the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
| 22 Apr 2026
Ion composition of the Earth plasmasphere observed by the PEP JEI and RPWI instruments on the JUICE spacecraft
Abstract. During the first Earth gravity assist maneuver of JUICE on 20th August 2024 the spacecraft passed through the Earth plasmasphere for about 2 hours. Before closest approach at a distance of 2.1 RE the Jovian Electron and Ion spectrometer JEI of the PEP instrument suite was switched on for 40 min in an ion mode test configuration. The high plasma density of about 3000/cm3 (observed by the RPWI plasma wave instrument) led to a negative charging of the spacecraft which allowed a rare observation of the cold and dense plasmaspheric ion populations. Since the ions are only corotating with the Earth at a velocity of about 1 km/s at this distance the observed ion speed is dominated by the spacecraft velocity of about 8 km/s. For this reason ions with different mass appear at different energies in the energy spectrum observed by the JEI sensor. In addition the spacecraft potential leads to specific filtering of ion masses in the observed angular distribution. By calculating the sensor response function for these specific observing conditions it is possible to quantify densities of the different ion species. But this response calculation depends critically on the response of the JEI channel electron multipliers to the ion velocity and mass. Since the sensor was operated with a low post-acceleration further laboratory calibrations may be needed for this specific setup. Still we can already conclude from the observations that ions with mass >4 amu/q contribute at least 30 % to the observed total ion density. A flux peak observed in the energy spectrum at 15 eV can only be explained by the presence of heavy molecular ions with mass ~30 amu/q. Molecular ions have only been rarely detected in the outer Earth plasmasphere. The observations indicate that the JEI sensor can also be used to achieve ion composition measurements in the exospheres of the Jovian moons.
Competing interests: At least one of the (co-)authors is a member of the editorial board of Annales Geophysicae.
Publisher's note: Copernicus Publications remains neutral with regard to jurisdictional claims made in the text, published maps, institutional affiliations, or any other geographical representation in this paper. While Copernicus Publications makes every effort to include appropriate place names, the final responsibility lies with the authors. Views expressed in the text are those of the authors and do not necessarily reflect the views of the publisher.- Preprint
(5805 KB) - Metadata XML
- BibTeX
- EndNote
Status: open (until 08 Jul 2026)
- AC1: 'Comment on egusphere-2026-2030', Markus Fränz, 20 May 2026 reply
-
RC1: 'Comment on egusphere-2026-2030', Anonymous Referee #1, 02 Jun 2026
reply
Comments on “Ion Composition of the Earth plasmasphere observed by the PEP JEI and RPWI instruments on the JUICE spacecraft”
The paper presents interesting and new observations of the cold ion population in the plasmasphere. I have a few comments and questions that should be addressed before publication.
General: The motivation for this study is very well laid out, but the results are not put into context enough. Simply comparing with old measurements is not sufficient, I would like to see some discussion on how the new findings from this study influence our general understanding of the plasmasphere and how knowledge of plasmasphere composition can advance our understanding of the wider field.
I also suggest a review of the font sizes in the figures, as some are very small (Fig. 6, 8, 14, 15).
Line by line:
L. 25 is this height or radius?
L. 26 a reference for the temperature and density would be good
l. 50 I think the reader would appreciate a short summary of the contents of that paper. Why is the cold ion population important for the magnetospheric dynamics?
l. 60 wrong parentheses on citation
Fig.1 Some of the text is overlapping in the figure. It is also unclear which direction the moon is moving.
Fig. 4 I cannot read the labels in this figure, they are too small and the contrast especially in the blue is poor.
Fig. 8 The figure should really be inverted to be printer friendly. I also recommend against the use of the rainbow colour scale, it is not colour blind friendly and the hues also do not have a linear brightness. Viridis is usually a good alternative. The same goes for the colorbar in the other figures.
L. 137 - 139 “It is interesting…” Is this statement to confirm that the spacecraft potential measured by RPWI is reasonable?
L. 142 “the asymmetric shape of the spacecraft potential” this may need some more explanation. Why is it asymmetric, how does that influence the detection direction?
l. 158 have you calculated the errors? Are they small compared to the overall counts?
l. 166 so would you characterise your values as a lower limit?
Fig. 11 Could you add error bars to the counts here? It would help to affirm the detection
l. 255 How did you get to 30%? is this from the numbers in equation 3 and the RPWI density?
l. 271-273 So could you explain at least the 15eV peak by a B parallel beam? Because the other peaks seemed less conclusive in the discussion in section 3. If you can attribute the 15eV peak to accelerated ions, then do you have sufficient evidence for the other heavy ions? What velocity would be necessary to achieve that signature with a B parallel beam? I think this one sentence needs more careful discussion.
Conclusion: I find it difficult to understand what your main conclusions are. The overall density is from RPWI and the 30% figure has not been explained sufficiently in the text. The 15eV peak could be due to magnetic field. I think there is sufficient new knowledge here, but a more precise conclusion would improve the paper. You say further laboratory calibration is needed, but why was it not included in this publication?
Citation: https://doi.org/10.5194/egusphere-2026-2030-RC1 -
AC2: 'Reply on RC1', Markus Fränz, 10 Jun 2026
reply
Since the deadline for discussion has been extended by one month to allow time for a second review,
we give a preliminary response to this review. A comprehensive response will be submitted with the revision of the paper.We thank the reviewer for the major critical points raised:
1) The main conclusion of the paper concerning the Earth plasmasphere is that we can confirm
the existence of a strong molecular heavy ion population at a distance of 2.1 R_E from Earth.
Since there has been only one comparable observation (Craven, 1985) by a special setting of
the RIMS instrument on DE-1 this is a very important confirmation which may lead to new
observation campaigns and simulations in the future.
2) The main achievement of the paper is a more technical one: we show for the first time that
the spacecraft potential can be used as a mass filter by its effect on the angular distribution
of the observed ion flux. To our knowledge this has never been described before.
3) On the effect of the magnetic field: as discussed in the paper field-parallel acceleration
of plasmaspheric plasma has been observed before at higher energies. But all observations
of this type show that this acceleration causes power law spectral tails. The spectra
observed by PEP JEI are not of this type, but they show different spectral peaks and a break-off
above 15eV which can not be explained by field-parallel acceleration. In contrast the
observations agree very well with the angular mass filtering effect described in the paper.
4) On additional tests of channeltrons at low voltage in laboratory: This requires construction
of a specific test setup by an engineering team. Since our engineering team is currently
overloaded with preparations for the RAMSES mission we can only schedule such tests
after instrument delivery for RAMSES next year. In the mean time the post-acceleration voltage
of PEP JEI onboard has been increased to -500V. We expect new observations of the plasmasphere
with this setting in September 2026.All other minor points we will address in the revision.
Citation: https://doi.org/10.5194/egusphere-2026-2030-AC2
-
AC2: 'Reply on RC1', Markus Fränz, 10 Jun 2026
reply
-
RC2: 'Comment on egusphere-2026-2030', Anonymous Referee #2, 24 Jun 2026
reply
Manuscript review
[Manuscript # doi.org/10.5194/egusphere-2026-2030]
Title: Ion composition of the Earth plasmasphere observed by the PEP JEI and RPWI instruments on the JUICE spacecraft
Author(s): M. Fränz et al.
Summary
This manuscript presents observations of cold plasmaspheric ions obtained during the first Earth gravity assist of the JUICE spacecraft on 20 August 2024. The authors analyze measurements from the PEP/JEI and RPWI instruments during a passage through the Earth's plasmasphere and report signatures for multiple ion species, including H+, He+, O+, and possibly heavier molecular ions such as N2+, NO+, and O2+. The interpretation is supported by a simplified model of ion trajectories in the spacecraft potential and by calculations of the JEI sensor response. The manuscript presents potentially unique observations, as direct measurements of cold plasmaspheric ion composition are scarce and the possibility of detecting heavy molecular ions in the outer plasmasphere is particularly intriguing. The paper is generally well written, contains a comprehensive overview of previous observations, and documents the observation geometry and instrumental setup. The main strength of the manuscript is that it goes beyond the presentation of a single Earth flyby dataset and demonstrates a potentially important new analysis capability of the JEI instrument, namely the possibility of using JEI measurements to infer the composition of cold ion populations. This aspect is likely to be particularly relevant for future JUICE observations of the exospheres of the Jovian moons. The manuscript is generally well written from both a grammatical and stylistic point of view, and the presentation is mostly clear and easy to follow. Still, several concerns regarding the interpretation of the observations and the robustness of the conclusions are discussed below. In general, I consider the manuscript suitable for publication, provided that the authors carefully address the comments below, which may help make the presented conclusions more robust and better substantiated.
General comments and suggestions
1/ The manuscript states in the Conclusions that negative spacecraft potentials have also been observed in the Jovian plasma environment and are predicted for JUICE, which supports the relevance of the present analysis for future observations near the moons of Jupiter. However, this point is only mentioned very briefly. Since one of the main motivations of the manuscript is the potential application of the JEI technique to ion composition measurements in the exospheres of the Jovian moons, I encourage the authors to discuss this connection in somewhat greater detail. In particular, it would be helpful to clarify under what plasma conditions similar negative spacecraft potentials are expected for JUICE in the Jovian system and how comparable those conditions are to the Earth plasmasphere case presented here.
2/ A substantial part of the interpretation presented in the manuscript relies on the assumed spacecraft potential structure around JUICE and on its effect on the observed ion energies and angular distributions. However, this aspect is not discussed in sufficient detail. Are there already dedicated estimates or numerical simulations of the spacecraft potential structure around JUICE available (possibly as part of Zeroual et al., 2026)? If so, I think it would be very valuable to include or discuss them in the manuscript in more detail, as they would provide a stronger physical basis for the assumed potential structure and for the interpretation of the JEI observations.
3/ The interpretation of the broad spectrum observed at theta about 33 deg as evidence for multiple ion populations and/or heavier ions is intriguing. However, the manuscript does not provide sufficient statistical context to assess how representative this spectrum is of the entire plasmasphere crossing. How frequently are such broad spectra observed? Are they consistently associated with similar energies and elevation angles, or do they represent only isolated events? Providing at least a brief overview of the occurrence frequency of these broad spectral features would considerably strengthen the interpretation. It would also help to better assess the reliability and robustness of the proposed method for inferring ion composition from JEI observations. Otherwise, it remains difficult to judge whether the inferred heavy-ion populations represent a persistent characteristic of the observed plasmasphere or are based primarily on a few selected examples.
4/ I found the definition and transformation of the relevant coordinate systems a bit difficult to follow in the current manuscript. In particular, a more explicit description of the conversion between GSE and the spacecraft reference frame (SRF) during the analyzed time interval would be very helpful, as it is not straightforward to infer this from a comparison of Figs. 4 and 5 alone. In this context, it could be useful either to plot the magnetic-field direction also in Fig. 5, or to express it explicitly in the SRF. At present, the magnetic-field information is only given in GSE coordinates in Fig. 6, while only limited information on the SRF geometry and the polar angle definition is provided in the text around line 100, with only later complementary information given in the discussion. Related to this, I found the term “polar inclination angle” somewhat confusing. The term polar angle usually refers to an angle measured from a reference axis (or normal), whereas inclination is more commonly understood as an angle measured relative to a plane. I would therefore suggest using simply polar angle (or alternatively defining the term more explicitly if a different convention is intended).
5/ I wonder whether the order of subsections 2.1 and 2.2 could be reversed. In my view, the discussion of the observing geometry would be easier to follow after first providing a clearer description of the JEI instrument itself. In addition, the current subsection 2.1 refers to other PEP sensors (e.g., NIM and JNA), which are not introduced elsewhere in the manuscript. It might therefore be useful to add a short general paragraph on the PEP instrument suite to the instrumentation subsection, in order to place JEI in context and make the discussion more self-contained.
Particular comments and suggestions
lines 9-10 - But this response -> This response...
line 12 - Still we can already conclude... -> We can conclude...
line 20 - Jovian Ion and Electron -> Jovian Electron and Ion
line 24 - The subsection title "The Earth plasmasphere" could be removed.
line 32-33 - This instrument -> RIMS instrument (?)
line 33 - mass 32 -> units amu/q?
line 48 - plasmaspheric temperature -> plasmaspheric ion temperature (?)
line 131/Figure 8 - Are these energy spectra integrated over all elevations?
line 140-142 - The manuscript invokes a possible asymmetry of the spacecraft potential structure as an explanation of the observed discrepancy between the direction of the peak counts and the spacecraft velocity vector. However, under the plasmaspheric conditions considered here, the Debye length is only of the order of centimeters, i.e. much smaller than the characteristic spacecraft dimensions. Could the authors better justify the expected magnitude and spatial extent of such asymmetries, and discuss whether they are sufficient to explain the observed ion deflections? It may also be worth commenting on whether magnetic-field effects could contribute to this discrepancy, or whether they can be safely neglected compared to the electrostatic deflection by the spacecraft sheath (ref. to paragraph lines 270+).
lines 145-147 - The sentence beginning “While an acceleration by the spacecraft potential...” is difficult to follow. At this point in the manuscript, the higher-energy spectral peaks have not yet been introduced, so the reader does not yet know what features are being referred. I suggest first introducing these additional spectral peaks explicitly and only then discussing their possible origin and significance. Furthermore, the manuscript states that the higher-energy spectral peaks were “unexpected”. However, in the presence of multiple ion species corotating with Earth, ions with different mass-to-charge ratios should naturally appear at different energies after acceleration by the spacecraft potential. Could the authors clarify in what sense these peaks were unexpected and whether they can be explained solely by the combination of corotation velocity and spacecraft acceleration?
line 166 - The rather low density can also be attributed to the spacecraft potential - see the later comment on equation B6.
line 167 - The apparent double peak in the spectrum at theta of 14.4 deg may indicate a bimodal distribution, although simple statistical fluctuations or instrumental effects should also be considered.
line 181-185 - In Fig. 12, ions are launched at a distance of 50 cm from the surface, while the Debye length estimated in the manuscript is only about 8 cm. Starting the ions at 50 cm may be reasonable if this is intended to represent a field-free region outside the sheath. However, the assumed linear potential drop from 0 V at 50 cm to -5 V at the surface appears difficult to reconcile with the quoted Debye length, since most of the potential variation should occur within a few Debye lengths. I suggest that the authors better justify the choice of the 50 cm scale length and discuss how sensitive the simulated ion deflections are to the assumed sheath thickness and potential profile. Although the SIMION method is well established, an appropriate reference could be added.
line 185-190 - Both equations (for tan(theta) and E/q) appear to contain dimensional inconsistencies, likely due to typographical errors. Please check them carefully.
line 192-193 - "Since the initial polar inclination angle is about 45 deg the expected inclination angle decreases with increasing potential." The sentence reads somewhat awkwardly. I suggest rephrasing it and briefly clarifying the underlying geometry and physical reasoning.
Figure 1 and 2 - The figures appear to use the same color-scale limits but show different colors in the plasmasphere interval. Could the authors explain this?
Figure 5 - A white background might improve the readability of the figure, in particular the visibility of the plotted directions and annotations and the SC structures.
Table 1 - It could be completed by a row for Vp = -6.5 V, as reported by RPWI measurements, for comparison.
Eq. B6 - There appears to be a typo in the expression: E^2 should likely read E. More importantly, this expression is only valid if the initial ion kinetic energy is much larger than q|Vp|, which is not the case for the present observations. The correct form would require a substitution E -> E + qVp and would therefore introduce another fitting parameter, Vp. If Eq. B6 is fitted directly to uncorrected spectra while the spacecraft potential is effectively absorbed into the fitted mean energy, the angular term remains inconsistent because it should include the correction for the potential energy as well. This may bias the fitted density, especially in the present case where the spacecraft potential is comparable to or larger than the intrinsic ion energy.
Citation: https://doi.org/10.5194/egusphere-2026-2030-RC2 -
AC3: 'Reply on RC2', Markus Fränz, 26 Jun 2026
reply
We thank the reviewer for the detailed and insightful comments. We will address all points raised by the reviewer in the revision. To animate the discussion we here give only short responses to the main points:
1) We will extend the discussion regarding the importance for observations at Jupiter. It is clear that conditions similar to the Earth plasmasphere do not exist anywhere in the Jovian environment, but the technology of mass separation using the spacecraft potential may be applicable in some regions.
2) The shape and strength of the spacecraft potential during the plasmasphere passage was simulated by Zeroual et al. using the ESA SPIS software. This analysis is described in an accompanying paper. The SPIS simulation results in a lower potential value than the one observed by RPWI. The PEP observations also support the value observed by RPWI. Important for our interpretation is mainly the small value of the Debye length which allows to regard the potential shape above the spacecraft deck as planar. This shape is also confirmed by the SPIS simulation. In the SIMION software the Debye shielding can not be simulated. The purpose of the respective figure is only to illustrate the principle of mass dependence of the polar angle. It would be possible to simulate exact ion paths using the SPIS model - which may be done in a later work. The purpose of our analytic approach is to enlighten the physical understanding.
3) The occurrence rate of the spectral peaks up to 15eV can be inferred from Figs. 8&9 of the paper. We will try to further quantify this rate in the revision and discuss whether this more energetic part is a permanent feature of the plasmaspheric ion population.
4) We will try to further clarify the coordinate systems used in the analysis. Concerning the local magnetic field vector: we can so far only use a model field vector because data of the JUICE magnetometer are still under revision.
We also thank for spotting the typo in eqn. B6. As mentioned in our previous comment eqn.1 also needs to be corrected. The revision will contain an extended analysis of a drifting Maxwellian distribution in a planar potential.
Citation: https://doi.org/10.5194/egusphere-2026-2030-AC3
-
AC3: 'Reply on RC2', Markus Fränz, 26 Jun 2026
reply
Viewed
| HTML | XML | Total | BibTeX | EndNote | |
|---|---|---|---|---|---|
| 246 | 157 | 22 | 425 | 20 | 26 |
- HTML: 246
- PDF: 157
- XML: 22
- Total: 425
- BibTeX: 20
- EndNote: 26
Viewed (geographical distribution)
| Country | # | Views | % |
|---|
| Total: | 0 |
| HTML: | 0 |
| PDF: | 0 |
| XML: | 0 |
- 1
We meanwhile noticed a mathematical error in the first equation of the paper. The impact on the results is minor. The revised version will contain an extended analysis of the phase space distribution of a drifting Maxwellian in a planar potential.