the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
Comparison of radiation belts electron fluxes simultaneously measured with PROBA-V/EPT and RBSP/MagEIS instruments
Alexandre Winant
Viviane Pierrard
Edith Botek
Abstract. Relativistic radiation belt electron observations from the Energetic Particle Telescope (EPT) onboard the PROBA-V satellite are compared to those performed by the Magnetic Electron Ion Spectrometer (MagEIS) onboard the Van Allen Probes (VAPs) formerly known as the Radiation Belt Storm Probes (RBSP). Despite their very different orbits, both instruments are able to measure fluxes of electrons trapped on a given magnetic shell. In the outer belt, the comparison of high and low altitude fluxes is performed during the first three months of 2014, featuring the most intense storms of the year. In the inner belt, measurements from the two instruments are compared only at conjunction, when the satellites are physically close to each other. Due to the low number of conjunctions, the whole period of mutual operation of both instrument is used (i.e. May 2013–October 2019). The comparisons show that flux variations appear simultaneously on both spacecraft, but the fluxes observed by the EPT are almost always lower than for MagEIS, as expected from their different orbits. In addition, this difference in flux intensity increases with electron energy. During geomagnetic storms, it is also shown that dropout events (i.e. sudden depletion of electrons) in the outer belt are more pronounced at low altitudes than near geomagnetic equator. The effect of the equatorial pitch angle value of electrons is investigated in the outer belt. The results show a good agreement between observations of the two instruments, especially if low pitch angle electrons near the equator are considered.
Alexandre Winant et al.
Status: final response (author comments only)
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RC1: 'Comment on angeo-2023-8', Anonymous Referee #1, 30 Apr 2023
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AC1: 'Reply on RC1', Alexandre Winant, 21 May 2023
Dear Editor,
I reviewed the article “Comparison of radiation belts electron fluxes simultaneously measured with PROBA-V/EPT and RBSP/MagEIS instruments” by Alexandre Winant et al. and submitted to AnnGeo.
The article is based on the comparison of electron radiation belt fluxes at low Earth orbit (LEO) and at an elliptic orbit as GTO. Proba-V/EPT is used at LEO. Van Allen Probes are used at GTO (MagEIS instrument). The difference in latitude causes the flux difference that one needs to know in order to better understand the physical processes occurring during the bounce motion of trapped electrons. Fluxes at LEO are also compared with the AE8 model. The comparison of the fluxes is made in a statistical way in the outer belt at both relativistic and ultra-relativistic energies during the year 2014. The work is very well done and results are well established. Another very interesting comparison is done at low L-shells for the few conjunction points that were found. In all cases, differences in flux are well established.
Results are at the state of the art and very interesting. The article is also well written but the organization is not fine (see my point 3 below). I am finding missing references too which I would like to see cited, including ones from the authors themselves (my point 1). Also, there are two recent publications, which the authors probably do not know, but with similar results and comparisons made. It is important to relate this study with the two articles.
These are the main recommendations I ask the authors to follow (more explanations in following). I will recommend publication of this article once the corrections are made:
Thank you for your review, comments and suggestions in order to improve our paper. The corrections in the text are in red for the removed sentences and in blue for the added sentences. Our answers are given below. Please note that the line numbers correspond to the lines of the track-changed version of the paper.
1) Missing references
Thank you for pointing out missing references. All your suggestions have be added.
- RBSP: cite Mauk et al. 2013 (The reference was added: line 36)
- MagEIS instrument : Blake et al. 2013 (This reference was added: line 91)
- Proba-V: cite the main article about that mission (is it Cyamukungu et al. 2014 ?) (A reference describing the main PROBA-V mission was added: line 37)
- Arase: cite Miyoshi et al. 2018 (SSR, ERG mission) (This reference was added: line 39)
- Radiation belt review: please cite in the introduction and refer to Ripoll, Claudepierre et al. 2020. (This reference was added: line 25)
- Please refer to Winant master thesis for further information in giving the website link. Is it relevant to do it line 208 where it is written “A similar analysis to that shown in Figure 4 was carried out for integral fluxes but is not displayed here.” (Added in line 308)
- Please refer to Viviane Pierrard, Alexandre Winant, et al. ,Simultaneous Observations of the 23 June 2015Intense Storm at LEO and GTO Orbits, URSI Radio Science Letters, Vol 4, 2022, doi: 10.46620/22-0016 (This reference was added: line 64)In saying that preliminary comparisons were provided and discuss in this article.
- Please acknowledge that the radiation belt often evolves in the plasmasphere and that wave-particle interactions that sculpt the radiation belts will be partly controlled by the local value of the plasmaspheric density. A recent review of plasmasphere modeling is available in Ripoll J-F et al. (2023), Modeling of the cold electron plasma density for radiation belt physics, Front. Astron. Space Sci. (This reference was added: line 30)
- The decrease in electron flux (MagEIS measurements) as pitch angle decreases is shown in Fig 2 of Ripoll et al. Ripoll, J.-F., Loridan, et al. (2019). Observations and Fokker-Planck simulations of the L-shell, energy, and pitch angle structure of Earth's electron radiation belts during quiet times. Journal of Geophysical Research: Space Physics, 124, 1125-1142. https://doi.org/10.1029/2018JA026111. Please cite.(This reference was added: line 177)
2) Similar comparison have recently been published in EGUsphere and should be referred to and commented
Comparisons at LEO and GTO have recently been carried in these two articles with links given below. I am assuming is that these two articles are two recent to be known by the authors.
Indeed we were not aware of those recent publications during the redaction of this paper. We have read those new studies, added and compared our results with the ones obtained with CARMEN.
1- Please cite and discuss briefly in the introduction the results in: https://ieeexplore.ieee.org/abstract/document/10078924
https://www.sciencedirect.com/science/article/pii/S0273117723000029
(Citations added in the introduction: In addition, recent studies have compared electron fluxes observed in the outer radiation belt at low and high latitudes. (Ginisty et al., 2023a) have taken advantage of the Electric Orbit Raising
(EOR) of CARMEN4 to geostationary orbit to compare simultaneous observations at LEO of CARMEN3. Both missions where developed by the Centre National d’Etudes Spatiales (CNES) and are fitted with the same instrument, the ICARE-NG
detector (Boscher et al., 2014). In this study, a linear relationship between logarithmic values of the electron fluxes ≥ 1.6 MeV45
at low and high altitude was found between L∗ = 3.5 − 4.8, where L∗ is the Roederer parameter (Roederer and Lejosne, 2018). In (Ginisty et al., 2023b) a similar comparison is undertaken between CARMEN2-3 at LEO and RBSP in the outer belt for relativistic electrons (≥ 1.6 MeV). In this work, they report that flux levels are quite similar for both mission, with a good linear correlation between L∗ = 3.5 − 4.8)2- In the main text, in the analysis, please discuss and comment the differences you find between EPT and RBSP with the differences found in the above articles between CARMEN and RBSP. My understanding is that the large differences found this article with EPT-MagEIS are not found between CARMEN (2, 3) and RBSP, in particular at high energy (and knowing differences EPT-RBSP increase with energy increasing).
This should be mentioned clearly to the readers and discussed (ideally explained but I am not sure explanations can be given).
(line 287: comparing our results with CARMEN/RBSP, especially at high energy, since we find a large difference in flux intensity, which is not observed with CARMEN. However, we seen in CARMEN/RBSP comparison that the flux at low altitude decrease more than at high altitudes, which is in agreement with what we have found with EPT)
(line 321: About integral flux comparison, we note the we have much larger correction factor than it was found with the 2 CARMEN missions between low and high altitudes. While for low equatorial pitch angle we the correction factor is similar to what was found with CARMEN, it is not the case with spin-averaged data. Especially at L = 4, 5. Moreover, we have an integral flux with energies > 500 keV while CARMEN measure the integral flux > 1600 keV. Above that energy, the difference that we would find between EPT and MagEIS would be much higher than what we have computed here.)
(line 336: Despite the differences in flux intensity that we observe with the EPT, throughout the outer belt we find a good linear correlation between low and high altitude measurements, which is in agreement with the results obtained with CARMEN)
3) The organization of the article is not fine
Indeed the structure of the paper might have been confusing. The global organization of the paper was modified as you requested.
- Please consider moving the methodology section before the world map section. (The methodology section was moved before the world map section)
- Why not integrating the world map section within the “results and discussion” section.(World map have been moved to the results and discussion section)
- The “Analysis of the EPT observations” is not an adapted title: you work with both EPT and MagEIS….. Why is this section not in the “results and discussion” section.(The name of this section was changed and moved to the results and discussion section)
- I suggest the 2 Instrument section becomes the 2 Instrument and method section, with 2.1 EPT, 2.2 MagEIS, 2.3 methodology. (The suggested structure is now used in the paper)
- Then, section 3 of results and discussion can have : 3.1 Analysis of the evolution of EPT and magEIS observations in 2014”, 3.2 Comparison with AE8 (formerly “world maps), 3.3 Comparison of outer belt fluxes, 3.4 Conjunction in the inner belt (Same as above, the suggested structure was added to the paper)
4) Writing clearly the main result
I am asking that in the analysis section of figure 4, a sentence is written and gives the correction factors between MagEIS and EPT for each of the 6 (L-shell, E). That sentence should be also copied in the conclusions. For instance: at L∼4, 5, while MagEIS 8° flux integral flux is∼20 times higher than the integral flux computed with the EPT. Please make a Table if needed to be clearer.
(Tables containing the correction factors were added both for differential fluxes and integral fluxes, for all L, E and pitch angle. For the differential fluxes, a full sentence might be to confusing to read so the reader is directed to the corresponding table.
For the integral flux, the sentence summarizing the correction factor between EPT and MagEIS was changed to explicitly tell the results found in the corresponding table:Line 315: Indeed at L = 4, 5, while MagEIS spin-averaged integral flux is 46, 48 times higher than the integral flux computed with the EPT respectively, small pitch angle fluxes are 16, 18 times higher respectively. The same is true at L = 6 where the spin-averaged MagEIS flux is 32 times larger than for the EPT and becomes 10 times larger when the integral flux is computed with 8° pitch angle electrons )
(About line 255, please give the energy at which the comparison is made.)
(The energy at which the comparison is made was added: line 367 )
So far I read in the conclusions: “but equatorial low pitch angle fluxes remain one order of magnitude higher than those at low 285 altitude in the outer belt.”. This is not accurate enough. I want clear numbers according to the (L,E) that is considered.
(line 386: This sentence was modified to be more precise: Such a reduction in flux intensity is also observed for the integral flux (> 500 keV). Spin-averaged MagEIS fluxes at L = 4, 5, 6 are 46, 48, 32 times higher than EPT fluxes respectively but equatorial low pitch angle fluxes remain one order of magnitude higher than those at low altitude in the outer belt. At L = 4, 5, 6, MagIES 8° fluxes are 16, 18, 10 times higher than EPT fluxes respectively.)
About the inner belt, it is written “A relatively good correlation is also obtained in the inner belt”. Ok, but you could be more precise: the one to one flux correspondence is excellent at 500-600 keV but decreases as energy increases (please give a number of the correction factor). (The correction factors were added in the text)
5) Other corrections
-Please rephrase “…. the inner belt, mainly composed of energetic protons, extends up to L = 2, depending on the particles energy, and presents a more stable configuration. The outer radiation belt, mainly composed of electrons, is highly sensitive ” There is an electron inner belt. Here you oppose a proton inner belt to an electron outer belt. (line 20: True, with this sentence it seem no electrons are found in the inner belt. The sentence was changed to: …the inner belt, composed of both protons and electrons of high energy, extends up to L = 2, depending on the particles energy,…)
-All references are weirdly made, for instance: “the detection of a third ultra-relativistic electron belt Baker et al. (2013)”. This should be “the detection of a third ultra- relativistic electron belt (Baker et al., 2013)” (The issue regarding the way citations were compiled by Overleaf was fixed)
-Please rephrase “Like the EPT, the Magnetic Electron Ion Spectrometer (MagEIS) is a science class spectrometer…” EPT is a telescope. MagEIS is a spectrometer. MagEIS uses a magnetic field to deviate and count a given energy range of electrons. This is a fundamentally different instrument….. Please acknowledge. Please read and cite Blake et al. 2013 about MagEIS.(line 90: A new line was added to highlight the different principle on which MagEIS is based compared to the EPT i.e. Unlike the EPT, MagEIS relies on uniform magnetic fields to focus electrons and sort their energy on a linear strip of detectors (Blake et al. 2013))
-Define clearly the ‘horns”, the ‘heart’ and the ‘arms’. You could use examples with (lat, long) if needed. (explanation added at line 186 for the horns and 193 for the heart and arms).
-Line 105: if we see so well the similarities between fig 1 and 2 why do we need fig 4 and 5. Change of argument: we see some similarities which require a more systematic one-to-one comparison in order to asses precisely the differences. BTW the differences found are large, so don’t say here that fluxes agree.
(The formulation of the sentence was changes to motivate the systematical comparison between the two instruments: line 167)
In addition, in the abstract, we removed the sentence saying that the fluxes agree and replaced it by: Despite the difference in flux intensity observed by the two instruments, especially at high energies, a linear relationship with good correlation was found. The correlation is maximum when low pitch angle electrons near the equator are considered.)
-Legend of fig 3: EPT is not ‘computed’ even if I understand you use Eq. 2 to build an integral flux. Rephrase. (In the figure caption, the word ‘computed’ was replaced by ‘retrieved’, in addition to emphasize the fact that it is not a directly measured by the EPT, a reference to the equation used to retrieve the integral flux was added)
-It is unclear how you deal with solar min and solar max. Are EPT data selected as
such? Or is it just AE8? Please explain? Why AE8 is only shown at solar max and not at solar min? Show it as well.
(We added explanations at line 200)
(We only vary the solar activity for the model while the observations of the EPT are for February 2014. The comparison with AE8 during minimum of solar activity is there to compare if the flux agreement with EPT is better than for maximum of solar activity.
In the text this was clarified: Note that for this comparison, EPT observations remain the same while only the solar activity in the model is changed. Also, in Figure 3 only the fluxes predicted by AE8 during solar maximum are displayed on the top right panel. Predictions of the model during solar minimum are not shown, since the general structure of the map is conserved while flux intensity slightly decreases in the outer belt and slightly increases in the inner belt.We feel that the addition of the flux map from the model during solar minimum does not bring a major point in the frame of this small comparison. If you still feel that this is required, we will add a figure)
-When you indicate “L~4,5,6” in many places; you can say first that the center L-shell value of the bin is used at L=4,5,6. This avoids using a ‘~’ which gives the idea the L is not known precisely while it is. Define Lc if you need. (This was changed through the entire paper as suggested. A sentence was added in the method section to clarify that when L = 5 refers to the central value of the bin.)
-Don’t write ~500 keV. Rather write 500-600 keV. Idem for 1-2.4 MeV. Don’t use ‘~’ (everywhere: text and legends) (This was also changed throughout the text)
-Line 226 in: “The same is true at L∼6 where MagEIS flux is∼30 times larger than
for the EPT and becomes∼10 times larger when the integral flux is computed with∼ 8° pitch angle electrons”. Please write it is the spin-averaged flux.
(Line 317: we specified the that the first correction factor corresponds to MagEIS spin-averaged fluxes. )
-The end of line 259 is not understandable because disconnected from the rest of the sentence: “high, and imposed corrections for MagEIS measurements Claudepierre et al. (2015).” It is possible that it is due to the coma “, and” that should be removed.
(Line 358: The sentence was changed to: The correlation coefficient (indicated at the top of the panels after the linear fit) should be taken with care since the resulted conjunction points are very few (even without the application of any additional flags for MagEIS data), in the region of the South Atlantic Anomaly where contamination from energetic protons can be high, thus imposing corrections for MagEIS measurements)
-Columns inverted in fig 4 (columns are now in correct order)
Citation: https://doi.org/10.5194/angeo-2023-8-AC1 -
AC2: 'Reply on AC1', Alexandre Winant, 21 May 2023
Please find here the document with track changes that is refeered to in the comments.
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RC2: 'Reply on AC2', Anonymous Referee #1, 25 May 2023
I have reviewed the answers of Winant et al in the attachment of AC2 and I am satisfied by:
-change in the organization of the article
-addition of the comparison with CNES measurements and its analysis
-addition of the refeneces I proposed
I move on to the next comment (AC3) to continue my report.
Citation: https://doi.org/10.5194/angeo-2023-8-RC2
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RC2: 'Reply on AC2', Anonymous Referee #1, 25 May 2023
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AC3: 'Reply on AC1', Alexandre Winant, 22 May 2023
Please find my answers to your comments (in AC1) in the form of a .dox file
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RC3: 'Reply on AC3 (with recommendation for publication)', Anonymous Referee #1, 25 May 2023
As just indicated in my reply to AC2 (RC2), I am satisfied by the answers of the authors. Here I could download the revised manuscript and see how their answers were integrated in it. I am very satisfied as well. The authors have done tremendous work in correcting their article and integrating their answers (new organisation, new discussion of the CNES results, new references). I did find very minor corrections which I attach here through my annotated revised version. As an important last correction I ask, I would like the main conclusions which the authors draw about their comparison with CNES CARMEN measurents in the text to be briefly reported in the conclusion section. As such, I am positive for the publication of this article. (Please note that the interface does not allow me to post my final review yet and to accept the article. I think that will be possible once the editor validates my comments and closes the interactive discussion.)
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AC4: 'Reply on RC3', Alexandre Winant, 26 May 2023
Thank you for those comments and suggestions.
Please find the last version of the track change version of the paper.About the section numbers: Note that in the track-change version of the paper, the number of the sections are not changed properly but in the final version it will be correct.
About the level 3 data: added sentence at line 105: “MagEIS level 2 and level 3 data were retrieved from https://rbsp-ect.newmexicoconsortium.org/data_pub/ and only the background corrected MagEIS electron fluxes have been used all along the present work. Level 2 data are the spin-averaged (averaged on the spin of the spacecraft) fluxes measured by the instrument, while level 3 data provide fluxes of electrons in given pitch angle bins.“
About the tables: The tables ordering was changed as you suggested it.
About the CNES measurements: as small paragraph was added in the conclusion at line 417:“ The comparison between CARMEN and RBSP performed by \cite{ginisty2023carmenRBSP} show a better agreement between the integral fluxes intensity measured at low altitude and high altitude than what is found with the EPT, especially considering that the lower energy threshold of CARMEN fluxes is 1600 keV, the energy at which the difference in intensity between EPT and MagEIS is the largest. The different results obtained in that work and our investigations may partially be explained by the different orbits of the PROBA-V and Jason 2, 3 satellites. Despite those differences, in both studies, dropout events are more important at LEO than at MEO, and in addition a good correlation between LEO and MEO fluxes is found.”
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RC4: 'Reply on AC4', Anonymous Referee #1, 26 May 2023
Ok, these corrections are good for me. Thank you. I need the editor to give me the hand to accept the article.
Citation: https://doi.org/10.5194/angeo-2023-8-RC4
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RC4: 'Reply on AC4', Anonymous Referee #1, 26 May 2023
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AC4: 'Reply on RC3', Alexandre Winant, 26 May 2023
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RC3: 'Reply on AC3 (with recommendation for publication)', Anonymous Referee #1, 25 May 2023
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AC2: 'Reply on AC1', Alexandre Winant, 21 May 2023
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AC1: 'Reply on RC1', Alexandre Winant, 21 May 2023
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RC5: 'Comment on angeo-2023-8', Anonymous Referee #2, 28 May 2023
This paper has shown a comparison between PROBA-V/EPT and RBSP/MagEIS instruments which had observed different altitudes in the radiation belts. The authors used L-shell sorted data to compare two satellite data, and a result of comparison seems to be good. The paper is well written and organized, but I have a couple of questions which the authors may consider.
1) Adiabatic effect at the low-altitude satellite observation
Tu and Li[2011, JGR, 10.1029/2011JA016468] has discussed the adiabatic loss effects at the low altitudes through variations of the mirror point altitudes. I suppose that the PROBA-V/EPT data has included such effect which causes differences from the RBSP observations. Could you discuss this point, especailly for the low flux time interval of PROBA-V?
2) L-shell definition
The authors have used McILwain L value for comparison of both satellites? Is this enough to compare two satellite data at different altitudes? I suggest the authors should use Roeder L* using the time-variable Tsyganeneko-04 or later model and include dicsussion how the authors confirm the accuracy of the field line mapping between two satellites.
Minor comments:
page 2: Please include XEP as well as HEP for Arase and relavant references (Miyoshi et al., 2018, , Earthe Planet and Space, doi: 10.1186/s40623-018-0862-0, Mitani et al, 2018, Earthe Planet and Space, doi 10.1186/s40623-018-0853-1, Higashio et al., 2018, Earthe Planet and Space, doi:10.1186/s40623-018-0901-x), and MagEIS (Blake et al., Space Sciece Review, 2013, doi:10.1007/s11214-021-00855-2)
Citation: https://doi.org/10.5194/angeo-2023-8-RC5
Alexandre Winant et al.
Alexandre Winant et al.
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