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A coronal mass ejection encountered by four spacecraft within 1 au from the Sun: Ensemble modelling of propagation and magnetic structure

T0 review · 3 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read Ensemble predictions of a CME's magnetic field spread more widely with heliocentric distance, implying a limit to how far an inner probe can anchor an outer probe's forecast.

desk verdict A genuinely rare four-probe CME event, carefully analysed; the ensemble-divergence conclusion is a useful hypothesis that still needs a structured-wind test before it becomes a general claim. read the letter →

arxiv 2411.12706 v1 pith:2DK7IYAE submitted 2024-11-19 astro-ph.SR physics.space-ph

Erika Palmerio , Christina Kay , Nada Al-Haddad , Benjamin J. Lynch , Domenico Trotta , Wenyuan Yu , Vincent E. Ledvina , Beatriz Sánchez-Cano
show 6 more authors
Pete Riley Daniel Heyner Daniel Schmid David Fischer Ingo Richter Hans-Ulrich Auster
This is my paper · ORCID
classification astro-ph.SRphysics.space-ph
keywords coronalmassejectionsmulti-spacecraftobservationsensemblemodellingfluxropemagneticstructureinnerheliospherespaceweatherforecastingstreamer-blowoutCMEOSPREI
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 analyses a slow, streamer-blowout CME that erupted from the Sun on 23 September 2021 and was encountered in situ by four spacecraft spread almost evenly in heliocentric distance between 0.4 and 1 au. It is, to the authors' knowledge, the first reported CME observed by four well-radially-separated probes inside 1 au. Using the OSPREI modelling suite in a 200-member ensemble hindcast, the authors find that the spread of predicted in-situ quantities grows with heliocentric distance: the best-fit solution at an inner probe is not necessarily a good fit at an outer probe. They argue from this that there may be a maximum angular and radial separation between inner and outer probes beyond which inner-probe measurements lose power to constrain the magnetic field orientation at 1 au. The result matters because space weather forecasts increasingly use upstream inner probes to predict what will hit Earth, and this event gives a concrete test of how far that strategy can work.

What carries the argument

The argument is carried by the OSPREI modelling suite in ensemble mode. OSPREI chains three analytic modules: ForeCAT, which computes coronal deflections and rotations of the CME's flux rope; ANTEATR, which propagates the CME through interplanetary space and builds the sheath; and FIDO, which generates synthetic in-situ time series along a chosen observer trajectory. The CME body is described by an elliptic-cylindrical flux rope, and 200 ensemble members perturb 24 input parameters (position, tilt, speed, mass, magnetic field, solar wind conditions) around a seed run. A goodness-of-fit score, the sum of fractional mean absolute errors on hourly averaged field and plasma quantities plus a timing error for the shock and ejecta boundaries, selects the best member at each spacecraft and globally.

What would settle it

Run the same 200-member OSPREI ensemble for a CME encountered by outer probes at separations between 0.1 and 0.6 au and measure whether the spread in predicted magnetic field orientation grows monotonically with separation; if an outer probe close in angle but far in radius shows no divergence, or a nearby probe shows large divergence, the proposed threshold picture collapses.

Watch

Extended reading notes

Core claim

The central claim is that for this event, the ensemble spread in predicted magnetic field and plasma quantities increases with heliocentric distance, and that this points to a practical limit on using inner spacecraft to constrain outer-spacecraft forecasts. The four probes, at about 0.44, 0.61, 0.78, and 0.96 au, all encountered the same CME, and OSPREI's seed run reproduced arrival times within the usual few-hour-to-10-hour uncertainty at all four. But in the 200-member ensemble, the single-spacecraft "best-fit" members for Bepi and Solar Orbiter become outliers by the time they are propagated to Parker Solar Probe and STEREO-A, while the same member that best fits PSP also best fits STEREO-A. At their CME arrival times, STEREO-A was separated from Bepi by 0.52 au and 12 degrees, from SolO by 0.35 au and 11 degrees, and from PSP by 0.18 au and 5 degrees; the authors propose that beyond some separation like these, inner-probe constraints on the in-situ magnetic field orientation, parameterised through flux rope geometry, increasingly diverge. They also show that mirroring all four encounters to the south of the modelled CME nose fixes a systematic sign error in the radial magnetic field component, suggesting the real CME deflected north of the simulated trajectory.

Load-bearing premise

The simulation treats the solar wind as a uniform, unchanging background, so any real solar-wind structures that bend or twist the CME on its way from 0.4 to 1 au are omitted.

Editorial extensions

If this is right

  • The same CME can be consistently identified at four probes from 0.4 to 1 au, and an analytic ensemble model can place all four arrivals within a few hours of observation.
  • Inner-probe data become a weaker constraint on outer-probe magnetic field orientation as the angular and radial separation grows; beyond some threshold, the best inner solution can mispredict arrival time by about 12 hours and field magnitude by roughly a factor of two at 1 au.
  • A sub-au probe near Venus's orbit is a plausible sweet spot for 1 au forecasts, close enough to remain correlated and far enough ahead to give lead time.
  • A systematic sign error in the predicted radial magnetic field can be traced to the assumed CME nose latitude, making the $B_R$ component a useful diagnostic of whether a crossing is north or south of the CME apex.

Reading between the lines

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

  • Editorial extension: a robust separation threshold would give a design rule for future heliospheric constellations, placing upstream monitors below roughly 0.2 au and a few degrees of angular separation to keep inner-outer correlation useful.
  • Editorial extension: because OSPREI assumes a uniform constant solar wind, the growing ensemble spread is a lower bound; realistic stream interaction regions and sector boundaries would add deflections and rotations that make inner-outer correlation fail at even smaller separations.
  • Editorial extension: the paper's mirroring exercise suggests a cheap test: compare the sign of the radial magnetic field across multiple spacecraft to estimate the CME nose latitude, an observable constraint independent of flux rope fitting.
  • Editorial extension: the divergence trend could be checked against metric choice; using dynamic time warping or other shape-sensitive scores might identify different "best" members, so a robustness study over metrics is a natural next step.
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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

3 major / 5 minor

Summary. The paper analyses the 23 September 2021 slow streamer-blowout CME that was observed in situ by BepiColombo, Solar Orbiter, Parker Solar Probe, and STEREO-A at heliocentric distances between 0.4 and 1 au. The authors identify shocks, sheaths, ejecta and core flux ropes at each spacecraft, perform EFF flux rope fits, and run a 200-member OSPREI ensemble in hindcast mode. They report that the spread in predicted in-situ quantities grows with heliocentric distance, and interpret this as evidence for a maximum angular/radial separation beyond which inner-probe constraints on the magnetic field orientation lose power. They also claim priority for the first four-probe radially-separated encounter inside 1 au.

Significance. The manuscript is a valuable contribution in the sense of documenting a rare multi-spacecraft CME encounter inside 1 au with consistent in-situ signatures across four probes. The OSPREI ensemble setup is open and reproducible, the WSA-Enlil comparison provides an independent arrival-time check, and the authors are transparent about many limitations. However, the central interpretive claim about the distance-dependent divergence of magnetic field predictions is not yet established as a general result: it is conditional on the uniform-wind simplification in OSPREI and on a trajectory that appears systematically offset given the wrong B_R sign. If the authors can either temper the claim or demonstrate robustness to structured solar wind, this would become a solid reference case for multi-probe CME modelling.

major comments (3)
  1. [Abstract, Sections 4.1 and 5.2] The central conclusion—that the ensemble spread in predicted in-situ quantities increases with heliocentric distance and that there is a maximum angular/radial separation beyond which inner-probe constraints on magnetic field orientation lose power—is derived from OSPREI runs that assume a constant, uniform solar wind background, as stated in Section 4.1 and Section 5.2. This assumption excludes interplanetary deflections and rotations by construction, so the growing spread reflects only the propagation of input-parameter uncertainties through a homogeneous expansion. The abstract and Section 6 present this result without the uniform-wind caveat; I recommend either softening the claim to a model-dependent result or adding a test with a structured background to show it is not an artifact of the missing physics.
  2. [Section 5.2, Figure 11] The seed run predicts the wrong sign of B_R at all four spacecraft, and the only way agreement is reached is by artificially mirroring each spacecraft crossing to the opposite side of the CME nose (Figure 11). This is direct evidence that the modelled heliospheric trajectory—and hence the CME nose latitude used to define the encounter geometry—is systematically incorrect. Because the 'best-fit' ensemble members are ranked by comparison with the observed profiles, the divergence of best-fit solutions with distance (Figure 9) may be an artifact of this geometric offset rather than a robust property of the CME. The paper should quantify how the mirroring changes the best-fit ranking and the divergence trend, or at minimum present the divergence result as conditional on the assumed trajectory.
  3. [Section 4.2] The ensemble 'best-fit' solutions are selected by comparing synthetic profiles to the same in-situ data used to set the seed parameters and the ensemble ranges (Table 4). This is a hindcast, as the paper states, but the abstract's phrase 'spread in the predicted quantities' and the discussion of using inner-probe observations 'to constrain predictions' could be misread as an out-of-sample forecast result. The divergence of the best-fit members is a measure of model sensitivity within a hindcast setup, not of predictive skill. Please rephrase the abstract and Section 5.2 to make this distinction explicit.
minor comments (5)
  1. [Table 2] The shock parameters in Table 2 are reported without uncertainties, even though the analysis uses averaging windows of 1 to 8 minutes; please provide uncertainty ranges or state that the variations are negligible.
  2. [Table 3] The EFF flux rope fit parameters in Table 3 include goodness-of-fit values but no parameter uncertainties; given the SolO trailing-edge data gap and the STEREO-A double-peak profile, a discussion of fit parameter confidence would strengthen the comparison.
  3. [Section 3.2] The SolO ejecta trailing edge is defined only by a data gap, and the flux rope fit is truncated at that boundary; the paper notes this, but it should explicitly state how a different choice of the trailing boundary would affect the fitted axis orientation and the multi-spacecraft comparison in Figure 10.
  4. [Section 6] The claim to be the 'first report of an event being observed in situ by four well-radially-separated probes inside 1 au' needs a supporting citation or a search statement; as written, it is a strong priority claim that is not documented.
  5. [Throughout] There are a number of minor language issues, for example 'in in Figure 4(b)' in Section 3.2 and 'different than' in Section 3.2; a careful proofread would resolve these.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: divergence finding is a forward-ensemble result, not a fitted prediction.

full rationale

The paper's central finding—that OSPREI ensemble predictions diverge with heliocentric distance and that inner-probe best-fit runs need not fit outer probes—is a forward-model property, not a quantity fitted into existence. The seed and ensemble runs are generated by propagating perturbed input parameters through OSPREI (Sections 4.1–4.2), and the in-situ data are used only in post-processing to label 'best-fit' members via a goodness-of-fit metric; the ensemble spread itself is computed before and independently of that labelling. No equation in the paper defines the target result in terms of its inputs: the divergence statistic is not an input parameter, and no fitted coefficient is renamed as a prediction. The paper explicitly labels the exercise a 'hindcast' and discloses that the solar wind background is uniform, and that the observed B_R sign required an ad-hoc mirroring of crossings; these are limitations on physical validity and generality, but they do not make the derivation circular. Self-citations to OSPREI and its modules (Kay et al. 2022a, etc.) document the model implementation, but the model is benchmarked here against four independent spacecraft data sets, so the citations are not load-bearing. I find no circular step.

Assumptions & free parameters 8 free parameters · 5 assumptions · 0 invented entities

The central modelling claim rests on a large set of hand-chosen seed parameters and ensemble ranges (Table 4), plus the assumption of a uniform solar wind background. No new physical entities are introduced. The EFF flux rope fits are derived measurements used for comparison, not model inputs.

free parameters (8)
  • Seed CME position and tilt (theta0, phi0, psi0) = (-29 deg, 350 deg, 60 deg)
    Chosen from AR/PIL observations (Section 4.1, Table 4); ensemble variations +/-3, +/-5, +/-10 deg.
  • Seed CME magnetic field, mass, temperature (B_FR, M_FR, T_FR) = 2.0e3 nT, 1.0e16 g, 1.5e5 K
    Described as 'best-guess approximations' (Section 4.1); ensemble +/-0.5e3 nT, +/-0.5e16 g, +/-0.5e5 K.
  • Seed CME morphology (AW, AW_perp, delta_AX, delta_CS) = 36 deg, 15 deg, 0.7, 0.9
    Loosely based on GCS reconstructions with modifications for EC model stability (Section 4.1).
  • Seed CME kinematics (V0, a0, V1, a1) = 50 km/s, 1.7 Rsun, 390 km/s, 8.0 Rsun
    Selected from off-limb LASCO observations (Section 4.1).
  • Interplanetary defaults (gamma, f_exp, C_d) = 1.33, 0.5, 1.0
    Left at OSPREI defaults (Section 4.1); varied in the ensemble.
  • Background solar wind (V_SW, B_SW, N_SW, T_SW) = 340 km/s, 5 nT, 10 cm^-3, 6.0e4 K
    Taken from STEREO-A pre-CME measurements, with V_SW lowered to match SolO (Section 4.1).
  • PFSS source surface radius (R_SS) = 2.5 Rsun
    Selected after testing 1.9, 2.1, 2.3 Rsun with 'no significant differences' (Section 4.1).
  • EFF flux rope fit parameters at four spacecraft = See Table 3 (e.g., Bepi: Theta0=39 deg, Phi0=46 deg, B0=82 nT, p0=0.23, tau=20 h)
    Fitted to in-situ magnetic field and, where available, speed profiles; used to characterize the flux rope at each probe (Section 3).
assumptions (5)
  • domain assumption The four spacecraft all encountered the same CME, specifically the second streamer-blowout from AR 12871 on 23 September 2021.
    Supported by WSA-Enlil and OSPREI arrival times and similar B_T/B_N trends, but multiple concurrent eruptions create ambiguity (Sections 2.2, 3, Appendix A).
  • domain assumption OSPREI's analytic flux rope model (EC) with a constant, uniform solar wind background adequately captures CME propagation for this study.
    Explicitly stated in Sections 4.1 and 5.2; no heliospheric deflections or rotations are modelled.
  • domain assumption The GCS reconstruction of the CME direction and the positive chirality inferred from remote sensing are correct.
    GCS is fitted by eye with acknowledged uncertainty (Section 2.2); chirality is inferred from PEA skewness (Section 4.1).
  • domain assumption The flux rope boundaries (ejecta, core) identified manually in in-situ data are correct.
    Boundaries are determined by visual inspection; SolO trailing edge is a data gap (Section 3).
  • standard math Standard PFSS and WSA-Enlil models provide valid background solar wind for the event.
    Used to generate coronal fields and heliospheric propagation (Sections 2, 4, Appendix A).

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Cite this review

Pith. "Pith review of A coronal mass ejection encountered by four spacecraft within 1 au from the Sun: Ensemble modelling of propagation and magnetic structure." pith.science (2026). https://pith.science/paper/2DK7IYAE

@misc{pith2026241112706,
  author       = {Pith},
  title        = {Pith review of: A coronal mass ejection encountered by four spacecraft within 1 au from the Sun: Ensemble modelling of propagation and magnetic structure},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/2DK7IYAE}},
  note         = {Machine review of arXiv:2411.12706}
}
read the original abstract

Understanding and predicting the structure and evolution of coronal mass ejections (CMEs) in the heliosphere remains one of the most sought-after goals in heliophysics and space weather research. A powerful tool for improving current knowledge and capabilities consists of multi-spacecraft observations of the same event, which take place when two or more spacecraft fortuitously find themselves in the path of a single CME. Multi-probe events can not only supply useful data to evaluate the large-scale of CMEs from 1D in-situ trajectories, but also provide additional constraints and validation opportunities for CME propagation models. In this work, we analyse and simulate the coronal and heliospheric evolution of a slow, streamer-blowout CME that erupted on 23 September 2021 and was encountered in situ by four spacecraft approximately equally distributed in heliocentric distance between 0.4 and 1 au. We employ the Open Solar Physics Rapid Ensemble Information (OSPREI) modelling suite in ensemble mode to predict the CME arrival and structure in a hindcast fashion and to compute the "best-fit" solutions at the different spacecraft individually and together. We find that the spread in the predicted quantities increases with heliocentric distance, suggesting that there may be a maximum (angular and radial) separation between an inner and an outer probe beyond which estimates of the in-situ magnetic field orientation (parameterised by flux rope model geometry) increasingly diverge. We discuss the importance of these exceptional observations and the results of our investigation in the context of advancing our understanding of CME structure and evolution as well as improving space weather forecasts.

Figures

Figures reproduced from arXiv: 2411.12706 by the authors.

Figure 1
Figure 1. Position of planets and spacecraft within 1 au from the Sun on 23 September 2021 at 04:30 UT, i.e. around the CME eruption time. The longitude of the CME source region is indicated with an arrow emanating from the surface of the Sun. The four probes that encountered the event under study are connected to the centre of the Sun via dashed lines. The orbits of Mercury, Venus, and Earth are also shown. 2011; Lugaz et al… view at source ↗
Figure 2
Figure 2. (c)) in addition to the PEA systems identified in STEREO-A imagery (arrows in [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: In-situ measurements of the 23 September 2021 CME at (a) Bepi, (b) SolO, (c) PSP, and (d) STEREO-A. Each plot shows, from top to bottom: magnetic field magnitude, magnetic field components in Radial–Tangential–Normal (RTN) coordinates, latitudinal and longitudinal angl…
Figure 5
Figure 5. Figure 5: Input photospheric conditions employed for the OSPREI simula￾tion. (a) HMI (pole-filled) synchronic map for 2021-09-23 12:00 UT with the HCS resulting from four different PFSS source surface heights overlaid in shades of green. The magnetogram has been saturated to ±10…
Figure 6
Figure 6. Figure 6: Overview of the (a) coronal and (b) heliospheric evolution of the CME modelled as the seed run for OSPREI. (a) ForeCAT deflections and rotations up to 20 𝑅◦. (b) Snapshot of the CME evolution in interplanetary space as seen from (left) the equatorial and (right) the no…
Figure 7
Figure 7. Figure 7: Overview of the OSPREI seed simulation run results shown against in-situ measurements of the 23 September 2021 CME at (a) Bepi, (b) SolO, (c) PSP, and (d) STEREO-A. Each plot shows, from top to bottom: magnetic field magnitude, magnetic field Cartesian components in RT…
Figure 8
Figure 8. Figure 8: Overview of the (a) coronal and (b) heliospheric evolution of the (200-member) ensemble CME run modelled with OSPREI. (a) ForeCAT deflections and rotations up to 20 𝑅◦. The seed run as well as the various best-fit runs are highlighted in different colours, whilst the r…
Figure 9
Figure 9. Figure 9: Overview of the OSPREI (200-member) ensemble simulation run results shown against in-situ measurements of the 23 September 2021 CME at (a) Bepi, (b) SolO, (c) PSP, and (d) STEREO-A. The seed run as well as the various best-fit runs are highlighted in different colours,…
Figure 10
Figure 10. Figure 10: Ejecta magnetic fields of the 23 September 2021 CME as observed by Bepi, SolO, PSP, and STEREO-A, normalised in duration so that each of the leading and trailing edges are aligned. The time series for (from top to bottom) field strength, (RTN) Cartesian field componen…
Figure 11
Figure 11. Figure 11: Overview of the OSPREI seed simulation run results with latitudinally-mirrored (with respect to the CME nose) spacecraft crossings shown against in-situ measurements of the 23 September 2021 CME at (a) Bepi, (b) SolO, (c) PSP, and (d) STEREO-A. All panels and paramete…

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    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.stat...

Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.