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REVIEW 4 major objections 4 minor 55 references

The Spatiotemporal Structure of Induced Magnetic Fields in Callisto's Plasma Environment due to their Propagation with MHD Modes

T0 review · 4 major / 4 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read The paper claims that Callisto's low-frequency induced magnetic fields are carried by anisotropic, finite-velocity MHD modes rather than arriving as an instantaneous vacuum dipole, so standard induction estimates are biased by tens of…

desk verdict A physically motivated MHD-transport correction to Callisto induction inversions; the asymmetry is robust, but the headline amplitudes and phase delays are conditional on source location and plasma parameters. read the letter →

arxiv 2411.15938 v1 pith:NWRPTNSU submitted 2024-11-24 astro-ph.EP physics.space-ph

David Strack , Joachim Saur This is my paper · ORCID
classification astro-ph.EPphysics.space-ph
keywords CallistoinducedmagneticfieldmagnetohydrodynamicsMHDwavepropagationGalileoflybysmoon-magnetosphereinteractioninductionphaseshiftplasmaenvironment
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

The paper argues that the induced magnetic fields Callisto generates in Jupiter's rotating magnetosphere do not travel to a spacecraft through empty space, as the standard induction formulas assume, but are carried by slow, anisotropic plasma (MHD) waves moving at a few hundred kilometers per second or less. On that basis it shows that ignoring transport biases the inferred induction signal: on the upstream side the field is compressed and its amplitude underestimated by about 26%, while downstream the field stretches out and is overestimated by about 39%. Transport also adds an extra phase delay between the source and the magnetometer that varies with location and can reach several to tens of degrees of the 10.18-hour driving period. The authors build this into a numerical MHD model of Callisto's plasma interaction and find the transported signals fit Galileo's C03 and C09 flyby data better than the vacuum superposition does. If correct, every prior and future inversion of Callisto's induction signals that assumes instantaneous vacuum propagation carries a systematic bias.

What carries the argument

The load-bearing device is a single-fluid MHD simulation of Callisto's interaction with Jupiter's magnetospheric plasma, with the induced field injected as a prescribed dipole field at the inner boundary at Callisto's radius (or the top of a thin ionosphere) and propagated through the inhomogeneous plasma self-consistently with the flow. The comparisons that carry the argument are a reference run without induction, whose output is subtracted to isolate the transported induced field, and a superposition model that naively adds the vacuum dipole to the reference run; the difference between those two defines the transport effect. The specific MHD features doing the work are the fast mode's anisotropic group velocity, the slow and Alfvén modes' inability to cross magnetic field lines, and the convection mode's purely downstream transport, all slowed by the dense, freshly ionized atmosphere.

What would settle it

Send a spacecraft through Callisto's near field at the same geocentric distance on both the upstream and downstream sides during the same 10.18-hour illumination cycle and compare the amplitude and phase of the induction signal: the vacuum formula predicts identical amplitudes and zero transport phase, while this model predicts about 26% smaller amplitude upstream, about 39% larger downstream, and phase shifts growing from about 0.3 degrees at the closest point to several degrees or more where convection dominates.

Watch

Extended reading notes

Core claim

The central claim is that, at the frequencies of Jupiter's ~10-hour magnetic variation, the ordinary electromagnetic mode cannot propagate in the dense magnetized plasma around Callisto because the wave frequency is far below the electron plasma and ion cyclotron frequencies; the induced field must therefore propagate as MHD slow, fast, and Alfvén modes plus the downstream convection mode. Because these modes have finite, density- and direction-dependent velocities, the induced field measured away from the moon is not the instantaneous dipole of the standard vacuum formula. The paper shows quantitatively that the result is an upstream/downstream asymmetry — compressed upstream, stretched downstream — and that a fitter using the vacuum formula would recover an amplitude 20–36% too low upstream and 37–53% too high downstream, roughly independent of the true amplitude. It further shows that the transport time across 0.25 of Callisto's radius averages about 32 seconds (up to several thousand seconds for convection in the near wake), adding an observer-position-dependent phase shift beyond the induction phase, and that incorporating these effects improves agreement with the Galileo C03 and C09 magnetometer data.

Load-bearing premise

The quantitative size of the effect rests on prescribing the induced dipole at Callisto's surface with an artificially stretched atmosphere and a reduced ionization rate, because a realistic dense ionosphere would shift the source to the top of the ionosphere and shorten the propagation path.

Editorial extensions

If this is right

  • Inverting a C09-type upstream flyby with the vacuum formula will underestimate the true induction amplitude by about 26%, while a C03-type downstream flyby will overestimate it by about 39%, so ocean and ionosphere conductivity inferences shift in opposite directions depending on flyby geometry.
  • Near the wake, transport delays can exceed 10 degrees of the 10.18-hour driving phase, so an observed signal may correspond to a noticeably weaker or stronger earlier primary field than assumed, changing the apparent timing of the induction response.
  • For future Europa Clipper and JUICE flybys, each encounter needs its own plasma-environment treatment because the correction depends on local plasma density, convection speed, and observer position.
  • Where the upstream plasma is dilute, the transport correction shrinks and the vacuum superposition becomes a better approximation, so the effect is strongest for high-density, strongly interacting flybys.
  • Because the amplitude bias scales almost linearly with the true induction amplitude, existing forward models can be patched with a multiplicative transport factor rather than requiring a different induction mechanism.

Reading between the lines

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

  • This suggests the same upstream/downstream amplitude split should be present in Galileo's other Callisto passes, which could be checked by re-fitting those data with a per-flyby transport factor.
  • If Callisto's real ionosphere is dense enough to be the induction source, the effective emission surface sits higher up, so the transport path and its corrections are probably smaller than the paper's headline numbers; those numbers should be read as upper bounds on the effect.
  • A practical upgrade to standard induction inversions would be to multiply the vacuum dipole by a geometry-dependent transport tensor rather than a single amplitude factor, since the ratio of transported to vacuum field is anisotropic.
  • A direct observational test would be a future flyby measuring the phase of the induction signal at two radially separated points along the same magnetic field line, where the phase difference should match the integrated MHD slowness rather than vanish.
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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

4 major / 4 minor

Summary. The paper argues that the low-frequency (10-hour period) induced magnetic field at Callisto cannot propagate through the surrounding magnetized plasma as an ordinary electromagnetic wave, but must instead propagate via the anisotropic, finite-velocity MHD modes (fast, slow, Alfven, and convection). Using a three-dimensional MHD model with a prescribed dipole boundary condition at Callisto's surface, the authors study the spatial and temporal modifications of the induced field. In a symmetric model they find an upstream/downstream asymmetry: relative to a vacuum superposition, the induced field amplitude is underestimated upstream (by ~26%) and overestimated downstream (by ~39%), and they report additional phase shifts of 'several to tens of degrees.' They also apply the model to Galileo's C03 and C09 flybys and conclude that including transport effects is qualitatively consistent with the magnetometer data, especially when the upstream plasma density is reduced by an order of magnitude.

Significance. The claim that induction signals at Callisto are not instantaneously propagated through a vacuum, but are instead carried by MHD modes with finite velocity and anisotropic structure, is physically well motivated and, if correct, would affect the interpretation of all past and future Callisto induction analyses, including those using the vacuum dipole formula. The paper provides a clear physical argument (Section 2), an openly available numerical implementation, and a symmetric-model prediction of an upstream/downstream asymmetry that is genuinely not fitted to the flyby data. These are strengths. However, the quantitative headline numbers (26%, 39%, phase shifts of several to tens of degrees) are conditional on parameter choices that the authors themselves describe as artificial, and the temporal interpretation relies on a timescale that is not shown to be the steady-state phase lag. The study is therefore a valuable and potentially publishable contribution, but its quantitative claims require substantial additional support before they can be taken at face value.

major comments (4)
  1. [Section 4.2, Appendix A2, Table 1] The amplitude corrections (26% upstream underestimation, 39% downstream overestimation, Figs. 5-7) are computed in a symmetric model with an artificially enhanced scale height H = 230 km and an ionization frequency reduced to 1/25 of the photoionization rate. Appendix A2 states explicitly that with a regular ionization rate a dense ionosphere builds up and would suppress propagation from the surface, in which case the induced field would propagate from the top of the ionosphere. The paper does not simulate this alternative source-location scenario, so the quoted percentages are conditional on a particular (and arguably non-representative) density configuration. The claim in A2 that the low-νion run 'covers both extreme cases' is not demonstrated, because moving the source outward by several scale heights shortens the dense, slow propagation path and is expected to reduce both the amplitude and phase corrections. A sensitivity study varying H, νion, and the source altitude is needed to make the quantitative results robust.
  2. [Section 4.3, Eq. (17), Figures 4, 9e, 10e] The abstract and Section 7 claim additional phase shifts of 'several to tens of degrees,' but the wave-front propagation times obtained from Eq. (17) yield only 0.3 degree in the symmetric model and 0.2-1.4 degrees for the flybys (Figs. 9e and 10e). The larger values are inferred in Section 4.3 from the time required for the wave pattern to become stationary after a pulsed excitation. For a sinusoidally driven system, the steady-state phase lag at an observer is set by the wave travel time (and possible reflections), not by the transient build-up time. The manuscript does not establish a connection between the standing-wave establishment time and the actual phase shift of a continuous 10-hour-period signal. A simulation with a sinusoidal boundary condition or an analytical derivation of the steady-state phase lag is required to support the claimed temporal effect.
  3. [Section 5, Figures 9-10, Table 1] The flyby case study is presented as evidence that transport effects are 'consistent with' the C03 and C09 measurements, but the comparison is qualitative and involves two adjustable choices: the background field B0 is obtained by fitting second-order polynomials to the same C03/C09 magnetometer data, and the upstream plasma density is reduced by an arbitrary factor of 10 to improve the fit. No quantitative goodness-of-fit metric is provided, and the paper acknowledges that the high-density model fits poorly (the C03 panel shows a 'poor' qualitative fit). This does not invalidate the modeling exercise, but it means the observational consistency claim is not a strong validation of the quantitative transport magnitudes. The authors should either present a statistical comparison or phrase the conclusion as an illustrative case study rather than a confirmation.
  4. [Section 2, Section 3.2] The argument that the ordinary electromagnetic mode cannot propagate is based on the cutoff condition ω << ωpe, ωci. This is correct for free linear waves, but the induced field at Callisto is a quasi-static, forced magnetic perturbation rather than a freely propagating wave. While the MHD-mode description is plausible, the paper would benefit from a clearer statement that the boundary condition at r = RC (a prescribed dipole) implicitly assumes the source region is decoupled from the plasma; the validity of this separation, and the possible role of finite-conductivity diffusion in a partially ionized ionosphere, are not discussed. This is not fatal, but it is a gap in the physical justification of the model setup.
minor comments (4)
  1. [General] There are several typographical errors: in Appendix A3 'we archive a resolution' should be 'we achieve a resolution'; in Section 4.2 'spacial' should be 'spatial'; in Section 4.3 'moon-magnetosphere cause' is missing the word 'interactions'; in Section 5, panel a of Figure 9 contains 'b= 18 %' which should probably be '≈ 18%'; and in Equation (12) 'were νion' should be 'where νion'.
  2. [Section 4.3] The sentence 'At an induction period of Tprim = 10.18 h, a phase shift of ϕph = 1◦ corresponds to a time span of about 102 s' is correct, but the subsequent statement that Figure 4 indicates phase shifts exceeding 10 degrees is not a logical consequence, as discussed in Major Comment 2. Clarifying the distinction between transient timescales and steady-state phase would avoid confusion.
  3. [Section 5] The definition of the 'low-density' and 'high-density' models is implicit in the figure captions and text; specifying the actual values of ρ0 used (and that 'factor of 10' refers to density) in the main text or table would make the experiments repeatable.
  4. [Appendix A2] The notation 'νion,ph ≈ 3.0·10−8 s−1' and the later use of 'νion = 1/25·νion,ph' in the symmetric model are clear, but the value νion = 1.2·10−9 s−1 in Table 1 is 1/25 of the photoionization rate only if the latter is exactly 3.0e-8; the table should state this explicitly to avoid round-off confusion.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the amplitude ratios and phase delays are forward-model outputs of a prescribed dipole propagating through a modeled plasma; flyby 'consistency' is a weak validation, not a fitted prediction.

full rationale

The paper's central claims are produced by a forward MHD model, not by fitting the target quantities. The induced field is prescribed as a dipole at the inner boundary (Eq. 1 and Section 3), and the transport-modified field is obtained by subtracting a reference simulation from a full simulation (Eq. 14). The reported under/overestimation ratios (0.74 upstream, 1.39 downstream) are ratios of forward-model outputs to the vacuum dipole expression (Eq. 16 and Figure 7); they are quantitative consequences of the MHD propagation, not fitted parameters renamed as predictions. The propagation-phase estimates are likewise forward integrals of the inverse fast-mode speed (Eq. 17) through the modeled plasma environment. The mode-propagation argument that the ordinary electromagnetic mode cannot carry 10-hour signals at Callisto rests on externally measured plasma frequencies (Kivelson et al. 2004; Ansher et al. 2017), not on a self-citation chain. Citations to Duling et al. (2014) and Hartkorn and Saur (2017) provide technical boundary conditions and contextual ionosphere-induction arguments, but these are not the load-bearing evidence for the transport effect itself. The empirical reduction of upstream density in the C03/C09 case study (Section 5) and the polynomial background-field fits do mean that the claimed 'consistency with observations' is not an independent confirmation; however, the transport asymmetries and phase corrections are not derived from those fitted values. The Appendix A2 statement that a realistic ionization rate would move the effective source to the top of the ionosphere and probably reduce the corrections is an explicit robustness limitation, not a circular step: it identifies sensitivity of the quantitative magnitude to the source-location assumption, but does not make the output equal to the input by construction. Therefore no specific circular reduction can be exhibited, and the appropriate score is 0.

Assumptions & free parameters 5 free parameters · 4 assumptions · 0 invented entities

The central quantitative results depend on several parameters that are either poorly constrained, chosen for numerical convenience, or fitted to the target data. No new physical entities are introduced. The most important free choices are the atmospheric scale height, the reduced ionization frequency, and the empirical density reduction factor in the flyby models.

free parameters (5)
  • Atmospheric scale height H = 230 km (symmetric model), 60 km (flyby models)
    Chosen for numerical feasibility rather than from measurement; realistic near-surface scale height is ~30 km. Affects plasma density profile and hence MHD wave velocities and transport times.
  • Ionization frequency νion = 1.2e-9 s^-1 (symmetric model); 3.0e-9 and 3.0e-8 s^-1 (flyby shadow/sunlit)
    In the symmetric model the ionization rate is artificially reduced to 1/25 of the photoionization value to prevent a dense ionosphere from suppressing propagation from the surface. This directly controls the mass loading and wave speeds near Callisto.
  • Upstream plasma mass density ρ0 = 0.96 amu cm^-3, with an empirical reduction factor of 10 in low-density flyby models
    The base value is poorly constrained from literature; in the C03 and C09 case studies the density is arbitrarily reduced by a factor of 10 to make simulated fields match the magnetometer data. This is a fit to the target observations.
  • Thermal pressure p0 = 9.6e-2 nPa
    Poorly constrained; chosen to give plasma beta on the order of values listed by Kivelson et al. (2004). Affects sound speed and fast-mode velocity.
  • Prescribed induced dipole amplitude A = 0.25, 0.5, 0.75, 1.0
    The induced magnetic field at the inner boundary is prescribed with an arbitrary amplitude in the symmetric study. The derived correction ratios are shown to scale linearly with A.
assumptions (4)
  • domain assumption Single-fluid ideal MHD equations with ion-neutral collisions, ionization, and recombination (Eqs. 5-8)
    The plasma is treated as a single charged fluid; kinetic and Hall effects are neglected. Justified by small gyroradii but still an approximation.
  • domain assumption Induced field at the inner boundary is a vacuum dipole field of amplitude A, using the boundary conditions of Duling et al. (2014)
    The induction process itself is prescribed, not solved; only its propagation is modeled. The form of the source directly shapes the field being transported.
  • domain assumption The induced field in the plasma is recovered by subtracting the reference simulation from the full simulation (Eq. 14)
    Assumes that moon-magnetosphere interaction and the induced field can be separated by linear subtraction, even though the full simulation includes nonlinear feedbacks.
  • domain assumption Callisto's atmosphere is radially symmetric, hydrostatic, single-species O2 (Eq. 9)
    Day/night and ram/wake asymmetries in the neutral atmosphere are neglected, which could affect the plasma density distribution and hence the propagation.

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Cite this review

Pith. "Pith review of The Spatiotemporal Structure of Induced Magnetic Fields in Callisto's Plasma Environment due to their Propagation with MHD Modes." pith.science (2026). https://pith.science/paper/NWRPTNSU

@misc{pith2026241115938,
  author       = {Pith},
  title        = {Pith review of: The Spatiotemporal Structure of Induced Magnetic Fields in Callisto's Plasma Environment due to their Propagation with MHD Modes},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/NWRPTNSU}},
  note         = {Machine review of arXiv:2411.15938}
}
read the original abstract

We investigate how the spatiotemporal structure of induced magnetic fields outside of Callisto is affected by their propagation with the magnetohydrodynamic (MHD) modes. At moons that are surrounded by dense magnetized plasmas like the Galilean moons, low-frequency induced magnetic fields cannot propagate with the ordinary electromagnetic mode as is implicitly used by standard analytical expressions. Instead, the induced magnetic fields propagate with the MHD modes, which exhibit anisotropic propagation properties and have finite velocities. Using an MHD framework, we model the spatiotemporal effects of the transport on the induced signals and analyze their contribution to Galileo's C03 and C09 flyby observations. We find that the induced magnetic field in Callisto's plasma environment is asymmetric with a pronounced upstream/downstream asymmetry. By neglecting the transport effects, the amplitude of the induced magnetic field is under- or overestimated by up to tens of percent, respectively. Additionally, we find that MHD wave and convection velocities are strongly reduced in Callisto's local plasma environment, resulting in an additional temporal delay between the emergence of the induced field at the surface of Callisto or the top of its ionosphere and the measurements at spacecraft location. The associated phase shift depends on the location of the observer and can reach values of several to tens of degrees of the phase of the primary inducing frequency. Transport effects impact the observed induction signals and are consistent with the C03 and C09 magnetic field measurements.

Figures

Figures reproduced from arXiv: 2411.15938 by the authors.

Figure 1
Figure 1. Model variables of the reference simulation in the xy-plane. The panels show (a) the plasma bulk velocity, (b) the total magnetic field, (c) the plasma mass density and (d) the thermal pressure. For the two vector variables, the white arrows indicate the projection of the direction onto the plane. –9– [PITH_FULL_IMAGE:figures/full_fig_p009_1.png] view at source ↗
Figure 2
Figure 2. Speed of sound cs (left) and Alfv´en velocity va (right) in the xy-plane. In case of the Alfv´en velocity, the white arrows show the projection of the magnetic field’s direction onto the plane. on the downstream side, where reacceleration occurs. Within the Alfv´en wings, the di￾rection of the magnetic field and of the bulk motion are (anti-)parallel. In terms of plasma density, our model predicts that the local env… view at source ↗
Figure 3
Figure 3. Contour plot of the magnitude of the induced magnetic field in the xy-plane. The upper half shows the induced magnetic field in the plasma environment from the MHD simula￾tions (Equation (14)), the lower half shows the induced magnetic field in a vacuum environment (Equation (1)). The thin gray lines indicate the up- and downstream profile, respectively. Our simplified model is symmetric to the y = 0-plane, allowing… view at source ↗
Figures from the paper (7 more)
Figure 4
Figure 4. Figure 4: Components of the total magnetic field at selected profiles color coded as a function of time. These profiles are: (a) y-profile at x = −1.25 RC, z = 0, (b) y-profile at x = 1.25 RC, z = 0, (c) x-profile at y = 1.25 RC, z = 0, and (d) z-profile at x = 0, y = 1.25 RC. T…
Figure 5
Figure 5. Figure 5: Best fit solutions of the superposition model fitted to the full simulation at the upstream profile (panel a, left) and the downstream profile (panel b, right). The amplitude A˜ of the best fit and the amplitude range of models that fit similarly well are given in the …
Figure 6
Figure 6. Figure 6: Distributions of the transport-altered amplitude A˜ based on Equation (16). The main body of the box plots represents the data in the 25-75 percentile range, the ends of the whiskers show the 5 and 95 percentile, respectively. The respective median value is indicated b…
Figure 7
Figure 7. Figure 7: Comparison of true (A) and transport-altered (A˜) amplitudes for both meth￾ods, the RMS minimization (dots) and the median based estimate (stars). The upstream pro￾file/hemisphere is plotted in green, the downstream profile/hemisphere in orange. The respective solid an…
Figure 8
Figure 8. Figure 8: Estimate of the induced magnetic field’s minimal propagation time to reach the spherical shell at r = 1.25 RC. The dashed gray line indicates the anti-Jovian meridian. The left half (0 − 180 degrees) shows the upstream hemisphere, the right half (180 − 360 degrees) sho…
Figure 9
Figure 9. Figure 9: Panels a-d: Measured (black) and simulated magnetic field (blue/orange) for Galileo’s C03 flyby. Panel e: Estimated wave propagation time of the induced magnetic field and the associated phase shift. –20– [PITH_FULL_IMAGE:figures/full_fig_p020_9.png]
Figure 10
Figure 10. Figure 10: Panels a-d: Measured (black) and simulated magnetic field (blue/orange) for Galileo’s C09 flyby. Panel e: Estimated wave propagation time of the induced magnetic field and the associated phase shift. –22– [PITH_FULL_IMAGE:figures/full_fig_p022_10.png]

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Works this paper leans on

55 extracted references · 27 canonical work pages

  1. [1]

    , Barnhardt, B L

    Ansher2017 APACrefauthors Ansher, J A. , Barnhardt, B L. , Richards, B H. , Gurnett, D A. \ Kurth, W S. APACrefauthors \ 2017 . GALILEO JUPITER PWS DERIVED PLASMA DENSITY FULL RES V1.0 , GO-J-PWS-5-DDR-PLASMA-DENSITY-FULL-V1.0 [ D ataset]. GALILEO JUPITER PWS DERIVED PLASMA DENSITY FULL RES V1.0 , GO-J-PWS-5-DDR-PLASMA-DENSITY-FULL-V1.0 [ D ataset]. NASA ...

    work page doi:10.17189/1519684 2017

  2. [2]

    \ Delamere, P A

    Bagenal2011 APACrefauthors Bagenal, F. \ Delamere, P A. APACrefauthors \ 2011 . Flow of Mass and Energy in the Magnetospheres of J upiter and S aturn Flow of mass and energy in the magnetospheres of J upiter and S aturn . Journal of Geophysical Research: Space Physics 116 A5 . APACrefDOI doi:10.1029/2010JA016294 APACrefDOI

    doi:10.1029/2010ja016294 2011

  3. [3]

    \ Dols, V

    Bagenal2020 APACrefauthors Bagenal, F. \ Dols, V. APACrefauthors \ 2020 . The Space Environment of I o and E uropa The space environment of I o and E uropa . Journal of Geophysical Research: Space Physics 125 5 . APACrefDOI doi:10.1029/2019ja027485 APACrefDOI

    doi:10.1029/2019ja027485 2020

  4. [4]

    , Wilson, R J

    Bagenal2016 APACrefauthors Bagenal, F. , Wilson, R J. , Siler, S. , Paterson, W R. \ Kurth, W S. APACrefauthors \ 2016 . Survey of G alileo Plasma Observations in J upiter s Plasma Sheet Survey of G alileo plasma observations in J upiter s plasma sheet . Journal of Geophysical Research: Planets 121 5 871--894 . APACrefDOI doi:10.1002/2016je005009 APACrefDOI

    doi:10.1002/2016je005009 2016

  5. [5]

    , Johnson, R E

    Mogan2023 APACrefauthors Carberry Mogan, S R. , Johnson, R E. , Vorburger, A. \ Roth, L. APACrefauthors \ 2023 . Electron Impact Ionization in the Icy G alilean Satellites' Atmospheres Electron impact ionization in the icy G alilean satellites' atmospheres . The European Physical Journal D 77 2 . APACrefDOI doi:10.1140/epjd/s10053-023-00606-8 APACrefDOI

    doi:10.1140/epjd/s10053-023-00606-8 2023

  6. [6]

    , Tucker, O

    Mogan2021 APACrefauthors Carberry Mogan, S R. , Tucker, O. , Johnson, R. , Vorburger, A. , Galli, A. , Marchand, B. Sreenivasan, K. APACrefauthors \ 2021 . A Tenuous, Collisional Atmosphere on C allisto A tenuous, collisional atmosphere on C allisto . Icarus 368 114597 . APACrefDOI doi:10.1016/j.icarus.2021.114597 APACrefDOI

    arXiv 2021

  7. [7]

    APACrefauthors \ 1999

    Carlson1999 APACrefauthors Carlson, R W. APACrefauthors \ 1999 . A Tenuous Carbon Dioxide Atmosphere on J upiter's Moon C allisto A tenuous carbon dioxide atmosphere on J upiter's moon C allisto . Science 283 5403 820--821 . APACrefDOI doi:10.1126/science.283.5403.820 APACrefDOI

    doi:10.1126/science.283.5403.820 1999

  8. [8]

    \ Saur, J

    Cervantes_2022 APACrefauthors Cervantes, S. \ Saur, J. APACrefauthors \ 2022 . Constraining E uropa s Subsolar Atmosphere with a Joint Analysis of HST Spectral Images and G alileo Magnetic Field Data Constraining E uropa s subsolar atmosphere with a joint analysis of HST spectral images and G alileo magnetic field data . Journal of Geophysical Research: S...

    work page doi:10.1029/2022ja030472 2022

Show all 55 references
  1. [9]

    , Spencer, J R

    Cunningham2015 APACrefauthors Cunningham, N J. , Spencer, J R. , Feldman, P D. , Strobel, D F. , France, K. \ Osterman, S N. APACrefauthors \ 2015 . Detection of C allisto's Oxygen Atmosphere with the H ubble Space Telescope Detection of C allisto's oxygen atmosphere with the ...

    2015 doi

  2. [10]

    , Milby, Z

    Kleer2023 APACrefauthors de Kleer, K. , Milby, Z. , Schmidt, C. , Camarca, M. \ Brown, M E. APACrefauthors \ 2023 . The Optical Aurorae of E uropa, G anymede, and C allisto The optical aurorae of E uropa, G anymede, and C allisto . The Planetary Science Journal 4 2 37 . APACre...

    2023 doi

  3. [11]

    , Saur, J

    Duling2022 APACrefauthors Duling, S. , Saur, J. , Clark, G. , Allegrini, F. , Greathouse, T. , Gladstone, R. Sulaiman, A H. APACrefauthors \ 2022 . G anymede MHD Model: Magnetospheric Context for J uno’s PJ34 Flyby G anymede MHD model: Magnetospheric context for J uno’s PJ34 f...

    2022 doi

  4. [12]

    , Saur, J

    Duling2014 APACrefauthors Duling, S. , Saur, J. \ Wicht, J. APACrefauthors \ 2014 . Consistent Boundary Conditions at Nonconducting Surfaces of Planetary Bodies: Applications in a New G anymede MHD Model Consistent boundary conditions at nonconducting surfaces of planetary bod...

    2014 doi

  5. [13]

    APACrefauthors \ 2024

    Grayver2024 APACrefauthors Grayver, A. APACrefauthors \ 2024 . Unravelling the Electrical Conductivity of E arth and Planets Unravelling the electrical conductivity of E arth and planets . Surveys in Geophysics 45 1 187--238 . APACrefDOI doi:10.1007/s10712-023-09813-9 APACrefDOI

    2024 doi

  6. [14]

    , Kurth, W S

    Gurnett1997 APACrefauthors Gurnett, D A. , Kurth, W S. , Roux, A. \ Bolton, S J. APACrefauthors \ 1997 . Absence of a Magnetic-field Signature in Plasma-wave Observations at C allisto Absence of a magnetic-field signature in plasma-wave observations at C allisto . Nature 387 6...

    1997 doi

  7. [15]

    , Persoon, A M

    Gurnett2000 APACrefauthors Gurnett, D A. , Persoon, A M. , Kurth, W S. , Roux, A. \ Bolton, S J. APACrefauthors \ 2000 . Plasma Densities in the Vicinity of C allisto from G alileo Plasma Wave Observations Plasma densities in the vicinity of C allisto from G alileo plasma wave...

    2000 doi

  8. [16]

    \ Saur, J

    Hartkorn2017b APACrefauthors Hartkorn, O. \ Saur, J. APACrefauthors \ 2017 . Induction Signals from C allisto s Ionosphere and Their Implications on a Possible Subsurface Ocean Induction signals from C allisto s ionosphere and their implications on a possible subsurface ocean ...

    2017 doi

  9. [17]

    , Saur, J

    Hartkorn2017a APACrefauthors Hartkorn, O. , Saur, J. \ Strobel, D F. APACrefauthors \ 2017 . Structure and Density of C allisto's Atmosphere from a Fluid-kinetic Model of Its Ionosphere: Comparison with H ubble Space Telescope and G alileo Observations Structure and density of...

    2017 doi

  10. [18]

    \ Mukherjee, J

    Huebner2015 APACrefauthors Huebner, W. \ Mukherjee, J. APACrefauthors \ 2015 . Photoionization and Photodissociation Rates in Solar and Blackbody Radiation Fields Photoionization and photodissociation rates in solar and blackbody radiation fields . Planetary and Space Science ...

    2015 doi

  11. [19]

    , Kivelson, M G

    Khurana1998 APACrefauthors Khurana, K K. , Kivelson, M G. , Stevenson, D J. , Schubert, G. , Russell, C T. , Walker, R J. \ Polanskey, C. APACrefauthors \ 1998 . Induced Magnetic Fields As Evidence for Subsurface Oceans in E uropa and C allisto Induced magnetic fields as evide...

    1998 doi

  12. [20]

    , Ebert, R W

    Kim2020 APACrefauthors Kim, T K. , Ebert, R W. , Valek, P W. , Allegrini, F. , McComas, D J. , Bagenal, F. Bolton, S J. APACrefauthors \ 2020 . Survey of Ion Properties in J upiter s Plasma Sheet: J uno JADE -I Observations Survey of ion properties in J upiter s plasma sheet: ...

    2020 doi

  13. [21]

    APACrefauthors \ 2004 01

    Kivelson2004a APACrefauthors Kivelson, M G. APACrefauthors \ 2004 01 . Moon–Magnetosphere Interactions: A Tutorial Moon–magnetosphere interactions: A tutorial . Advances in Space Research 33 11 2061--2077 . APACrefDOI doi:10.1016/j.asr.2003.08.042 APACrefDOI

    2004 doi

  14. [22]

    , Bagenal, F

    Kivelson2004 APACrefauthors Kivelson, M G. , Bagenal, F. , Kurth, W S. , Neubauer, F M. , Paranicas, C. \ Saur, J. APACrefauthors \ 2004 . Magnetospheric Interactions with Satellites Magnetospheric interactions with satellites . F. Bagenal, T E. Dowling \ W B. McKinnon\ ( ), (...

    2004

  15. [23]

    , Khurana, K K

    Kivelson2000 APACrefauthors Kivelson, M G. , Khurana, K K. , Russell, C T. , Volwerk, M. , Walker, R J. \ Zimmer, C. APACrefauthors \ 2000 . G alileo Magnetometer Measurements: A Stronger Case for a Subsurface Ocean at E uropa G alileo magnetometer measurements: A stronger cas...

  16. [24]

    , Khurana, K K

    Kivelson1997a APACrefauthors Kivelson, M G. , Khurana, K K. , Russell, C T. , Walker, R J. , Joy, S P. \ Mafi, J N. APACrefauthors \ 1997 . GALILEO ORBITER AT JUPITER CALIBRATED MAG HIGH RES V1.0 , GO-J-MAG-3-RDR-HIGHRES-V1.0 [ D ataset]. GALILEO ORBITER AT JUPITER CALIBRATED ...

    1997 doi

  17. [25]

    , Khurana, K K

    Kivelson1999 APACrefauthors Kivelson, M G. , Khurana, K K. , Stevenson, D J. , Bennett, L. , Joy, S. , Russell, C T. Polanskey, C. APACrefauthors \ 1999 . E uropa and C allisto: Induced or Intrinsic Fields in a Periodically Varying Plasma Environment E uropa and C allisto: Ind...

    1999 doi

  18. [26]

    , Khurana, K K

    Kivelson2002 APACrefauthors Kivelson, M G. , Khurana, K K. \ Volwerk, M. APACrefauthors \ 2002 . The Permanent and Inductive Magnetic Moments of G anymede The permanent and inductive magnetic moments of G anymede . Icarus 157 2 507--522 . APACrefDOI doi:10.1006/icar.2002.6834 ...

    2002

  19. [27]

    , Anabtawi, A

    Kliore2002 APACrefauthors Kliore, A J. , Anabtawi, A. , Herrera, R G. , Asmar, S W. , Nagy, A F. , Hinson, D P. \ Flasar, F M. APACrefauthors \ 2002 . Ionosphere of C allisto from G alileo Radio Occultation Observations Ionosphere of C allisto from G alileo radio occultation o...

    2002 doi

  20. [28]

    , Roussos, E

    Krupp2023 APACrefauthors Krupp, N. , Roussos, E. , Fränz, M. , Kollmann, P. , Paranicas, C. , Clark, G. Galli, A. APACrefauthors \ 2023 . Pitch Angle Distributions of Energetic Particles Near C allisto Pitch angle distributions of energetic particles near C allisto . Journal o...

    2023 doi

  21. [29]

    , Holmström, M

    Lindkvist2015 APACrefauthors Lindkvist, J. , Holmström, M. , Khurana, K K. , Fatemi, S. \ Barabash, S. APACrefauthors \ 2015 . C allisto Plasma Interactions: Hybrid Modeling Including Induction by a Subsurface Ocean C allisto plasma interactions: Hybrid modeling including indu...

    2015 doi

  22. [30]

    , Feyerabend, M

    Liuzzo2015 APACrefauthors Liuzzo, L. , Feyerabend, M. , Simon, S. \ Motschmann, U. APACrefauthors \ 2015 . The Impact of C allisto s Atmosphere on Its Plasma Interaction with the J ovian Magnetosphere The impact of C allisto s atmosphere on its plasma interaction with the J ov...

    2015 doi

  23. [31]

    , Simon, S

    Liuzzo2016 APACrefauthors Liuzzo, L. , Simon, S. , Feyerabend, M. \ Motschmann, U. APACrefauthors \ 2016 . Disentangling Plasma Interaction and Induction Signatures at C allisto: The G alileo C10 Flyby Disentangling plasma interaction and induction signatures at C allisto: The...

    2016 doi

  24. [32]

    , Simon, S

    Liuzzo2017 APACrefauthors Liuzzo, L. , Simon, S. , Feyerabend, M. \ Motschmann, U. APACrefauthors \ 2017 . Magnetic Signatures of Plasma Interaction and Induction at C allisto: The G alileo C21 , C22 , C23 , and C30 Flybys Magnetic signatures of plasma interaction and inductio...

    2017 doi

  25. [33]

    \ Saur, J

    Mauk2007 APACrefauthors Mauk, B H. \ Saur, J. APACrefauthors \ 2007 . Equatorial electron beams and auroral structuring at J upiter Equatorial electron beams and auroral structuring at J upiter . Journal of Geophysical Research: Space Physics 112 A10 . APACrefDOI doi:10.1029/2...

    2007 doi

  26. [34]

    , Bodo, G

    Mignone2007 APACrefauthors Mignone, A. , Bodo, G. , Massaglia, S. , Matsakos, T. , Tesileanu, O. , Zanni, C. \ Ferrari, A. APACrefauthors \ 2007 . PLUTO : A Numerical Code for Computational Astrophysics PLUTO : A numerical code for computational astrophysics . The Astrophysica...

    2007 doi

  27. [35]

    APACrefauthors \ 1998 1

    Neubauer1998 APACrefauthors Neubauer, F M. APACrefauthors \ 1998 1 . Oceans inside J upiter s Moons Oceans inside J upiter s moons . Nature 395 6704 749--751 . APACrefDOI doi:10.1038/27335 APACrefDOI

    1998 doi

  28. [36]

    APACrefauthors \ 1998 2

    Neubauer1998a APACrefauthors Neubauer, F M. APACrefauthors \ 1998 2 . The Sub- A lfv \' e nic Interaction of the G alilean Satellites with the J ovian Magnetosphere The sub- A lfv \' e nic interaction of the G alilean satellites with the J ovian magnetosphere . Journal of Geop...

    1998 doi

  29. [37]

    APACrefauthors \ 1999

    Neubauer1999 APACrefauthors Neubauer, F M. APACrefauthors \ 1999 . A lfv \' e n Wings and Electromagnetic Induction in the Interiors: E uropa and C allisto A lfv \' e n wings and electromagnetic induction in the interiors: E uropa and C allisto . Journal of Geophysical Researc...

    1999 doi

  30. [38]

    APACrefauthors \ 1983

    Parkinson1983 APACrefauthors Parkinson, W D. APACrefauthors \ 1983 . Introduction to Geomagnetism Introduction to geomagnetism . Edinburgh Scottish Academic Press

    1983

  31. [39]

    APACrefauthors \ 2021

    Saur2021 APACrefauthors Saur, J. APACrefauthors \ 2021 . Overview of Moon–Magnetosphere Interactions Overview of moon–magnetosphere interactions . R. Maggiolo, N. André, H. Hasegawa \ D T. Welling\ ( ), ( \ 575--593). Hoboken, NJ Wiley . APACrefDOI doi:DOI: 10.1002/97811198156...

    2021 doi

  32. [40]

    , Duling, S

    Saur2015 APACrefauthors Saur, J. , Duling, S. , Roth, L. , Jia, X. , Strobel, D F. , Feldman, P D. Hartkorn, O. APACrefauthors \ 2015 . The Search for a Subsurface Ocean in G anymede with H ubble Space Telescope Observations of Its Auroral Ovals The search for a subsurface oce...

    2015 doi

  33. [41]

    , Grambusch, T

    Saur2013 APACrefauthors Saur, J. , Grambusch, T. , Duling, S. , Neubauer, F M. \ Simon, S. APACrefauthors \ 2013 . Magnetic Energy Fluxes in Sub- A lfv \' e nic Planet Star and Moon Planet Interactions Magnetic energy fluxes in sub- A lfv \' e nic planet star and moon planet i...

    2013 doi

  34. [42]

    , Neubauer, F M

    Saur2010 APACrefauthors Saur, J. , Neubauer, F M. \ Glassmeier, K H. APACrefauthors \ 2010 . Induced Magnetic Fields in Solar System Bodies Induced magnetic fields in solar system bodies . Space science reviews 152 1 391--421 . APACrefDOI doi:10.1007/s11214-009-9581-y APACrefDOI

    2010 doi

  35. [43]

    , Neubauer, F M

    Schilling2007 APACrefauthors Schilling, N. , Neubauer, F M. \ Saur, J. APACrefauthors \ 2007 . Time-varying Interaction of E uropa with the J ovian Magnetosphere: Constraints on the Conductivity of E uropa s Subsurface Ocean Time-varying interaction of E uropa with the J ovian...

    2007 doi

  36. [44]

    APACrefauthors \ 2012

    Seufert2012 APACrefauthors Seufert, M. APACrefauthors \ 2012 . \ C allisto: Induction Signals, Atmosphere and Plasma Interaction C allisto: Induction signals, atmosphere and plasma interaction \ . \ University of Cologne . \ Available online at https://kups.ub.uni-koeln.de/4903/

    2012

  37. [45]

    , Saur, J

    Seufert2011 APACrefauthors Seufert, M. , Saur, J. \ Neubauer, F M. APACrefauthors \ 2011 . Multi-frequency Electromagnetic Sounding of the G alilean Moons Multi-frequency electromagnetic sounding of the G alilean moons . Icarus 214 2 477--494 . APACrefDOI doi:10.1016/j.icarus....

    2011 doi

  38. [46]

    APACrefauthors \ 1966

    Srivastava1966 APACrefauthors Srivastava, S P. APACrefauthors \ 1966 . Theory of the Magnetotelluric Method for a Spherical Conductor Theory of the magnetotelluric method for a spherical conductor . Geophysical Journal International 11 4 373--387 . APACrefDOI doi:10.1111/j.136...

    1966 doi

  39. [47]

    APACrefauthors \ 1992

    Stix1992 APACrefauthors Stix, T H. APACrefauthors \ 1992 . Waves in plasmas Waves in plasmas . New York, NY American Inst. of Physics . Rev. and updated ed. of: The theory of plasma waves. 1962

    1992

  40. [48]

    The Spatiotemporal Structure of Induced Magnetic Fields in C allisto's Plasma Environment due to their Propagation with MHD Modes

    Strack2024 APACrefauthors Strack, D. \ Saur, J. APACrefauthors \ 2024 . Data for "The Spatiotemporal Structure of Induced Magnetic Fields in C allisto's Plasma Environment due to their Propagation with MHD Modes" [ D ataset]. Data for "the spatiotemporal structure of induced m...

    2024 doi

  41. [49]

    , Saur, J

    Strobel2002 APACrefauthors Strobel, D F. , Saur, J. , Feldman, P D. \ McGrath, M A. APACrefauthors \ 2002 . H ubble Space Telescope Space Telescope Imaging Spectrograph Search for an Atmosphere on C allisto: A J ovian Unipolar Inductor H ubble space telescope space telescope i...

    2002 doi

  42. [50]

    , Zhu, X

    Strobel1994 APACrefauthors Strobel, D F. , Zhu, X. \ Summers, M E. APACrefauthors \ 1994 . On the Vertical Thermal Structure of I o’s Atmosphere On the vertical thermal structure of I o’s atmosphere . Icarus 111 1 18--30 . APACrefDOI doi:10.1006/icar.1994.1130 APACrefDOI

    1994

  43. [51]

    , Vance, S D

    Styczinski2022 APACrefauthors Styczinski, M J. , Vance, S D. , Harnett, E M. \ Cochrane, C J. APACrefauthors \ 2022 . A Perturbation Method for Evaluating the Magnetic Field Induced from an Arbitrary, Asymmetric Ocean World Analytically A perturbation method for evaluating the...

    2022

  44. [52]

    , Styczinski, M J

    Vance2021 APACrefauthors Vance, S D. , Styczinski, M J. , Bills, B G. , Cochrane, C J. , Soderlund, K M. , Gómez‐Pérez, N. \ Paty, C. APACrefauthors \ 2021 . Magnetic Induction Responses of J upiter s Ocean Moons Including Effects from Adiabatic Convection Magnetic induction r...

    2021 doi

  45. [53]

    , Pfleger, M

    Vorburger2019 APACrefauthors Vorburger, A. , Pfleger, M. , Lindkvist, J. , Holmström, M. , Lammer, H. , Lichtenegger, H I M. Wurz, P. APACrefauthors \ 2019 . Three-dimensional Modeling of C allisto s Surface Sputtered Exosphere Environment Three-dimensional modeling of C allis...

    2019 doi

  46. [54]

    \ Saur, J

    Winkenstern2023 APACrefauthors Winkenstern, J. \ Saur, J. APACrefauthors \ 2023 . Detectability of Local Water Reservoirs in E uropa’s Surface Layer Under Consideration of Coupled Induction Detectability of local water reservoirs in E uropa’s surface layer under consideration ...

    2023 doi

  47. [55]

    , Khurana, K K

    Zimmer2000 APACrefauthors Zimmer, C. , Khurana, K K. \ Kivelson, M G. APACrefauthors \ 2000 . Subsurface Oceans on E uropa and C allisto: Constraints from G alileo Magnetometer Observations Subsurface oceans on E uropa and C allisto: Constraints from G alileo magnetometer obse...

    2000

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