Pith. sign in

REVIEW 2 major objections 4 minor 55 references

Three-Dimensional Modeling of Callisto's Surface Sputtered Exosphere Environment

T0 review · 2 major / 4 minor · reviewed 2026-08-14 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read Callisto's ionosphere switches its exosphere from lopsided to nearly uniform.

desk verdict Useful 3D Callisto sputtered exosphere model with two scenarios, but the headline uniform-versus-ram contrast is partly imposed by the isotropic hot-plasma input and the ~2.5 density factor doesn't match the reported numbers. read the letter →

arxiv 1909.01014 v1 pith:LNGNUHIJ submitted 2019-09-03 astro-ph.EP physics.space-ph

Audrey Vorburger , Martin Pfleger , Jesper Lindkvist , Mats Holmström , Helmut Lammer , Herbert I. M. Lichtenegger , André Galli , Martin Rubin
show 1 more author
Peter Wurz
This is my paper · ORCID
classification astro-ph.EPphysics.space-ph
keywords CallistoexosphereplasmasputteringionospherehybridmodelJUICEneutralmassspectrometryicymoon
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper uses a three-dimensional plasma-interaction and Monte Carlo exosphere model to argue that Callisto's surface sputtering exosphere is controlled by the moon's variable ionosphere. When no ionosphere shields the surface, cold Jovian plasma sputters material mostly from the ram-facing trailing hemisphere, producing an exosphere densest there and about 2.5 times denser overall than the shielded case. When an ionosphere is present, nearly none of the cold plasma reaches the surface, sputtering is driven mainly by energetic ions that arrive almost isotropically, and the exosphere becomes nearly uniform in latitude and longitude. The paper further claims that JUICE's NIM mass spectrometer will detect the main ice sputter products out to thousands of kilometers and the major non-ice species near closest approach, so exospheric composition can be read directly as surface composition. The payoff is testable: the predicted spatial pattern distinguishes the two plasma regimes and gives a way to constrain Callisto's formation conditions from flyby data.

What carries the argument

The load-bearing machinery is a two-stage simulation chain. First, a 3D hybrid plasma-planetary interaction model (ions as particles, electrons as a massless fluid) produces two-dimensional precipitation maps of the cold magnetospheric ions H$^+$, O$^+$, O$^{++}$, and S$^{++}$ onto Callisto's surface; the hot, energetic plasma is instead implemented as uniform arrival over the whole sphere because its gyro-radii are comparable to Callisto's radius. Second, those precipitation maps are multiplied by energy-dependent sputter yields for an oxidizing icy surface and LL/CI chondrite minerals, and the ejected neutrals are followed individually in a collision-free 3D Monte Carlo exosphere model until they escape, ionize, dissociate, or stick to the surface. The two scenarios—full penetration versus 0.07% cold-plasma penetration with all hot plasma—are the controlled comparison that produces the density contrast and geometry change.

What would settle it

A direct test would be a spacecraft flyby that resolves exospheric density at comparable altitudes on the ram and anti-ram sides while an ionosphere is known to be present, for example via radio occultation: the ionosphere scenario predicts nearly equal densities, so a measured ram/anti-ram ratio much larger than unity, or a measured global density more than about 2.5 times the predicted uniform value, would falsify the model's isotropic-hot-plasma and shielding assumptions. Comparing a day/trailing flyby with a night/leading flyby would test the predicted scenario switch.

Watch

Extended reading notes

Core claim

On the model's own terms, the central discovery is that Callisto's ionosphere is the switch that sets the exosphere's geometry and density. In the 'no ionosphere' scenario, the cold magnetospheric H$^+$, O$^+$, O$^{++}$, and S$^{++}$ ions precipitate mainly on the ram side, sputtering a water-dominated exosphere whose ram-hemisphere densities are about 1.5 times the global average and whose anti-ram densities are about half the global average; the global water density is roughly 110 cm$^{-3}$ at the surface, 32 cm$^{-3}$ at 1,000 km, and 1 cm$^{-3}$ at 10,000 km. In the 'ionosphere' scenario, only 0.07% of the cold plasma reaches the surface and it is slowed to energies too low to sputter, while all of the hot plasma arrives almost isotropically; the resulting exosphere is nearly uniform, with densities roughly 2.5 times lower for icy species and 5.5 times lower for non-icy species than in the no-ionosphere case. The paper also establishes that cold and hot plasma contribute about equally to the water density in the no-ionosphere case, and that ionospheric O$_2^+$ charge exchange dominates neutral losses when an ionosphere is present.

Load-bearing premise

The load-bearing premise is that the energetic plasma that sputters when the ionosphere is present arrives at Callisto's surface uniformly from all directions; if the energetic flux is actually anisotropic, the predicted near-uniform exosphere and the factor of 2.5 density contrast would change.

Editorial extensions

If this is right

  • If no ionosphere is present during a Callisto encounter, the sputtered exosphere will be denser by roughly a factor of 2.5 and peaked toward the ram-facing hemisphere; if an ionosphere is present, the density profile will be almost uniform.
  • NIM on JUICE should detect H2O out to about 10,000 km, CO and O2 to a few thousand kilometers, and CO2 near 1,000 km, so the main icy species can be measured on a single flyby.
  • The exospheric ratios of icy species mirror their surface abundances, so measuring them tells the surface composition and can distinguish oxidizing from reducing formation compositions.
  • Non-icy species are much fainter; among minerals only Mg should rise above NIM's background, and only near closest approach, so mineral detection will be marginal.
  • Because the mineral-to-ice density ratio changes by about a factor of two between scenarios, combining ice and mineral abundances can indicate which plasma regime was active.

Reading between the lines

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

  • Beyond the paper: the ram-versus-anti-ram asymmetry can itself serve as an ionosphere detector on a single flyby, since the two scenarios differ geometrically before any density calibration.
  • Beyond the paper: the model's uniform-hot-plasma assumption could be tested by looking for density variations tied to Callisto's position in the Jovian current sheet; if energetic ions arrive anisotropically on short timescales, the 'ionosphere' profile would acquire a measurable directional component.
  • Beyond the paper: the factor of 2.5 is computed for one ionospheric density; because Galileo saw ionospheric densities vary by orders of magnitude between flybys, the real contrast should be treated as a continuum, and repeated flybys could map exospheric density against ionospheric state.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 4 minor

Summary. The paper presents a 3D Monte Carlo model of Callisto's surface-sputtered exosphere, driven by precipitation maps from a hybrid plasma interaction model for the cold Jovian plasma and a uniform flux for the hot energetic plasma. Two scenarios are compared: full plasma penetration ('no ionosphere') and an ionosphere that blocks the cold plasma from sputtering while allowing all hot plasma to reach the surface ('ionosphere'). The authors report that the no-ionosphere exosphere is ram-side asymmetric, whereas the ionosphere exosphere is nearly uniform and about 2.5 times less dense, and they discuss the detectability of the predicted exospheric populations by the JUICE/NIM instrument.

Significance. If the modeling assumptions hold, the paper provides a useful 3D synthesis of plasma precipitation, sputtering, and ballistic transport for Callisto, with concrete predictions for JUICE/NIM. Its strengths include the use of hybrid-model-derived precipitation maps for the cold plasma, the use of laboratory-based sputter yields, a transparent statement of the scenario assumptions, and a data availability statement. The qualitative distinction between a ram-favored exosphere in the unshielded case and a more uniform exosphere in the ionosphere case is physically plausible and testable. However, as discussed below, the uniformity of the ionosphere case is largely inherited from an input assumption, and the reported factor of about 2.5 is not supported by the paper's own density numbers.

major comments (2)
  1. [Sec. 2.3 and Sec. 3.2] The near-uniform density profile in the 'ionosphere' scenario is inherited from the prescribed uniform hot-plasma precipitation rather than emerging from the 3D transport calculation. Section 2.3 states that for the hot, energetic plasma, 'due to the particles' large gyro-radii, [the plasma] is almost isotropic' and that uniform arrival onto the complete spherical surface is implemented; Section 2.4 then makes hot plasma the only sputtering source in the ionosphere scenario. A uniform source necessarily yields a nearly uniform exosphere. The physical justification is not fully convincing: the quoted gyro-radii of 1.3e3–5.2e3 km (Section 2.3) are only comparable to Callisto's radius of 2.41e3 km, and finite-gyroradius shadowing or pitch-angle anisotropy could produce a tens-of-percent ram/anti-ram asymmetry in the energetic precipitation. A sensitivity run with an anisotropic energetic-particle source, or a clearly stated caveat that the uniform result is an input assumption rather than a prediction, is needed to support the abstract's contrast between the two scenarios.
  2. [Sec. 3.1, Sec. 3.2, and Abstract] The claimed factor-of-2.5 density reduction between the 'no ionosphere' and 'ionosphere' scenarios is not supported by the numbers reported in the text. For H2O, Section 3.1 gives global densities of about 110, 32, and 1 cm^-3 at 0, 1,000, and 10,000 km, while Section 3.2 gives about 76, 21, and 0.53 cm^-3; these imply ratios of about 1.45, 1.5, and 1.9. The 'ionosphere' section itself first states the densities are '~2 times lower' and later states they are '≈ 2.5 times lower', and the abstract and conclusions repeat the 2.5 value. Please correct the factor so that the abstract, conclusions, and Section 3.2 are mutually consistent, or report a properly defined global-mean ratio with an explanation of its altitude dependence.
minor comments (4)
  1. [Sec. 2.6] The manuscript does not state how sputter yields are evaluated for the hot plasma population at 10 keV–100 MeV; because the yields are energy-dependent, please specify a representative energy and any extrapolation used beyond the laboratory data.
  2. [Sec. 2.7 and Table 1] The loss rates computed for O2 and Mg are applied to all neutral species, as acknowledged in the text; since the headline density numbers in Section 3 are for H2O, please add an explicit caveat near those densities that the results inherit the O2-based loss rates, and indicate the expected uncertainty.
  3. [Sec. 4] The statement that NIM will detect H2O 'as far out as 10^4 km above the surface' is marginal, because the ionosphere-scenario density at 10^4 km is 0.53 cm^-3, below the ~1 cm^-3 detection limit; please qualify the detectability statement by scenario.
  4. [General] The manuscript contains a number of typographical errors (e.g., 'Figure 3 shows he density profiles' in Section 3) and some inconsistent hyphenation; a careful proofread is recommended.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the exosphere profiles are forward-model outputs, and the cited self-works are laboratory-based inputs rather than fitted targets.

full rationale

The two headline results are generated by separate forward simulations rather than by fitting or by definitional identity. The cold-plasma precipitation maps come from a hybrid plasma interaction model, and the sputtered exosphere densities are computed by Monte Carlo trajectory integration with explicit loss processes. The near-uniform density profile in the 'ionosphere' scenario does inherit the spherical symmetry of the hot-plasma precipitation input, which is stated explicitly in Sec. 2.3 ('we implement uniform plasma arrival onto the complete spherical surface') and in Sec. 2.4 ('we only implement sputtering by hot plasma ions but not by cold plasma ions'). This is an openly declared scenario assumption, not a hidden fit or a parameter renamed as a prediction; the resulting densities, altitude profiles, and loss-rate effects are computed, not imposed. The surface compositions and sputter yields taken from Vorburger et al. (2015) and Vorburger & Wurz (2018) trace to laboratory sputtering experiments and SRIM calculations, not to the exosphere densities being predicted, so these self-citations are not load-bearing in a circular sense. The paper's abstract states a 'factor of ~2.5' density reduction, while the values in Secs. 3.1 and 3.2 imply ratios around 1.45-1.9; that is an internal numerical inconsistency or correctness concern, but it is not circularity. Similarly, the sensitivity of the uniform result to the assumed isotropy of the hot plasma is a physical assumption and an uncertainty, not a circular step.

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

The model combines literature-based inputs (plasma parameters, sputter yields, surface composition) with standard physics; no new entities are introduced. The main assumptions are the isotropic hot plasma precipitation, the stoichiometric release, and the extrapolation of loss rates from O2/Mg to all species.

assumptions (5)
  • domain assumption The sputtered particle energy distribution is given by f(E) in Eq. 1, with surface binding energy Eb and maximum transferred energy Ec.
    Used in Section 2.7 as the basis for the Monte Carlo ejection energies; this is a standard sputtering formula from Sigmund theory.
  • domain assumption Particles returning to the surface are completely sticking.
    Section 2.7: 'Particles that return to the surface are assumed to be completely sticking.' This simplifies the surface interaction and may affect residence times.
  • domain assumption Sputtered species are released stoichiometrically from the surface.
    Section 1 and 4: 'Under the assumption that sputtering releases all species present on the surface stoichiometrically into the exosphere (Plainaki et al., 2018)'. This is needed to link exospheric composition to surface composition.
  • ad hoc to paper Loss rates computed for O2 and Mg apply to all other neutral species.
    Section 2.7: 'Considering the overall uncertainties in cross sections and particle fluxes, we feel confident that the loss rates reported for O2 and Mg in Table 1 are also applicable for other neutral species.' This is an extrapolation without explicit cross sections for H2O, CO, CO2, or Fe.
  • domain assumption The ionosphere allows only 0.07% of the cold plasma to reach the surface and does not affect hot plasma.
    Section 2.4 bases this on Strobel et al. (2002). This defines the 'ionosphere' scenario used for all subsequent density predictions.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Three-Dimensional Modeling of Callisto's Surface Sputtered Exosphere Environment." pith.science (2026). https://pith.science/paper/LNGNUHIJ

@misc{pith2026190901014,
  author       = {Pith},
  title        = {Pith review of: Three-Dimensional Modeling of Callisto's Surface Sputtered Exosphere Environment},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/LNGNUHIJ}},
  note         = {Machine review of arXiv:1909.01014}
}
read the original abstract

We study the release of various elements from Callisto's surface into its exosphere by plasma sputtering. The cold Jovian plasma is simulated with a 3D plasma-planetary interaction hybrid model, which produces 2D surface precipitation maps for magnetospheric H+ , O+ , O++ , and S++ . For the hot Jovian plasma, we assume isotropic precipitation onto the complete spherical surface. Two scenarios are investigated: One where no ionospheric shielding takes place and accordingly full plasma penetration is implemented ('no ionosphere' scenario), and one where an ionosphere lets virtually none of the cold plasma but all of the hot plasma reach Callisto's surface ('ionosphere' scenario). In the 3D exosphere model, neutral particles are sputtered from the surface and followed on their individual trajectories. The 3D density profiles show that whereas in the 'no ionosphere' scenario the ram direction is favored, the 'ionosphere' scenario produces almost uniform density profiles. In addition, the density profiles in the 'ionosphere' scenario are reduced by a factor of ~2.5 with respect to the 'no ionosphere' scenario. We find that the Neutral gas and Ion Mass spectrometer, which is part of the Particle Environment Package on board the JUICE mission, will be able to detect the different sputter populations from Callisto's icy surface and the major sputter populations from Callisto's non-icy surface. The chemical composition of Callisto's exosphere can be directly linked to the chemical composition of its surface, and will offer us information not only on Callisto's formation scenario but also on the building blocks of the Jupiter system.

Figures

Figures reproduced from arXiv: 1909.01014 by the authors.

Figure 1
Figure 1. Magnetospheric ion flow around Callisto in the hybrid model for two geometric planes: XZ for panels a and c, and XY for panels b and d. Shown in color is the total ion number densities (a, b) and the mean ion speed (c, d). The vector field in (c, d) shows the direction of the mean ion velocity. The axes are given in Callisto radii, RC = 2410.3 km. –6– [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Maps of precipitating cold magnetospheric H+, O+, O++, and S++ ions onto Cal￾listo’s surface in units of cm−2 s −1 used in the ‘no ionosphere’ case. The hemisphere facing Jupiter’s co-rotating magnetospheric plasma flow (ram side) lies in the center of the precipita￾tion maps, positive latitudes correspond to Callisto’s northern hemisphere, positive longitudes represent the eastern hemisphere. rC /16, is not infinit… view at source ↗
Figure 3
Figure 3. Number density cuts in units of cm−3 for surface sputtered H2O. The magne￾tospheric ram side is on the right hand side, and -B0 points upwards. The left two panels show the individual sputter contributions by the cold and the hot plasma for a fixed loss rate (0.2 × 10−6 s −1 ). The middle two panels show the density profiles for full plasma penetration for two different loss rates. The right two panels show the comp… view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: Number density cuts in units of cm−3 for H2O, CO2, CO, and O2 sputtered from an oxidizing icy surface, Mg sputtered from a LL-type chondritic non-icy surface, and Fe sput￾tered from a CI chondritic non-icy surface for the ‘no ionosphere’ case. The magnetospheric ram si…
Figure 5
Figure 5. Figure 5: Number density cuts in units of cm−3 for H2O, CO2, CO, and O2 sputtered from an oxidizing icy surface, Mg sputtered from a LL-type chondritic non-icy surface and Fe sput￾tered from a CI chondritic non-icy surface for the ‘ionosphere’ case. The magnetospheric ram side i…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

55 extracted references · 34 canonical work pages

  1. [1]

    , Mordasini, C

    Alibert2005a APACrefauthors Alibert, Y. , Mordasini, C. , Benz, W. \ Winisdoerffer, C. APACrefauthors \ 2005 . Models of giant planet formation with migration and disc evolution Models of giant planet formation with migration and disc evolution . Astron. & Astrophys. 434 343--353

    work page 2005

  2. [2]

    , Mousis, O

    Alibert2005b APACrefauthors Alibert, Y. , Mousis, O. \ Benz, W. APACrefauthors \ 2005 . Modeling the Jovian subnebula: I. Thermodynamic conditions and migration of proto-satellites Modeling the Jovian subnebula: I. Thermodynamic conditions and migration of proto-satellites . Astron. & Astrophys. 439 1205--1213

    work page 2005

  3. [3]

    , Shemansky, D E

    Bagenal1992 APACrefauthors Bagenal, F. , Shemansky, D E. , Jr, R L M. , Schreier, R. \ Eviatar, A. APACrefauthors \ 1992 . The abundance of O ^ ++ in the Jovian magnetosphere The abundance of O ^ ++ in the Jovian magnetosphere . Geophys. Res. Lett. 19 2 79--82

    work page 1992

  4. [4]

    , Sidrow , E

    Bagenal2015 APACrefauthors Bagenal , F. , Sidrow , E. , Wilson , R J. , Cassidy , T A. , Dols , V. , Crary , F J. Paterson , W R. APACrefauthors \ 2015 11 . Plasma conditions at Europa's orbit Plasma conditions at Europa's orbit . Icarus 261 1-13 . APACrefDOI doi:10.1016/j.icarus.2015.07.036 APACrefDOI

    doi:10.1016/j.icarus.2015.07.036 2015

  5. [5]

    , Wurz , P

    Barabash2013 APACrefauthors Barabash , S. , Wurz , P. , Brandt , P. , Wieser , M. , Holmstr \"o m , M. , Futaana , Y. Grodent , D. APACrefauthors \ 2013 . Particle Environment Package (PEP) Particle Environment Package (PEP) . European Planetary Science Congress 2013, held 8-13 September in London, UK 8 709

    work page 2013

  6. [6]

    \ Srivastava , S K

    Boivin1998 APACrefauthors Boivin , R F. \ Srivastava , S K. APACrefauthors \ 1998 . Electron-impact ionization of Mg Electron-impact ionization of Mg . Journal of Physics B Atomic Molecular Physics 31 2381-2394 . APACrefDOI doi:10.1088/0953-4075/31/10/024 APACrefDOI

    work page doi:10.1088/0953-4075/31/10/024 1998

  7. [7]

    \ Clark, R N

    Calvin1991 APACrefauthors Calvin, W M. \ Clark, R N. APACrefauthors \ 1991 . Modeling the Reflectance Spectrum of Callisto 0.25 to 4.1 m Modeling the Reflectance Spectrum of Callisto 0.25 to 4.1 m . Icarus 89 305--317

    work page 1991

  8. [8]

    , Smythe, W

    Carlson1996 APACrefauthors Carlson, R. , Smythe, W. , Baines, K. , Barbinis, E. , Becker, K. , Burns, R. Weissman, P. APACrefauthors \ 1996 . Near-infrared spectroscopy and spectral mapping of Jupiter and the Galilean satellites: Results from Galileo's initial orbit Near-infrared spectroscopy and spectral mapping of Jupiter and the Galilean satellites: Re...

    work page 1996

Show all 55 references
  1. [9]

    APACrefauthors \ 1999

    Carlson1999 APACrefauthors Carlson, R W. APACrefauthors \ 1999 . A Tenuous Carbon Dioxide Atmosphere on Jupiter's Moon Callisto A Tenuous Carbon Dioxide Atmosphere on Jupiter's Moon Callisto . Science 283 820 . APACrefURL www.sciencemag.org APACrefURL APACrefDOI doi:10.1126/sc...

    1999 doi

  2. [10]

    , Johnson, R E

    Cooper2001 APACrefauthors Cooper, J F. , Johnson, R E. , Mauk, B H. , Garrett, H B. \ Gehrels, N. APACrefauthors \ 2001 . Energetic Ion and Electron Irradiation of the Icy Galilean Satellites Energetic Ion and Electron Irradiation of the Icy Galilean Satellites . Icarus 149 13...

    2001

  3. [11]

    , 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 Callisto's oxygen atmosphere with the Hubble Space Telescope Detection of Callisto's oxygen atmosphere with the Hub...

    2015 doi

  4. [12]

    , Becker , K

    Deutsch2000 APACrefauthors Deutsch , H. , Becker , K. , Matt , S. \ M \"a rk , T D. APACrefauthors \ 2000 02 . Theoretical determination of absolute electron-impact ionization cross sections of molecules Theoretical determination of absolute electron-impact ionization cross se...

    2000 doi

  5. [13]

    , Shi, J

    Fama2008 APACrefauthors Fam \'a , M. , Shi, J. \ Baragiola, R A. APACrefauthors \ 2008 . Sputtering of ice by low-energy ions Sputtering of ice by low-energy ions . Surface Science. 602 156--161 . APACrefURL www.sciencedirect.com APACrefURL APACrefDOI doi:10.1016/j.susc.2007.1...

    2008 doi

  6. [14]

    , Wetzel , R C

    Freund1990 APACrefauthors Freund , R S. , Wetzel , R C. , Shul , R J. \ Hayes , T R. APACrefauthors \ 1990 04 . Cross-section measurements for electron-impact ionization of atoms Cross-section measurements for electron-impact ionization of atoms . Physical Review A 41 3575-359...

    1990 doi

  7. [15]

    , Vorburger , A

    Galli2018 APACrefauthors Galli , A. , Vorburger , A. , Wurz , P. , Cerubini , R. \ Tulej , M. APACrefauthors \ 2018 09 . First experimental data of sulphur ions sputtering water ice First experimental data of sulphur ions sputtering water ice . Icarus 312 1-6 . APACrefDOI doi:...

    2018 doi

  8. [16]

    , Vorburger , A

    Galli2017 APACrefauthors Galli , A. , Vorburger , A. , Wurz , P. \ Tulej , M. APACrefauthors \ 2017 07 . Sputtering of water ice films: A re-assessment with singly and doubly charged oxygen and argon ions, molecular oxygen, and electrons Sputtering of water ice films: A re-ass...

    2017 doi

  9. [17]

    , Redmon, L T

    Garrett1985 APACrefauthors Garrett, B C. , Redmon, L T. , McCurdy, C W. \ Redmon, M J. APACrefauthors \ 1985 . Electronic excitation and dissociation of O2 and S2 by electron impact Electronic excitation and dissociation of O2 and S2 by electron impact . Phys. Rev. A 32 6

    1985

  10. [18]

    , Dougherty, M K

    Grasset2013 APACrefauthors Grasset, O. , Dougherty, M K. , Coustenis, A. , Bunce, E J. , Erd, C. , Titov, D. Hoolst, T V. APACrefauthors \ 2013 . JUpiter ICy moons Explorer (JUICE): An ESA mission to orbit Ganymede and to characterise the Jupiter system JUpiter ICy moons Explo...

    2013 doi

  11. [19]

    , Klemaszewski, J E

    Greeley2000 APACrefauthors Greeley, R. , Klemaszewski, J E. , Wagner, R. \ the Galileo Imaging Team. APACrefauthors \ 2000 . Galileo views of the geology of Callisto Galileo views of the geology of Callisto . Planet. Space Sci. 48 829--853 . APACrefURL www.elsevier.nl/locate/p...

    2000

  12. [20]

    , Kurth , W S

    Gurnett1997 APACrefauthors Gurnett , D A. , Kurth , W S. , Roux , A. \ Bolton , S J. APACrefauthors \ 1997 05 . Absence of a magnetic-field signature in plasma-wave observations at Callisto Absence of a magnetic-field signature in plasma-wave observations at Callisto . Nature ...

    1997 doi

  13. [21]

    , Persoon , A M

    Gurnett2000 APACrefauthors Gurnett , D A. , Persoon , A M. , Kurth , W S. , Roux , A. \ Bolton , S J. APACrefauthors \ 2000 07 . Plasma densities in the vicinity of Callisto from Galileo plasma wave observations Plasma densities in the vicinity of Callisto from Galileo plasma ...

    doi

  14. [22]

    , McCord, T B

    Hibbitts2000 APACrefauthors Hibbitts, C A. , McCord, T B. \ Hansen, G B. APACrefauthors \ 2000 . Distributions of CO2 and SO2 on the surface of Callisto Distributions of CO2 and SO2 on the surface of Callisto . J. Geophys. Res 105 E9 . APACrefURL http://dx.doi.org/10.1029/1999...

    2000 doi

  15. [23]

    APACrefauthors \ 2011 10

    Holmstrom2011a APACrefauthors Holmstr \"o m , M. APACrefauthors \ 2011 10 . An Energy Conserving Parallel Hybrid Plasma Solver An Energy Conserving Parallel Hybrid Plasma Solver . N V. Pogorelov , E. Audit \ G P. Zank \ ( ), 5th International Conference of Numerical Modeling o...

    2011

  16. [24]

    APACrefauthors \ 2013 04

    Holmstrom2013 APACrefauthors Holmstr \"o m , M. APACrefauthors \ 2013 04 . Handling Vacuum Regions in a Hybrid Plasma Solver Handling Vacuum Regions in a Hybrid Plasma Solver . N V. Pogorelov , E. Audit \ G P. Zank \ ( ), Numerical Modeling of Space Plasma Flows (ASTRONUM2012)...

    2013

  17. [25]

    \ Barabash , S

    Holmstrom2011b APACrefauthors Holmstr \"o m , M. \ Barabash , S. APACrefauthors \ 2011 10 . Hybrid Simulations of the Callisto-Magnetosphere Interaction Hybrid Simulations of the Callisto-Magnetosphere Interaction . EPSC-DPS Joint Meeting 2011 Epsc-dps joint meeting 2011 \ ( 689)

    2011

  18. [26]

    , Fatemi , S

    Holmstrom2012 APACrefauthors Holmstr \"o m , M. , Fatemi , S. , Futaana , Y. \ Nilsson , H. APACrefauthors \ 2012 02 . The interaction between the Moon and the solar wind The interaction between the Moon and the solar wind . Earth, Planets, and Space 64 237-245 . APACrefDOI do...

    2012 doi

  19. [27]

    , Keady, J J

    Huebner1992 APACrefauthors Huebner, W F. , Keady, J J. \ Lyon, S P. APACrefauthors \ 1992 . Solar photo rates for planetary atmospheres and atmospheric pollutants Solar photo rates for planetary atmospheres and atmospheric pollutants . Astrophys. and Space Sci. 195 1 1--294

    1992

  20. [28]

    , Liu , M

    Johnson2002b APACrefauthors Johnson , R E. , Liu , M. \ Tully , C. APACrefauthors \ 2002 01 . Collisional dissociation cross sections for O+O _ 2 , CO and N _ 2 , O _ 2 +O _ 2 , N+N _ 2 , and N _ 2 +N _ 2 Collisional dissociation cross sections for O+O _ 2 , CO and N _ 2 , O _...

    2002 doi

  21. [29]

    , Trajmar , S

    Kanik1993 APACrefauthors Kanik , I. , Trajmar , S. \ Nickel , J C. APACrefauthors \ 1993 04 . Total electron scattering and electronic state excitations cross sections for O2, CO, and CH4 Total electron scattering and electronic state excitations cross sections for O2, CO, and...

    1993 doi

  22. [30]

    , Bagenal, F

    Kivelson2004 APACrefauthors Kivelson, M G. , Bagenal, F. , Kurth, W S. , Neubauer, F M. , Paranicas, C. \ Saur, J. APACrefauthors \ 2004 . Jupiter: The Planet, Satellites and Magnetosphere Jupiter: The Planet, Satellites and Magnetosphere . ( 1, \ 513--536). Cambridge University Press

    2004

  23. [31]

    , 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 Callisto from Galileo radio occultation observations Ionosphere of Callisto from Galileo radio occultation obser...

    2002 doi

  24. [32]

    \ Kronrod, V A

    Kuskov2005 APACrefauthors Kuskov, O L. \ Kronrod, V A. APACrefauthors \ 2005 . Internal structure of Europa and Callisto Internal structure of Europa and Callisto . Icarus 177 550--569 . APACrefURL www.elsevier.com/locate/icarus APACrefURL APACrefDOI doi:10.1016/j.icarus.2005....

    2005 doi

  25. [33]

    , Holmstr \"o m , M

    Lindkvist2015 APACrefauthors Lindkvist , J. , Holmstr \"o m , M. , Khurana , K K. , Fatemi , S. \ Barabash , S. APACrefauthors \ 2015 06 . Callisto plasma interactions: Hybrid modeling including induction by a subsurface ocean Callisto plasma interactions: Hybrid modeling incl...

    2015 doi

  26. [34]

    , McGrath , C

    Luna2005 APACrefauthors Luna , H. , McGrath , C. , Shah , M B. , Johnson , R E. , Liu , M. , Latimer , C J. \ Montenegro , E C. APACrefauthors \ 2005 08 . Dissociative Charge Exchange and Ionization of O _ 2 by Fast H ^ + and O ^ + Ions: Energetic Ion Interactions in Europa's ...

    2005

  27. [35]

    , Shah, M B

    McCallion1992 APACrefauthors McCallion, P. , Shah, M B. \ Gilbody, H B. APACrefauthors \ 1992 . Multiple ionization of magnesium by electron impact Multiple ionization of magnesium by electron impact . Journal of Physics B: Atomic, Molecular, and Optical Physics 25 1051

    1992

  28. [36]

    , Malone , C P

    McConkey2008 APACrefauthors McConkey , J W. , Malone , C P. , Johnson , P V. , Winstead , C. , McKoy , V. \ Kanik , I. APACrefauthors \ 2008 09 . Electron impact dissociation of oxygen-containing molecules A critical review Electron impact dissociation of oxygen-containing mol...

    2008 doi

  29. [37]

    , Hansen, G B

    McCord1998 APACrefauthors McCord, T B. , Hansen, G B. , Clark, R N. , Martin, P D. , Hibbitts, C A. , Fanale, F P. Danielson, G E. APACrefauthors \ 1998 . Non-water-ice constituents in the surface material of the icy Galilean satellites from the Galileo near-infrared mapping s...

    1998

  30. [38]

    \ Johnson , R E

    McGrath1998 APACrefauthors McGrath , M A. \ Johnson , R E. APACrefauthors \ 1989 03 . Charge exchange cross sections for the Io plasma torus Charge exchange cross sections for the Io plasma torus . J. Geophys. Res 94 2677-2683 . APACrefDOI doi:10.1029/JA094iA03p02677 APACrefDOI

    1989 doi

  31. [39]

    , Belcher , J W

    McNutt1981 APACrefauthors McNutt , R L. , Belcher , J W. \ Bridge , H S. APACrefauthors \ 1981 09 . Positive ion observations in the middle magnetosphere of Jupiter Positive ion observations in the middle magnetosphere of Jupiter . J. Geophys. Res 86 8319-8342 . APACrefDOI doi...

    1981 doi

  32. [40]

    \ Alibert, Y

    Mousis2006 APACrefauthors Mousis, O. \ Alibert, Y. APACrefauthors \ 2006 . Modeling the Jovian subnebula - II. Composition of regular satellite ices Modeling the Jovian subnebula - II. Composition of regular satellite ices . Astron. & Astrophys. 448 L7 771--778 . APACrefDOI do...

    2006 doi

  33. [41]

    , Lacerda, P

    Muntean2016 APACrefauthors Muntean, E A. , Lacerda, P. , Field, T A. , Fitzsimmons, A. , Fraser, W C. , Hunniford, A C. \ McCullough, R W. APACrefauthors \ 2016 . A laboratory study of water ice erosion by low-energy ions A laboratory study of water ice erosion by low-energy i...

    2016

  34. [42]

    , Breuer, D

    Nagel2004 APACrefauthors Nagel, K. , Breuer, D. \ Spohn, T. APACrefauthors \ 2004 . A model for the interior structure, evolution, and differentiation of Callisto A model for the interior structure, evolution, and differentiation of Callisto . Icarus 169 402--412 . APACrefURL ...

    2004 doi

  35. [43]

    APACrefauthors \ 1998 09

    Neubauer1998 APACrefauthors Neubauer , F M. APACrefauthors \ 1998 09 . The sub-Alfv \'e nic interaction of the Galilean satellites with the Jovian magnetosphere The sub-Alfv \'e nic interaction of the Galilean satellites with the Jovian magnetosphere . J. Geophys. Res 103 1984...

    1998 doi

  36. [44]

    , Lichtenegger , H I M

    Pfleger2015 APACrefauthors Pfleger , M. , Lichtenegger , H I M. , Wurz , P. , Lammer , H. , Kallio , E. , Alho , M. Mart \' n-Fern \'a ndez , J A. APACrefauthors \ 2015 09 . 3D-modeling of Mercury's solar wind sputtered surface-exosphere environment 3D-modeling of Mercury's so...

    2015 doi

  37. [45]

    , Cassidy , T A

    Plainaki2018 APACrefauthors Plainaki , C. , Cassidy , T A. , Shematovich , V I. , Milillo , A. , Wurz , P. , Vorburger , A. Teolis , B. APACrefauthors \ 2018 02 . Towards a Global Unified Model of Europa's Tenuous Atmosphere Towards a Global Unified Model of Europa's Tenuous A...

    2018 doi

  38. [46]

    , Teulet , P

    Riahi2006 APACrefauthors Riahi , R. , Teulet , P. , Ben Lakhdar , Z. \ Gleizes , A. APACrefauthors \ 2006 11 . Cross-section and rate coefficient calculation for electron impact excitation, ionisation and dissociation of H _ 2 and OH molecules Cross-section and rate coefficien...

    2006 doi

  39. [47]

    , Neubauer , F M

    Saur1999 APACrefauthors Saur , J. , Neubauer , F M. , Strobel , D F. \ Summers , M E. APACrefauthors \ 1999 11 . Three-dimensional plasma simulation of Io's interaction with the Io plasma torus: Asymmetric plasma flow Three-dimensional plasma simulation of Io's interaction wit...

    1999 doi

  40. [48]

    , Baragiola, R A

    Shi1995 APACrefauthors Shi, M. , Baragiola, R A. , Grosjean, D E. , Johnson, R E. , Jurac, S. \ Schou, J. APACrefauthors \ 1995 . Sputtering of Water Ice Surfaces and the Production of Extended Neutral Atmospheres Sputtering of Water Ice Surfaces and the Production of Extended...

    1995

  41. [49]

    , Renault , P

    Straub1996 APACrefauthors Straub , H C. , Renault , P. , Lindsay , B G. , Smith , K A. \ Stebbings , R F. APACrefauthors \ 1996 09 . Absolute partial cross sections for electron-impact ionization of H _ 2 , N _ 2 , and O _ 2 from threshold to 1000 eV Absolute partial cross sec...

    1996 doi

  42. [50]

    , Saur, J

    Strobel2002 APACrefauthors Strobel, D F. , Saur, J. , Feldman, P D. \ McGrath, M A. APACrefauthors \ 2002 . Hubble Space Telescope Space Telescope Imaging Spectograph Search for an Atmosphere on Callisto: A Jovian Unipolar Inductor Hubble Space Telescope Space Telescope Imagin...

    2002

  43. [51]

    , Itikawa , Y

    Tawara1990 APACrefauthors Tawara , H. , Itikawa , Y. , Nishimura , H. \ Yoshino , M. APACrefauthors \ 1990 05 . Cross Sections and Related Data for Electron Collisions with Hydrogen Molecules and Molecular Ions Cross Sections and Related Data for Electron Collisions with Hydro...

    1990 doi

  44. [52]

    APACrefauthors \ 2019 Feb

    Vorburger2019 APACrefauthors Vorburger, A. APACrefauthors \ 2019 Feb . Callisto 3D Exosphere . Callisto 3D Exosphere . osf.io/kuzdf . OSF

    2019

  45. [53]

    \ Wurz , P

    Vorburger2018 APACrefauthors Vorburger , A. \ Wurz , P. APACrefauthors \ 2018 09 . Europa's ice-related atmosphere: The sputter contribution Europa's ice-related atmosphere: The sputter contribution . Icarus 311 135-145 . APACrefDOI doi:10.1016/j.icarus.2018.03.022 APACrefDOI

    2018 doi

  46. [54]

    , Wurz , P

    Vorburger2015 APACrefauthors Vorburger , A. , Wurz , P. , Lammer , H. , Barabash , S. \ Mousis , O. APACrefauthors \ 2015 12 . Monte-Carlo simulation of Callisto's exosphere Monte-Carlo simulation of Callisto's exosphere . Icarus 262 14-29 . APACrefDOI doi:10.1016/j.icarus.201...

    2015 doi

  47. [55]

    APACrefauthors \ 2004

    Ziegler2004 APACrefauthors Ziegler, J. APACrefauthors \ 2004 . SRIM-2003 SRIM-2003 . Nucl. Instrum. Methods B Nucl. instrum. methods b \ ( \ 1027--1036)

    2004

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.