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Simultaneous Mars-orbit observations reveal Kelvin-Helmholtz instability-driven bulk atmospheric ion escape

T0 review · 4 major / 5 minor · reviewed 2026-08-05 · deepseek-v4-flash

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Pith's one-line read Simultaneous two-point Mars observations identify plasma clouds as nonlinear Kelvin-Helmholtz wave packets and show they carry ion fluxes one to two orders above steady escape channels.

desk verdict A solid, field-relevant MAVEN+Tianwen-1 study that makes the KHI case for Mars plasma clouds about as well as single- and two-point data currently allow, but the headline claims overreach on 'direct evidence' and on the one-event spatial-scale bound. read the letter →

arxiv 2608.03780 v1 pith:PAZQHTWW submitted 2026-08-04 physics.space-ph astro-ph.EPphysics.plasm-ph

Chi Zhang , Chuanfei Dong , Gangkai Poh , Jasper Halekas , Xuanye Ma , Ruhunusiri Suranga , Kathleen G. Hanley , Han-Wen Shen
show 6 more authors
Hongyang Zhou Xinmin Li Liang Wang Jiawei Gao Shannon Curry Christian Mazelle
This is my paper · ORCID
classification physics.space-phastro-ph.EPphysics.plasm-ph
keywords MarsatmosphereionescapeKelvin-HelmholtzinstabilityplasmacloudsMAVENTianwen-1inducedmagnetospheresolarwindinteraction
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 uses simultaneous observations from two Mars orbiters, MAVEN near the planet and Tianwen-1 upstream, to argue that localized plasma clouds of escaping heavy ions near the Martian ion composition boundary are nonlinear wave packets produced by the Kelvin-Helmholtz instability. With real-time upstream magnetic-field context, it shows the clouds can form under steady solar-wind conditions, appear preferentially in the −E hemisphere near the draping center, and carry mean O+ and O2+ fluxes of 5.04×10^7 and 3.62×10^7 cm−2 s−1, one to two orders of magnitude above the steady plume and magnetotail escape channels. If the interpretation holds, Kelvin-Helmholtz instability is a major, possibly continuous bulk escape pathway at Mars and would operate similarly at other unmagnetized planets. The paper also delivers the first two-spacecraft constraint on plasma-cloud size, with some events smaller than about 0.6 Mars radius.

What carries the argument

The Kelvin-Helmholtz instability (KHI) at the interface between fast magnetosheath protons and slower planetary heavy ions near the ion composition boundary, diagnosed in Mars Solar Electric (MSE) coordinates that align with the upstream solar-wind velocity and motional electric field. The paper reads each cloud as a crossing of a tailward-moving KH wave packet: a gradual downstream edge, a sharp compressional upstream edge with bipolar B_ZSE signatures and amplified B_YSE, vortex proton flows, and a central pressure minimum. Supporting machinery includes the linear single-fluid MHD KHI growth rate used to explain the −E-hemisphere preference, the two-spacecraft geometry that constrains clou

What would settle it

Re-examine the quasi-periodic 31 July 2023 event by cross-correlating MAVEN's ~2-minute cloud recurrence against the contemporaneous Tianwen-1 upstream IMF and plasma time series. If a ~2-minute periodicity in the upstream clock angle, field magnitude, or flow speed appears at the matching phase, the cloud recurrence could be a temporal boundary response rather than a spatial KH wave packet, and the paper's central interpretive step would fail; a clean absence of such upstream periodicity would support the spatial wave-packet reading.

Watch

Extended reading notes

Core claim

The paper's central claim is that each plasma-cloud crossing—alternating layers of magnetosheath protons and O+/O2+ heavy ions, with vortex-like proton flows, a central depletion in magnetic field and total pressure, and a sharp compressional upstream edge carrying impulsive bipolar magnetic-field signatures—is the spacecraft's traversal of a nonlinear Kelvin-Helmholtz wave packet growing at the ion composition boundary. Two representative events (one quasi-periodic, one isolated), both with steady upstream IMF measured by Tianwen-1, anchor the interpretation, and a 62-event statistical sample shows the same signatures. All events occur in the −E hemisphere near the draping center, an asymme

Load-bearing premise

The argument assumes that what one spacecraft saw as an alternating sequence of solar-wind protons and heavy ions was a spatial crossing of a coherent, tailward-moving Kelvin-Helmholtz wave packet, not a temporal change in the boundary's position or a solar-wind variation.

Editorial extensions

If this is right

  • If correct, plasma clouds no longer require upstream solar-wind disturbances: KHI can generate them at the boundary under steady solar-wind conditions.
  • KHI would constitute a substantial bulk escape channel, with cloud fluxes averaging 10–100 times the steady plume and magnetotail channels and a simple cylindrical estimate giving a total escape rate near 10^25 s−1, comparable to the tail channel.
  • Escaping ion fluxes would be organized into wave-like, banded, or detached structures concentrated in the −E hemisphere, so global escape inventories must account for IMF and motional-electric-field orientation.
  • Cloud spatial scales can be smaller than 0.6 Mars radius, well below earlier single-spacecraft estimates of 2.5–6 Mars radii; earlier global escape-rate estimates may need revisiting.
  • KHI activity may persist for at least ~8 hours or longer, implying quasi-continuous modulation of planetary ion escape rather than isolated bursts.

Reading between the lines

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

  • Beyond the paper: if these fluxes are representative, KHI-driven clouds could be a leading heavy-ion loss channel at unmagnetized planets; at Venus, with its similar ionopause velocity shear, two-spacecraft or sustained surveys should find analogous clouds preferentially on one E-hemisphere side.
  • Beyond the paper: the exclusive −E-hemisphere occurrence implies that reconstructed atmospheric loss for ancient Mars should be conditioned on upstream magnetic-field and motional-electric-field angles, rather than averaged uniformly over time.
  • Beyond the paper: the single ~0.56 Mars-radius non-detection bound suggests that earlier global KHI escape-rate estimates assuming cloud radii of 2.5–6 Mars radii may substantially overcount transported mass; a dedicated small-separation two-orbit conjunction campaign could measure the actual cloud size distribution.
  • Beyond the paper: because isolated clouds may be detached KH vortices, a targeted search inside them for magnetic-reconnection signatures (electron heating, bidirectional beams, or quadrupolar field perturbations) would test whether vortex detachment completes the transport pathway.
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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 / 5 minor

Summary. The paper uses simultaneous MAVEN and Tianwen-1 observations to interpret plasma clouds at Mars as nonlinear K-H instability (KHI) wave packets. Two representative events (one quasi-periodic, one isolated) are analyzed in MSE coordinates, and a catalog of 16 isolated and 46 quasi-periodic events is assembled. The authors report common signatures: total-pressure minima at cloud centers, sharp compressional upstream edges with bipolar B_z variations, vortex-like proton velocity reversals, and concentration in the −E hemisphere near the draping center. They use the Chandrasekhar single-fluid KHI growth rate (Eq. 1) to argue the −E asymmetry is consistent with stronger velocity shear and weaker magnetic fields there. They further report O+ and O2+ fluxes around 10^7–10^8 cm^−2 s^−1, one to two orders of magnitude above steady plume/tail channels, and use one two-spacecraft non-detection to suggest the spatial scale of clouds can be smaller than 0.56 R_M. A simple cylinder model yields a global escape rate of about 10^25 s^−1, comparable to the tail channel.

Significance. If the interpretation holds, the paper provides a coherent physical explanation for a class of transient escape events at Mars and identifies KHI as a possibly continuous bulk escape channel, with implications for other unmagnetized planets. The use of Tianwen-1 as a real-time upstream monitor is a genuine advance over prior single-spacecraft studies. The paper also ships the event list and analysis code, which aids reproducibility. The KHI interpretation is tested against an external benchmark (the Chandrasekhar growth rate) rather than fitted to the data, and the qualitative agreement of the observed signatures with KHI vortex structure is persuasive. However, the load-bearing spatial-scale constraint rests on a single non-detection, and the spatial-vs-temporal interpretation of the single-spacecraft crossings remains a structural assumption for the bulk of the catalog.

major comments (4)
  1. [Results, Figs. 1–3; catalog description] The central interpretation that the alternating magnetosheath-proton/heavy-ion layers are spatial crossings of tailward-moving KH wave packets is assumed rather than demonstrated: 'the spacecraft intercepted each cloud from the downstream edge, traversed through the cloud core, and exited at the upstream edge.' For the 62-event catalog, the steady-IMF check from Tianwen-1 is shown only for the two representative events and used qualitatively. Temporal boundary motion—ICB flapping, solar-wind dynamic-pressure changes, or internal oscillations—can produce the same single-spacecraft layered signatures. Because the KHI identification, the wavelength estimate, and the subsequent escape-rate calculation all hinge on this spatial assumption, I ask for a quantitative test: for the two representative events, compute the expected crossing speed and boundary-normal motion from MAVEN's own plasma an
  2. [Discussion, fig. S9] The claimed first constraint on KH wave-packet spatial scale rests on a single non-detection: when MAVEN saw an isolated cloud, Tianwen-1 at 0.56 R_M separation did not. This bounds the cloud size only if Tianwen-1 was on the same field lines or at the same boundary crossing that MAVEN sampled. If Tianwen-1 was outside the interaction region (e.g., upstream of the ICB), its non-detection carries no size information. The paper does not establish the magnetic connectivity or boundary-sampling geometry for the fig. S9 interval. Since the statement that cloud scales 'can be much smaller than previous estimates of 2.5–6 R_M' is a headline conclusion, this missing check is load-bearing.
  3. [Discussion, 'Role in ion escape'] The escape-rate estimate of ~10^25 s^−1 is presented as a quantitative result but depends on three unvalidated choices: (i) the cylinder radius of ~0.5 R_M, which is essentially the non-detection bound from fig. S9 and not an independently measured cloud radius; (ii) the use of a representative flux near ~10^8 cm^−2 s^−1, whereas the catalog means are 5.04×10^7 and 3.62×10^7 cm^−2 s^−1 and the peak values are ~10^8; and (iii) the assumption that the estimated flux is a bulk escape flux rather than a localized enhancement. I recommend presenting the escape rate as a range with explicit sensitivity to these parameters, and clearly separating the measured flux from the geometric extrapolation.
  4. [Discussion, Eq. (1) and Fig. 6] The hemispheric asymmetry argument is qualitative. Eq. (1) is a linear, single-fluid, incompressible MHD formula, while the structures are explicitly nonlinear wave packets with substantial heavy-ion gyroradii; the authors acknowledge this limitation. Yet the conclusion that 'KHI has large γ in the −E hemisphere' is based on visual inspection of averaged fields (Fig. 6) rather than a quantitative comparison between the predicted growth-rate asymmetry and the observed occurrence-rate asymmetry. I ask for a concrete computation: evaluate Eq. (1) along the ICB from the averaged MSE profiles, and compare the resulting γ(−E)/γ(+E) ratio with the observed occurrence ratio (all 62 events in −E, none in +E). This would convert a plausible consistency argument into a quantitative test.
minor comments (5)
  1. [Results, Fig. 3 caption] The caption refers to 'density ratio of protons to heavy ions' while the text (and Fig. 3C) describes the heavy-ion density ratio. Please make the definition and normalization explicit.
  2. [Discussion, 'Role in ion escape'] The wavelength estimate uses a duration of ~70 s and phase speed 125 km/s to obtain ~8750 km, but the event recurrence period is stated as ~2 min. Readers may not see why the cloud transit duration, rather than the wave period, is used for the wavelength. Clarify whether 8750 km is the cloud width or the KH wavelength.
  3. [Discussion, 'Origin and nature of isolated plasma clouds'] There is a typo: 'this is corresponds to BMSE_y' should read 'this corresponds to B_MSE^y'.
  4. [Materials and Methods] The phrase 'we use the c6 and d1 data of STATIC' is not self-explanatory to a general reader. Define these data products (e.g., energy/angle ranges) or cite the instrument description with appropriate products.
  5. [Results, 'Representative cases'] In Fig. 1H, the clock-angle difference of ~30° between the magnetosheath and solar wind is cited as 'consistent with characteristic differences' from refs. 42, 43, but no quantitative comparison is given. A brief statement of the expected range and the event's location within it would strengthen the interpretation.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the KHI conclusion is supported by external theoretical growth-rate comparisons and independent observations, not by construction.

full rationale

The paper's central claim—that alternating magnetosheath-proton/heavy-ion layers observed by MAVEN are nonlinear Kelvin-Helmholtz wave packets—is an interpretive identification, not a derivation from fitted parameters. The only quantitative stability calculation is Eq. 1 (Chandrasekhar 1961), applied to independently measured plasma and field distributions to show that the -E hemisphere has a larger KH growth rate; no parameter is adjusted to match the event catalog. The authors' own earlier statistical maps (ref. 34) are used as input for velocity-shear and magnetic-field distributions, but that paper is an independent observational data product, not an output of this study's model, and the comparison is externally falsifiable. The two-point spatial-scale 'constraint' (fig. S9) is a logical inference from one non-detection, with the acknowledged caveat that Tianwen-1's location relative to the boundary matters; whether the inference is fully justified is a data-interpretation question, not circularity. The stated limitations (FLR uncertainty, shear-layer-thickness discrepancy, and the general spatial-vs-temporal degeneracy for the event catalog) are correctness risks, not self-referential reductions. No equation in the paper is defined in terms of the conclusion, no fitted value is relabeled as a prediction, and no load-bearing uniqueness claim is imported from the authors' prior work. Hence no circular step can be quoted.

Assumptions & free parameters 4 free parameters · 6 assumptions · 0 invented entities

The central claim does not depend on fitted constants; it depends on three classes of assumptions: that the single-spacecraft crossing is a spatial sample of a KH wave packet rather than a temporal disturbance, that the nominal boundary model and upstream-context measurements are accurate enough to define MSE coordinates, and that the standard single-fluid KHI growth rate captures the asymmetry despite multispecies and kinetic effects. The escape-rate estimate adds a geometric guess (0.5 R_M cylinder) and a flux-core selection threshold (density ratio >0.5).

free parameters (4)
  • KH wave packet cylinder radius = 0.5 R_M
    Used in the Discussion to convert the observed ~1e8 cm^-2 s^-1 flux into a total escape rate of ~1e25 s^-1. The radius is assumed, not measured.
  • KH phase velocity = 125 km/s
    Assumed to equal the average mass-center velocity of protons and heavy ions for the quasi-periodic event; combined with a 70 s duration to estimate a wavelength of ~8750 km. Phase velocity is not directly measured.
  • heavy ion density ratio threshold = 0.5
    Used to define cloud-core data points when computing mean escape flux; no sensitivity test is reported.
  • clock angle difference threshold = 30 degrees
    Applied when Tianwen-1 was in the magnetosheath to decide which events have reliable MSE coordinates; chosen without sensitivity analysis.
assumptions (6)
  • domain assumption Chandrasekhar single-fluid ideal MHD KHI growth rate (Eq. 1) applies to the proton-heavy-ion interface at Mars
    The paper uses Eq. 1 to explain the -E hemisphere preference while acknowledging that a multifluid or kinetic treatment would be more appropriate and that no simple analytical expression exists for the multispecies case.
  • domain assumption X_MSO = X_MSE, i.e., upstream solar wind flows exactly along -X_MSO
    Stated in Materials and Methods; used to construct MSE coordinates from Tianwen-1 magnetic fields. Solar wind Y and Z flow components are neglected.
  • domain assumption Nominal MPB position from Trotignon et al. (2006) is a valid proxy for the ion composition boundary
    Used throughout to place events and to select ICB crossing intervals; ICB and MPB are related but not identical surfaces.
  • ad hoc to paper Single-spacecraft crossings are spatial traversals of tailward-moving KH wave packets, not temporal boundary motion
    The paper assumes MAVEN intercepts the cloud from the downstream edge, passes through the core, and exits at the upstream edge; if the boundary flaps or the solar wind varies, the signatures could have other causes.
  • domain assumption Tianwen-1 magnetic field measurements represent the upstream context relevant to MAVEN
    When Tianwen-1 is in the magnetosheath, a clock-angle match with MAVEN is required, but the two spacecraft are at different positions and times; mesoscale solar wind structure could decorrelate the measurements.
  • ad hoc to paper Simple geometric cylinder model for the KH wave packet escape-rate estimate
    The total escape rate of ~1e25 s^-1 is derived by treating a nonlinear KH wave packet as a cylinder of radius 0.5 R_M; this geometry is not constrained by the observations.

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Pith. "Pith review of Simultaneous Mars-orbit observations reveal Kelvin-Helmholtz instability-driven bulk atmospheric ion escape." pith.science (2026). https://pith.science/paper/PAZQHTWW

@misc{pith2026260803780,
  author       = {Pith},
  title        = {Pith review of: Simultaneous Mars-orbit observations reveal Kelvin-Helmholtz instability-driven bulk atmospheric ion escape},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/PAZQHTWW}},
  note         = {Machine review of arXiv:2608.03780}
}
read the original abstract

Atmospheric ion escape driven by the solar wind is a key process controlling the long-term loss of the Martian atmosphere. Localized plasma clouds can carry substantial fluxes of planetary ions away from Mars, representing episodes of bulk escape. However, their origin has remained unclear due to the absence of simultaneous upstream measurements. Using joint observations from the MAVEN and Tianwen-1 missions, which provide real-time upstream monitoring, we present direct evidence that these plasma clouds are nonlinear wave packets generated by the Kelvin-Helmholtz instability (KHI). The spatial scale of KH waves is constrained for the first time via two-point measurements. Ion fluxes within plasma clouds are one to two orders of magnitude higher than those in typical steady-state escape channels. Our results indicate that KHI is an important process for solar wind coupling to planetary upper atmospheres and plays a crucial role in shaping atmospheric ion escape for unmagnetized planets.

Figures

Figures reproduced from arXiv: 2608.03780 by the authors.

Figure 1
Figure 1. Overview of a representative quasi-periodic plasma cloud event observed on 31 July 2023. (A) Average spacecraft locations in the XMSO − √ Y2 MSO + Z2 MSO plane. The red star and blue star denote MAVEN and Tianwen-1, respectively. The dashed curves in (A) indicate the nominal bow shock (BS) and magnetic pileup boundary (MPB). (B) Average spacecraft locations in the YZMSO plane; the gray circle represents Mars. (C) H+… view at source ↗
Figure 2
Figure 2. Overview of a representative isolated plasma cloud event observed on 19 October 2022. (A) Average spacecraft locations in the XMSO − √ Y2 MSO + Z2 MSO plane. (B) Average spacecraft locations in the YZMSO plane. (C) H+ energy spectra. (D) O+ energy spectra. (E) O2 + energy spectra. (F) Magnetic fields observed by MAVEN in MSO co￾ordinates. (G) Magnetic fields observed by Tianwen-1. (H) Magnetic field clock angles. Th… view at source ↗
Figure 3
Figure 3. Properties of plasma clouds in the MSE coordinates. (A1 and A2) Magnetic fields. (B1 and B2) Total ion density. (C1 and C2) Density ratio of protons to heavy ions (O+ and O2 +). (D1 and D2) Proton velocities Vx and Vy. (E1 and E2) Proton Vz component (V MSE z ). Red (blue) arrows indicate intervals, where δV MSE z > 0 (δV MSE z < 0), associated with the cloud, where δV MSE z denotes the change in V MSE z . (F1 and F… view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: Simple schematic illustration of the KHI at the interface between magne￾tosheath protons and planetary heavy ions. Protons with higher tailward speeds occupy the lower side, while planetary heavy ions with lower speeds are located on the upper side. Black arrows indica…
Figure 5
Figure 5. Figure 5: D presents histograms of the average escaping flux of O+ and O2 + for these clouds. For each event, we selected data points where the heavy ion density ratio exceeds 0.5 and calculated the mean escaping flux across those points, yielding one representative value per cl…
Figure 6
Figure 6. Figure 6: Average ion velocity and magnetic field distributions near the ICB. (A) The center-of-mass velocity of heavy ions in the XZMSE plane, averaged over −1 RM < YMSE < 1 RM. (B) Proton velocity. (C) Velocity shear between protons and heavy ions. (D) Magnetic field strength.…

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Works this paper leans on

77 extracted references · 77 canonical work pages

  1. [1]

    J. A. hurowitz, J. P . Grotzinger, W. W. Fischer, S. M. Mclennan, R. e. Milliken, n. Stein, A. R. vasavada, d. F. Blake, e. dehouck, J. l. eigenbrode, A. G. Fairén, J. Frydenvang, R. Gellert, J. A. Grant, S. Gupta, K. e. herkenhoff, d. W. Ming, e. B. Rampe, M. e. Schmidt, K. l. Siebach, K. Stack- Morgan, d. Y. Sumner, R. c. Wiens, Redox stratification of ...

    work page 2017

  2. [2]

    B. M. hynek, M. Beach, M. R. t. hoke, Updated global map of Martian valley networks and implications for climate and hydrologic processes. J. Geophys. Res. 115, e09008 (2010)

    work page 2010

  3. [3]

    R. J. lillis, S. Robbins, M. Manga, J. S. halekas, h. v. Frey, time history of the Martian dynamo from crater magnetic field analysis. J. Geophys. Res. Planets 118, 1488–1511 (2013)

    work page 2013

  4. [4]

    Jakosky, d

    B. Jakosky, d. Brain, M. chaffin, S. curry, J. deighan, J. Grebowsky, J. halekas, F. leblanc, R. lillis, J. luhmann, l. Andersson, n. Andre, d. Andrews, d. Baird, d. Baker, J. Bell, M. Benna, d. Bhattacharyya, S. Bougher, c. Bowers, P . chamberlin, J. Y. chaufray, J. clarke, G. collinson, M. combi, J. connerney, K. connour, J. correira, K. crabb, F. crary...

    work page 2018

  5. [5]

    d ong, Y

    c. d ong, Y. lee, Y. Ma, M. lingam, S. Bougher, J. luhmann, S. curry, G. toth, A. nagy, v. tenishev, X. Fang, d. Mitchell, d. Brain, B. Jakosky, Modeling martian atmospheric losses over time: implications for exoplanetary climate evolution and habitability. Astrophys. J. Lett. 859, l14 (2018)

    work page 2018

  6. [6]

    R. J. lillis, d. A. Brain, S. W. Bougher, F. leblanc, J. G. luhmann, B. M. Jakosky, R. Modolo, J. Fox, J. deighan, X. Fang, Y. c. Wang, Y. lee, c. dong, Y. Ma, t. cravens, l. Andersson, S. M. curry, n. Schneider, M. combi, i. Stewart, J. clarke, J. Grebowsky, d. l. Mitchell, R. Yelle, A. F. nagy, d. Baker, R. P . lin, characterizing atmospheric escape fro...

    work page 2015

  7. [7]

    J. l. Fox, A. B. hać, Photochemical escape of oxygen from Mars: A comparison of the exobase approximation to a Monte carlo method. Icarus 204, 527–544 (2009)

    work page 2009

  8. [8]

    t . e. cravens, A. Rahmati, J. l. Fox, R. lillis, S. Bougher, J. luhmann, S. Sakai, J. deighan, Y. lee, M. combi, B. Jakosky, hot oxygen escape from Mars: Simple scaling with solar eUv irradiance. J. Geophys. Res. Space Phys. 122, 1102–1116 (2017)

    work page 2017

Show all 77 references
  1. [9]

    R. J. lillis, J. deighan, J. l. Fox, S. W. Bougher, Y. lee, M. R. combi, t. e. cravens, A. Rahmati, P . R. Mahaffy, M. Benna, M. K. elrod, J. P . McFadden, R. e. ergun, l. Andersson, c. M. Fowler, B. M. Jakosky, e. thiemann, F. eparvier, J. S. halekas, F. leblanc, J. chaufray,...

    2017

  2. [10]

    t . e. cravens, O. hamil, S. houston, S. Bougher, Y. Ma, d. Brain, S. ledvina, estimates of ionospheric transport and ion loss at Mars. J. Geophys. Res. Space Phys. 122, 10626–10637 (2017)

    2017

  3. [11]

    lundin, A

    R. lundin, A. Zakharov, R. Pellinen, h. Borg, B. hultqvist, n. Pissarenko, e. M. dubinin, S. W. Barabash, i. liede, h. Koskinen, First measurements of the ionospheric plasma escape from Mars. Nature 341, 609–612 (1989)

    1989

  4. [12]

    Zhang, Z

    c. Zhang, Z. Rong, X. li, M. Fränz, h. n ilsson, R. Jarvinen, M. Persson, Y. Futaana, c. dong, M. Yamauchi, J. Gao, Y. Zhou, l. Wang, Z. Shi, Y. Wei, F. he, M. holmström, S. Barabash, the energetic oxygen ion beams in the martian magnetotail current sheets: hints from the comp...

    2024

  5. [13]

    Zhang, c

    c. Zhang, c. d ong, h. Zhou, J. halekas, M. Yamauchi, h. nilsson, t. Z. liu, M. Persson, S. curry, Y. dong, Y. Futaana, Y. chen, M. Zhou, R. Suranga, K. G. hanley, c. Mazelle, S. Xu, R. Ramstad, M. holmström, l. J. chen, Anomalous transient enhancement of planetary ion escape ...

    2025

  6. [14]

    d ong, S

    c. d ong, S. W. Bougher, Y. Ma, G. toth, Y. lee, A. F. nagy, v. tenishev, d. J. Pawlowski, M. R. combi, d. najib, Solar wind interaction with the Martian upper atmosphere: crustal field orientation, solar cycle, and seasonal variations. J. Geophys. Res. Space Phys. 120, 7857–7...

    2015

  7. [15]

    d ong, S

    c. d ong, S. W. Bougher, Y. Ma, G. toth, A. F. nagy, d. najib, Solar wind interaction with Mars upper atmosphere: Results from the one- way coupling between the multifluid Mhd model and the MtGcM model. Geophys. Res. Lett. 41, 2708–2715 (2014)

    2014

  8. [16]

    n ilsson, Q

    h. n ilsson, Q. Zhang, G. Stenberg Wieser, M. holmström, S. Barabash, Y. Futaana, A. Fedorov, M. Persson, M. Wieser, Solar cycle variation of ion escape from Mars. Icarus 393, 114610 (2023)

    2023

  9. [17]

    Ramstad, S

    R. Ramstad, S. Barabash, Y. Futaana, h. nilsson, M. holmström, ion escape from mars through time: An extrapolation of atmospheric loss based on 10 years of mars express measurements. J. Geophys. Res. Planets 123, 3051–3060 (2018)

    2018

  10. [18]

    Y. dong, X. Fang, d. A. Brain, J. P . McFadden, J. S. halekas, J. e. connerney, S. M. curry, Y. harada, J. G. luhmann, B. M. Jakosky, Strong plume fluxes at Mars observed by MAven: An important planetary ion escape channel. Geophys. Res. Lett. 42, 8942–8950 (2015)

    2015

  11. [19]

    X. Z. li, Z. J. Rong, M. Fraenz, c. Zhang, l. Klinger, Z. Shi, J. W. Gao, M. W. dunlop, Y. Wei, two types of martian magnetotail current sheets: MAven observations of ion composition. Geophys. Res. Lett. 50, e2022Gl102630 (2023)

    2023

  12. [20]

    dubinin, M

    e . dubinin, M. Fraenz, M. Pätzold, J. McFadden, J. S. halekas, G. A. diBraccio, J. e. P . connerney, F. eparvier, d. Brain, B. M. Jakosky, O. vaisberg, l. Zelenyi, the effect of solar wind variations on the escape of oxygen ions from mars through different channels: MAven obs...

    2017

  13. [21]

    S. inui, K. Seki, S. Sakai, d. Brain, t. hara, J. McFadden, J. halekas, d. Mitchell, G. diBraccio, B. Jakosky, Statistical Study of heavy ion Outflows From Mars Observed in the Martian- induced Magnetotail by MAven. J. Geophys. Res. Space Phys. 124, 5482–5497 (2019)

    2019

  14. [22]

    Brace, R

    l. Brace, R. theis, W. hoegy, Plasma clouds above the ionopause of venus and their implications. Planet. Space Sci. 30, 29–37 (1982)

    1982

  15. [23]

    M. h. Acuña, J. e. P . connerney, P . Wasilewski, R. P . lin, K. A. Anderson, c. W. carlson, J. McFadden, d. W. curtis, d. Mitchell, h. Reme, c. Mazelle, J. A. Sauvaud, c. d’Uston, A. cros, J. l. Medale, S. J. Bauer, P . cloutier, M. Mayhew, d. Winterhalter, n. F. ness, Magnet...

    1998

  16. [24]

    c. t. Russell, J. G. luhmann, R. c. elphic, F. l. Scarf, l. h. Brace, Magnetic field and plasma wave observations in a plasma cloud at venus. Geophys. Res. Lett. 9, 45–48 (1982). Downloaded from https://www.science.org on August 04, 2026 Zhang et al., Sci. Adv. 12, eaed9072 (2...

    1982

  17. [25]

    t . Penz, n. erkaev, h. Biernat, h. lammer, U. Amerstorfer, h. Gunell, e. Kallio, S. Barabash, S. Orsini, A. Milillo, W. Baumjohann, ion loss on Mars caused by the Kelvin–helmholtz instability. Planet. Space Sci. 52, 1157–1167 (2004)

    2004

  18. [26]

    J. S. halekas, d. A. Brain, S. Ruhunusiri, J. P . McFadden, d. l. Mitchell, c. Mazelle, J. e. P . connerney, Y. harada, t. hara, J. R. espley, G. diBraccio, B. M. Jakosky, Plasma clouds and snowplows: Bulk plasma escape from Mars observed by MAven. Geophys. Res. Lett. 43, 1426...

    2016

  19. [27]

    J. S. halekas, S. Ruhunusiri, J. P . McFadden, J. R. espley, G. A. diBraccio, ion composition boundary layer instabilities at Mars. Geophys. Res. Lett. 46, 10303–10312 (2019)

    2019

  20. [28]

    Zhang, Z

    c. Zhang, Z. Rong, h. n ilsson, l. Klinger, S. Xu, Y. Futaana, Y. Wei, J. Zhong, M. Fränz, K. li, h. Zhang, K. Fan, l. Wang, M. holmström, Y. Ge, J. cui, MAven Observations of Periodic low- altitude Plasma clouds at Mars. Astrophys. J. Lett. 922, l33 (2021)

    2021

  21. [29]

    G. Poh, J. R. espley, K. nykyri, c. M. Fowler, X. Ma, S. Xu, G. hanley, n. Romanelli, c. Bowers, J. Gruesbeck, G. A. diBraccio, On the growth and development of non- linear Kelvin– helmholtz instability at Mars: MAven observations. J. Geophys. Res. Space Phys. 126, e2021JA0292...

    2021

  22. [30]

    l. Wang, c. huang, A. d u, Y. Ge, G. chen, Z. Yang, S. li, K. Zhang, Kelvin–helmholtz instability at Mars: in situ observations and kinetic simulations. Astrophys. J. 947, 51 (2023)

    2023

  23. [31]

    X. Wang, X. Xu, Y. Ye, J. Wang, M. Wang, Z. Zhou, Q. chang, Q. Xu, J. Xu, l. luo, P . he, S. cheng, MAven observations of the Kelvin- helmholtz instability developing at the ionopause of Mars. Geophys. Res. Lett. 49, e2022Gl098673 (2022)

    2022

  24. [32]

    Z. Koh, G. Poh, c. M. Fowler, K. G. hanley, X. Ma, J. R. Gruesbeck, d. c. P . Kuruppuaratchi, W. Sun, G. A. diBraccio, J. R. espley, Global occurrence of Kelvin- helmholtz vortices at Mars. Geophys. Res. Lett. 52, e2025Gl117836 (2025)

    2025

  25. [33]

    Zhang, Z

    c. Zhang, Z. Rong, l. Klinger, h. n ilsson, Z. Shi, F. he, J. Gao, X. li, Y. Futaana, R. Ramstad, X. Wang, M. holmström, S. Barabash, K. Fan, Y. Wei, three- dimensional configuration of induced magnetic fields around Mars. J. Geophys. Res. Planets 127, e2022Je007334 (2022)

    2022

  26. [34]

    Zhang, c

    c. Zhang, c. d ong, h. Zhou, J. halekas, X. li, J. Gao, h. Shen, X. Wang, h. nilsson, R. Ramstad, c. Mazelle, l. Wang, S. Xu, A. tadlock, K. G. hanley, S. M. curry, d. l. Mitchell, Global energy transport and conversion in the solar wind- mars interaction: MAven observations. ...

    2025

  27. [35]

    Zhang, c

    c. Zhang, c. d ong, h. Zhou, J. deca, S. Xu, Y. harada, S. M. curry, d. l. Mitchell, Z. liu, J. Qin, c. Mazelle, Observational characteristics of electron distributions in the martian induced magnetotail. Geophys. Res. Lett. 52, e2024Gl113030 (2025)

    2025

  28. [36]

    luhmann, S

    J. luhmann, S. ledvina, c. Russell, induced magnetospheres. Adv. Space Res. 33, 1905–1912 (2004)

    1905

  29. [37]

    M. l. Marquette, R. J. lillis, J. S. halekas, J. G. luhmann, J. R. Gruesbeck, J. R. espley, Autocorrelation study of solar wind plasma and iMF Properties as measured by the MAven Spacecraft. J. Geophys. Res. Space Phys. 123, 2493–2512 (2018)

    2018

  30. [38]

    A. R. Azari, e. Abrahams, F. Sapienza, J. halekas, J. Biersteker, d. l. Mitchell, F. Pérez, M. Marquette, M. J. Rutala, c. F. Bowers, c. M. Jackman, S. M. curry, A virtual solar wind monitor at mars with uncertainty quantification using gaussian processes. J. Geophys. Res. Mac...

    2024

  31. [39]

    W. X. Wan, c. Wang, c. l. li, Y. Wei, china’s first mission to Mars. Nat. Astron. 4, 721–721 (2020)

    2020

  32. [40]

    B. M. Jakosky, R. P . lin, J. M. Grebowsky, J. G. luhmann, d. F. Mitchell, G. Beutelschies, t. Priser, M. Acuna, l. Andersson, d. Baird, d. Baker, R. Bartlett, M. Benna, S. Bougher, d. Brain, d. carson, S. cauffman, P . chamberlin, J. Y. chaufray, O. cheatom, J. clarke, J. con...

    2015

  33. [41]

    trotignon, c

    J. trotignon, c. Mazelle, c. Bertucci, M. Acuña, Martian shock and magnetic pile- up boundary positions and shapes determined from the Phobos 2 and Mars Global Surveyor data sets. Planet. Space Sci. 54, 357–369 (2006)

    2006

  34. [42]

    Y. dong, X. Fang, d. A. Brain, d. M. hurley, J. S. halekas, J. R. espley, R. Ramstad, S. Ruhunusiri, B. M. Jakosky, Magnetic field in the martian magnetosheath and the application as an iMF clock angle proxy. J. Geophys. Res. Space Phys. 124, 4295–4313 (2019)

    2019

  35. [43]

    cheng, c

    Z. cheng, c. Zhang, c. dong, h. Zhou, J. Gao, A. tadlock, X. li, l. Wang, Revisiting Mars’ induced magnetic field and clock angle departures under real- time upstream solar wind conditions. J. Geophys. Res. Space Phys. 130, e2025JA034688 (2025)

    2025

  36. [44]

    Masson, K

    A. Masson, K. nykyri, Kelvin–helmholtz instability: lessons learned and ways forward. Space Sci. Rev. 214, 71 (2018)

    2018

  37. [45]

    J. R. Johnson, S. Wing, P . A. delamere, Kelvin helmholtz instability in Planetary Magnetospheres. Space Sci. Rev. 184, 1–31 (2014)

    2014

  38. [46]

    hasegawa, M

    h. hasegawa, M. Fujimoto, t. d. Phan, h. Rème, A. Balogh, M. W. dunlop, c. hashimoto, R. tandokoro, transport of solar wind into earth’s magnetosphere through rolled- up Kelvin–helmholtz vortices. Nature 430, 755–758 (2004)

    2004

  39. [47]

    A. Otto, d. h. Fairfield, Kelvin- helmholtz instability at the magnetotail boundary: Mhd simulation and comparison with Geotail observations. J. Geophys. Res. 105, 21175–21190 (2000)

    2000

  40. [48]

    d . h. Fairfield, M. M. Kuznetsova, t. Mukai, t. nagai, t. i. Gombosi, A. J. Ridley, Waves on the dusk flank boundary layer during very northward interplanetary magnetic field conditions: Observations and simulation. J. Geophys. Res. 112, A08206 (2007)

    2007

  41. [49]

    Sundberg, S

    t . Sundberg, S. A. Boardsen, J. A. Slavin, l. G. Blomberg, J. A. cumnock, S. c. Solomon, B. J. Anderson, h. Korth, Reconstruction of propagating Kelvin–helmholtz vortices at Mercury’s magnetopause. Planet. Space Sci. 59, 2051–2057 (2011)

  42. [50]

    hasegawa, Structure and dynamics of the magnetopause and its boundary layers

    h. hasegawa, Structure and dynamics of the magnetopause and its boundary layers. Monogr. Environ. Earth Planets 1, 71–119 (2012)

    2012

  43. [51]

    d . A. Brain, J. P . McFadden, J. S. halekas, J. e. P . connerney, S. W. Bougher, S. curry, c. F. dong, Y. dong, F. eparvier, X. Fang, K. Fortier, t. hara, Y. harada, B. M. Jakosky, R. J. lillis, R. livi, J. G. luhmann, Y. Ma, R. Modolo, K. Seki, the spatial distribution of pl...

    2015

  44. [52]

    chandrasekhar, Hydromagnetic and hydrodynamic stability (Oxford Univ

    S. chandrasekhar, Hydromagnetic and hydrodynamic stability (Oxford Univ. Press, 1961)

    1961

  45. [53]

    dubinin, M

    e . dubinin, M. Fraenz, M. Pätzold, J. S. halekas, J. Mcfadden, J. e. P . connerney, B. M. Jakosky, O. vaisberg, l. Zelenyi, Solar wind deflection by mass loading in the Martian magnetosheath based on MAven observations. Geophys. Res. Lett. 45, 2574–2579 (2018)

    2018

  46. [54]

    dubinin, M

    e . dubinin, M. Fraenz, M. Pätzold, S. tellmann, J. McFadden, J. halekas, G. diBraccio, Solar wind—ionosphere interface at Mars. ion dynamics, asymmetry, plasma jets. Geophys. Res. Lett. 51, e2023Gl105073 (2024)

    2024

  47. [55]

    dubinin, R

    e . dubinin, R. Modolo, M. Fraenz, M. Päetzold, J. Woch, l. chai, Y. Wei, J. e. P . connerney, J. Mcfadden, G. diBraccio, J. espley, e. Grigorenko, l. Zelenyi, the induced magnetosphere of Mars: Asymmetrical topology of the magnetic field lines. Geophys. Res. Lett. 46, 12722–1...

    2019

  48. [56]

    M. Yan, J. lei, n. terada, B. Zhang, t. dang, R. Sakata, S. Sakai, Y. Ma, Asymmetrically distributed Kelvin- helmholtz instability at venusian magnetosphere. Geophys. Res. Lett. 53, e2026Gl121691 (2026)

    2026

  49. [57]

    luhmann, c

    J. luhmann, c. Russell, J. Spreiter, S. Stahara, evidence for mass- loading of the venus magnetosheath. Adv. Space Res. 5, 307–311 (1985)

    1985

  50. [58]

    terada, S

    n. terada, S. Machida, h. Shinagawa, Global hybrid simulation of the Kelvin–helmholtz instability at the venus ionopause. J. Geophys. Res. 107, SMP 30–1–SMP 30–20 (2002)

    2002

  51. [59]

    t . dang, J. lei, B. Zhang, t. Zhang, Z. Yao, J. lyon, X. Ma, S. Xiao, M. Yan, O. Brambles, K. Sorathia, v. Merkin, Oxygen ion escape at venus associated with three- dimensional Kelvin- helmholtz instability. Geophys. Res. Lett. 49, e2021Gl096961 (2022)

    2022

  52. [60]

    J. d. huba, the Kelvin- helmholtz instability: Finite larmor radius magnetohydrodynamics. Geophys. Res. Lett. 23, 2907–2910 (1996)

    1996

  53. [61]

    henri, S

    P . henri, S. S. cerri, F. califano, F. Pegoraro, c. Rossi, M. Faganello, O. Šebek, P . M. trávníček, P . hellinger, J. t. Frederiksen, A. nordlund, S. Markidis, R. Keppens, G. lapenta, nonlinear evolution of the magnetized Kelvin- helmholtz instability: From fluid to kinetic ...

    2013

  54. [62]

    Paral, R

    J. Paral, R. Rankin, dawn–dusk asymmetry in the Kelvin–helmholtz instability at Mercury. Nat. Commun. 4, 1645 (2013)

    2013

  55. [63]

    P . A. delamere, R. J. Wilson, A. Masters, Kelvin- helmholtz instability at Saturn’s magnetopause: hybrid simulations. J. Geophys. Res. 116, A10222 (2011)

    2011

  56. [64]

    liljeblad, t

    e . liljeblad, t. Sundberg, t. Karlsson, A. Kullen, Statistical investigation of Kelvin- helmholtz waves at the magnetopause of Mercury. J. Geophys. Res. Space Phys. 119, 9670–9683 (2014)

    2014

  57. [65]

    hasegawa, M

    h. hasegawa, M. Fujimoto, K. takagi, Y. Saito, t. Mukai, h. Rème, Single- spacecraft detection of rolled- up Kelvin- helmholtz vortices at the flank magnetopause. J. Geophys. Res. 111, A09203 (2006)

    2006

  58. [66]

    hasegawa, A

    h. hasegawa, A. Retinò, A. vaivads, Y. Khotyaintsev, M. André, t. K. M. nakamura, W. teh, B. U. Ö. Sonnerup, S. J. Schwartz, Y. Seki, M. Fujimoto, Y. Saito, h. Rème, P . canu, Kelvin- helmholtz waves at the earth’s magnetopause: Multiscale development and associated reconnecti...

    2009

  59. [67]

    t . K. M. nakamura, M. Fujimoto, A. Otto, Structure of an Mhd- scale Kelvin- helmholtz vortex: two- dimensional two- fluid simulations including finite electron inertial effects. J. Geophys. Res. 113, A09204 (2008)

    2008

  60. [68]

    W. li, M. André, Y. v. Khotyaintsev, A. vaivads, d. B. Graham, S. toledo- Redondo, c. norgren, P . henri, c. Wang, B. B. tang, B. lavraud, Y. vernisse, d. l. turner, J. Burch, R. torbert, W. Magnes, c. t. Russell, J. B. Blake, B. Mauk, B. Giles, c. Pollock, J. Fennell, A. Jayn...

    2016

  61. [69]

    X. Ma, P . delamere, A. Otto, B. Burkholder, Plasma transport driven by the three- dimensional Kelvin- helmholtz instability. J. Geophys. Res. Space Phys. 122, 10382–10395 (2017). Downloaded from https://www.science.org on August 04, 2026 Zhang et al., Sci. Adv. 12, eaed9072 (...

    2017

  62. [70]

    Ruhunusiri, J

    S. Ruhunusiri, J. S. halekas, J. P . McFadden, J. e. P . connerney, J. R. espley, Y. harada, R. livi, K. Seki, c. Mazelle, d. Brain, t. hara, G. A. diBraccio, d. e. larson, d. l. Mitchell, B. M. Jakosky, h. hasegawa, MAven observations of partially developed Kelvin- helmholtz ...

    2016

  63. [71]

    najib, A

    d . najib, A. F. nagy, G. tóth, Y. Ma, three- dimensional, multifluid, high spatial resolution Mhd model studies of the solar wind interaction with Mars. J. Geophys. Res. 116, A05204 (2011)

    2011

  64. [72]

    J. P . McFadden, O. Kortmann, d. curtis, G. dalton, G. Johnson, R. Abiad, R. Sterling, K. hatch, P . Berg, c. tiu, d. Gordon, S. heavner, M. Robinson, M. Marckwordt, R. lin, B. Jakosky, MAven suprathermal and thermal ion composition (StAtic) instrument. Space Sci. Rev. 195, 19...

    2015

  65. [73]

    J. e. P . connerney, J. espley, P . lawton, S. Murphy, J. Odom, R. Oliversen, d. Sheppard, the MAven magnetic field investigation. Space Sci. Rev. 195, 257–291 (2015)

    2015

  66. [74]

    G. Wang, S. Xiao, M. Wu, Y. Zhao, S. Jiang, Z. Pan, X. hao, Y. li, K. liu, Y. chi, Z. Zou, M. chen, Z. Su, c. Shen, J. Guo, l. cheng, Z. Wu, M. Xu, Y. Wang, t. Zhang, calibration of the zero offset of the fluxgate magnetometer on board the tianwen- 1 orbiter in the Martian mag...

    2024

  67. [75]

    Y. Wang, t. Zhang, G. Wang, S. Xiao, Z. Zou, l. cheng, Z. Pan, K. liu, X. hao, Y. li, M. chen, Z. Zhang, W. Yan, Z. Su, Z. Wu, c. Shen, Y. chi, M. Xu, J. Guo, Y. du, the Mars orbiter magnetometer of tianwen- 1: in- flight performance and first science results. Earth Planet. Ph...

    2023

  68. [76]

    Z. Zou, Y. Wang, t. Zhang, G. Wang, S. Xiao, Z. Pan, Z. Zhang, W. Yan, Y. du, Y. chi, l. cheng, Z. Wu, X. hao, Y. li, K. liu, M. chen, Z. Su, c. Shen, M. Xu, J. Guo, in- flight calibration of the magnetometer on the Mars orbiter of tianwen- 1. Sci. China Technol. Sci. 66, 2396...

    2023

  69. [77]

    J. W. Gao, Z. J. Rong, l. Klinger, X. Z. li, d. liu, Y. Wei, A spherical harmonic martian crustal magnetic field model combining data sets of MAven and MGS. Earth Space Sci. 8, e2021eA001860 (2021). Acknowledgments: We thank the MAven and tianwen- 1 instrument team for working...

    2021

Pith tools

Reviewed August 5, 2026 · model on record in the stance chip above.