotron measurements. revision: yes

  2. Referee: [Abstract] Abstract: The text states that 'such observations are non-standard and require special consideration in scheduling, calibration, and imaging' yet offers no analysis or reference to SKA-specific mitigation strategies. This operational premise is load-bearing for the downstream claim of improved predictive accuracy but is asserted rather than demonstrated.

    Authors: We accept that the statement requires supporting references. We will add citations to SKA science operations documents and to published work on non-standard solar observing modes with SKA precursors (e.g., MWA and LOFAR solar campaigns) that outline scheduling, calibration, and imaging approaches. These references will indicate the pathways being developed rather than claiming that the challenges have already been solved at SKA scale. revision: yes

Circularity Check

0 steps flagged

No circularity; prospective claim independent of derivations or fits

full rationale

The paper is a forward-looking perspective on SKA-enabled radio diagnostics for CME magnetic fields. It contains no equations, parameter fits, or derivation chains. The central claim—that SKA sensitivity/bandwidth/frequency gains will fully exploit existing techniques—rests on hardware specifications and cited precursor observations rather than any self-definitional loop, fitted-input prediction, or self-citation load-bearing uniqueness theorem. No ansatz smuggling, renaming of known results, or reduction of outputs to inputs by construction is present. The argument is self-contained as a qualitative assessment of instrumental capabilities.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a perspective and review-style paper on observational prospects rather than a technical derivation or empirical analysis; no free parameters, axioms, or invented entities are introduced in the provided abstract.

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