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Experiments and modeling of dust particle heating resulting from changes in polarity switching in the PK-4 microgravity laboratory

T0 review · 4 major / 5 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read Polarity switching heats microgravity dust clouds by triggering a Coulomb-like expansion, and the added energy takes far longer to dissipate than gas drag predicts.

desk verdict A solid experimental report of a new microgravity dust-heating signature at polarity switching, with a plausible but under-constrained mechanism because the MD screening lengths are fitted to the data. read the letter →

arxiv 2501.12248 v3 pith:ZR3Q2ZKW submitted 2025-01-21 physics.plasm-ph

Lori S. McCabe , Jeremiah Williams , Saikat Chakraborty Thakur , Uwe Konopka , Evdokiya Kostadinova , Mikhail Pustylnik , Hubertus Thomas , Markus Thoma
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Edward Thomas
This is my paper · ORCID
classification physics.plasm-ph PACS 52.27.Lw
keywords complex(dusty)plasmamicrogravitypolarityswitchingdustkinetictemperatureeffectivescreeninglengthCoulombexpansionconfigurationalenergyPK-4experiment
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 reports that dust particles in the microgravity PK-4 experiment on the ISS heat up when the electric field is switched in polarity to capture them, and that the heated cloud expands slightly at the same time. The equivalent ground-based experiment shows only a brief temperature blip and no expansion, so the effect is tied to the three-dimensional, unconfined conditions of microgravity. The authors propose that for a few milliseconds the plasma loses some of its ability to shield the dust grains, the dust-dust interaction becomes more Coulomb-like, and the cloud undergoes a Coulomb-like expansion that turns stored configurational energy into thermal energy. The paper matters because it shows a fast plasma change can visibly convert a dust cloud's arrangement energy into heat, and because the measured cooling time is far longer than ordinary gas drag would allow, implying that the screening recovers slowly.

What carries the argument

The central object is the effective screening length of the dust-dust interaction, which appears in the Yukawa (Debye-screened Coulomb) potential $U(r) = \frac{Q}{4\pi\varepsilon_0 r} e^{-r/\lambda_D}$ used to model the charged grains. The argument works by changing this screening length: at the onset of polarity switching the plasma is assumed to collapse, so the screening length briefly becomes large and the interaction approaches Coulomb-like; this drives a Coulomb explosion of the cloud, converting configurational potential energy into kinetic energy. In the molecular dynamics code YOAKμM, the transient is implemented by imposing a 2.5 ms interval of large screening length (empirically chosen) followed by successively smaller screening lengths (3, 2, 1.5, 1 mm) that set the extended cooling rate seen in the data.

What would settle it

Run a fast-sampling Langmuir probe or laser-induced fluorescence measurement in the PK-4 chamber during the first 10 ms after polarity switching: if the electron density never drops below its steady ~2×$10^{8}$ $cm^{-3}$ value, the plasma collapse that triggers the proposed Coulomb-like expansion is absent and the heating must have another cause.

Watch

Extended reading notes

Core claim

In the PK-4 microgravity experiment, applying 500 Hz polarity switching to capture a flowing dust cloud produces a sharp rise in the effective dust kinetic temperature in the axial direction within 1–2 video frames (≈0.03 s), an increase in interparticle spacing of about one pixel over 0.5 s, and a long temperature decay that lasts much longer than the Epstein drag damping time (~0.011 s). Ground-based PK-4 runs under identical operating conditions show only a momentary temperature rise and no cloud expansion. Based on these observations and on YOAKμM molecular dynamics simulations, the paper argues that at the moment of switching the plasma briefly collapses and the effective screening length grows (modeled as a 2.5 ms interval of near-Coulomb interaction), releasing the cloud's configurational potential energy as kinetic energy through a Coulomb-like expansion. The simulation reproduces the measured temperature decay only when the effective screening length starts well above the electron Debye length (≈3 mm, versus $k_{De} = 1.45$ mm) and then relaxes stepwise (2 mm, 1.5 mm, 1 mm) as the plasma recovers.

Load-bearing premise

The explanation assumes that during the first few milliseconds after polarity switching the plasma's shielding briefly collapses, making the dust grains interact almost like bare charges, but this collapse is not measured: the 2.5 ms duration and the subsequent screening lengths are chosen to match the observed temperature decay.

Editorial extensions

If this is right

  • In microgravity, every polarity-switch capture should be expected to deposit thermal energy into the dust cloud, so ISS experimental protocols must allow an extended settling time (≈0.5 s or more) before taking quiescent measurements.
  • The measured cooling curve is a rough clock for plasma recovery: the effective screening length inferred from the simulation starts near 3 mm (about twice the electron Debye length) and drops stepwise toward 1 mm within a second after the switch.
  • Because no expansion or extended heating appears in ground-based experiments, the effect requires the unconfined 3D geometry that only microgravity provides; 2D or confined dusty plasma experiments will not show it.
  • The heating is anisotropic (stronger along the field than transverse), so the released configurational energy is not distributed isotropically; ion-wake orientation likely channels it.
  • Dust kinetic temperature is not a reliable constant during the capture phase of PK-4 experiments; it is actively evolving due to the plasma disturbance, not just in steady state.

Reading between the lines

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

  • The mechanism suggests a general control knob: any fast change in plasma parameters that transiently lengthens the Debye length could release stored configurational energy in a dusty plasma, not just polarity switching; pulsed discharges or abrupt current steps might produce the same heating.
  • The 2.5 ms collapse time and the stepwise screening-length recovery in the simulation are concrete predictions for plasma diagnostics: a fast probe or spectral measurement should see electron density dip immediately after the switch and recover within a few hundred milliseconds.
  • If the heating really comes from configurational energy, the magnitude should scale with the dust cloud's initial coupling parameter; varying particle density or charge in the experiment would provide a quantitative check the paper does not perform.
  • The ground-versus-microgravity difference implies confinement is the switch that turns on the expansion channel; an intermediate experiment with a weak confining potential might show a tunable threshold between the two behaviors.
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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 reports experiments in the PK-4 microgravity laboratory on the ISS and in a ground-based reference module, studying the response of a dust cloud to polarity switching of a dc discharge. Using PIV, the authors measure the evolution of drift velocity and effective kinetic temperature of the dust, and using particle tracking they measure interparticle spacing. They find that in microgravity the dust temperature in the direction parallel to the electric field rises sharply within 1–2 video frames after polarity switching, the dust cloud expands (interparticle spacing increases by about 1 pixel over ~0.5 s), and the temperature decays over timescales much longer than Epstein drag. In ground-based experiments, only a brief temperature rise is seen and no cloud expansion. The paper proposes that at polarity switching a transient plasma collapse weakens screening, causing the dust particles to interact in a more Coulomb-like manner for about 2.5 ms, leading to a Coulomb-like expansion that converts configurational potential energy into kinetic energy; the subsequent recovery of screening produces the extended cooling. Molecular dynamics simulations with the YOAKlM code reproduce the temperature rise and decay by imposing an empirically chosen 2.5 ms Coulomb-like phase and time-dependent screening lengths of 3, 2, 1.5, and 1 mm.

Significance. If the proposed mechanism is correct, the paper identifies a previously unreported energy-conversion channel in microgravity complex plasmas, connecting polarity-switching dynamics to Coulomb-explosion physics, and would be of interest to the dusty-plasma community. The experimental observations are valuable: they come from a unique ISS facility, are compared with a matched ground-based instrument, and are cross-checked by regional PIV analysis, particle tracking, and pair-correlation measurements. The authors are also transparent about the empirically chosen simulation parameters. However, as the stress-test correctly notes, the simulation is a fit rather than an independent prediction: the key screening-length inputs are not measured, so the agreement in Fig. 7 does not by itself validate the plasma-collapse hypothesis. The experimental facts of heating, expansion, and slow decay are plausible but their causal interpretation is underdetermined.

major comments (4)
  1. [IV, Fig. 7] The central mechanistic claim rests on a simulation whose key inputs are fitted. The paper states in Sec. IV that the 2.5 ms plasma suppression is 'empirically chosen to best reproduce the heating event numerically,' and the post-switch screening lengths (3, 2, 1.5, 1 mm) are selected to match the temperature decay. Because these time-varying screening lengths are the only way the proposed mechanism enters the MD model, the agreement in Fig. 7 demonstrates that the model can be tuned to reproduce the data, not that the plasma actually undergoes the prescribed transient. To make the simulation a test of the hypothesis, the authors should add a control simulation with fixed nominal screening (no 2.5 ms Coulomb-like phase) and show that it does not reproduce the heating; they should also seek independent constraints on the plasma transient, for example from the ionization-wave measurements cited in Refs. 12 and 33 or from a time-resolved plasma model.
  2. [III, Fig. 4] The headline ground-versus-microgravity contrast is based on a single selected case, which the authors describe as 'the most pronounced result.' No error bars, confidence intervals, or statistics over the multiple capture datasets are provided for the effective temperature traces. Since the central claim is the existence of a qualitatively different thermal response in microgravity, the paper should report the reproducibility of the heating magnitude and decay time across capture events, and should state how the temperature uncertainty from the Maxwellian fits is quantified.
  3. [III, Fig. 6] The cloud expansion is quantified by an interparticle-spacing increase of about 1 pixel, but no uncertainty or statistical test is reported for this quantity. Given that the claimed expansion is a key piece of experimental evidence for the proposed mechanism, the authors should provide a measurement uncertainty for the pair-correlation peak position and, ideally, a direct measure of cloud size or volume evolution rather than a single-pixel shift.
  4. [IV] The paper does not rule out a simpler alternative explanation for the observations: direct heating of the dust by the rapidly oscillating electric field or by ion drag at the onset of switching, followed by slow thermalization during gradual expansion of the unconfined microgravity cloud. A simulation with the oscillating field but without any change in screening length should be presented as a baseline. If such a simulation fails to produce the observed temperature rise and decay, that would substantially strengthen the proposed Coulomb-explosion mechanism; if it succeeds, the screening-length hypothesis would need to be revised.
minor comments (5)
  1. [V] The summary states that polarity switching 'causes a brief structure collapse in the dust cloud, and the screening length decreases' immediately before describing a 'Coulomb-like explosion.' As written, this is internally inconsistent with the model in Sec. IV, where the explosion is produced by a large screening length (Coulomb-like interactions). Presumably 'the screening by the plasma decreases' is intended; please reword.
  2. [IV, Eq. (2)] The Langevin thermal heater is said to be set at room temperature, but the actual temperature value is not given. Please state the assumed neutral temperature and report the sensitivity of the baseline dust temperature to this choice.
  3. [IV] The drag coefficient is 'adjusted in the code to match the magnitude of the particle drift velocity measured during the experimental injection process.' Please give the adjusted value or its ratio to the Epstein value (f_Epstein = 88.3 s^-1), so that the reader can judge whether the adjustment is physically reasonable.
  4. [Fig. 4 caption] The caption says 'There is heating in the dust cloud at the application of polarity switching observed in both ground and microgravity experiments,' while the text emphasizes that only microgravity shows a significant, extended heating. Please clarify that the ground-based heating is momentary and much smaller, or adjust the caption to avoid apparent contradiction.
  5. [References] Reference 13 is cited as 'private communications' for the plasma collapse that motivates the central hypothesis. For a load-bearing point in the proposed mechanism, this should be replaced by a citable published source or by direct measurements presented in this paper.

Circularity Check

2 steps flagged · score 6.0 of 10

The simulation-support claim reduces to fitted inputs: the 2.5 ms Coulomb-like phase and the 3→2→1.5→1 mm screening-length sequence are chosen to reproduce the observed heating and decay, so the inferred plasma-collapse mechanism is not independently tested.

  1. fitted input called prediction [Sec. IV, Numerical Modeling (paragraph describing simulation steps)]
    "At the onset of polarity switching, a 2.5 ms suppression of the plasma12,13 is modeled by allowing the screening length of the particles to become disturbed, i.e., kscreening is allowed to become large, and the particles are allowed to have a more Coulomb-like particle interaction during this period. This 2.5 ms is empirically chosen to best reproduce the heating event numerically."

    The duration of the Coulomb-like phase is the simulation input that encodes the hypothesized plasma collapse, and it is adjusted until the simulated temperature rise matches the measurement. The paper then presents the agreement as support for the collapse mechanism ('Based on our simulations, we can replicate the thermal response...'). The reproduced heating is therefore a product of the fit rather than an independent validation of the mechanism.

  2. fitted input called prediction [Sec. IV, Numerical Modeling (discussion of Fig. 7)]
    "The results of the simulations suggest that immediately after the heating event, an effective screening length kscreening ≈ 3 mm for the first video frame, followed by an effective screening length of ≈ 2 mm, provides an effective fit to the experimental observations... Then, for t > 0.4 s, kscreening ≈ 1.0 mm provides reasonable agreement with the experimental data."

    The screening-length values are selected post hoc so the simulated temperature decay overlaps the experimental curve. The inferred screening-length evolution (3→2→1.5→1 mm) and the associated claim of increasing plasma density are read off from these fitted values, so the Fig. 7(a) agreement is a fit to the target data, not a prediction that independently confirms the screening-length mechanism.

full rationale

The experimental findings—microgravity dust heating at polarity onset, cloud expansion, and slow decay—are self-contained observations. The circularity lies in the modeling claim that the simulation supports the proposed plasma-collapse/screening mechanism. The key parameters that realize that mechanism, the 2.5 ms Coulomb-like phase and the time-dependent screening-length sequence, are explicitly fitted to reproduce the measured heating and decay curves. Because the simulated temperature evolution is controlled by these fitted inputs, the agreement in Fig. 7(a) cannot serve as independent evidence for the mechanism; it is a restatement of the fit. No load-bearing self-citation chain is present: the cited ionization-wave and dust-charging studies are external and the private-communication reference is not the basis of the central reduction. The central claim is thus partially circular: the observation survives, but the proposed causal story reduces to parameters chosen to match the data it is supposed to explain.

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

The paper's central mechanism rests on several free parameters: the duration of the supposed plasma suppression and a time profile of effective screening lengths, all chosen to match the measured temperature curves. The experimental comparison provides external benchmarks, but the screening-length variation itself is not directly measured. No new physical entities are introduced.

free parameters (4)
  • 2.5 ms plasma suppression / Coulomb-like phase duration = 2.5 ms
    Chosen to best reproduce the measured heating event (Sec. IV: 'This 2.5 ms is empirically chosen to best reproduce the heating event numerically').
  • Post-switch effective screening length, early phase = 3 mm, then 2 mm
    Time-dependent screening lengths giving a fit to experimental temperature decay for 0<t<0.25 s, larger than kDe=1.45 mm.
  • Post-switch effective screening length, late phase = 1.5 mm, then 1.0 mm
    Chosen to fit temperature data for 0.25<t<0.4 s and t>0.4 s.
  • Drag coefficient adjustment = not stated
    The drag coefficient in YOAKMuM is adjusted to match the measured injection drift velocity (Sec. IV).
assumptions (6)
  • domain assumption Dust-dust interactions are pairwise Yukawa with a single effective screening length (Eqs. 1 and 3).
    Standard model for dusty plasma interactions invoked from prior literature; used throughout experiment interpretation and MD.
  • domain assumption Dust charge remains fixed during the simulation; charge is computed from OML and plasma parameters.
    Computational simplification stated in Sec. IV; real charge may vary during the transient, which is exactly what the mechanism proposes, so the model excludes a possibly relevant effect.
  • ad hoc to paper At polarity switching, the plasma is suppressed for 2.5 ms, modeled by letting the screening length become large (Coulomb-like).
    This is the key mechanism input, and the duration is empirically chosen to reproduce the heating; no direct measurement is presented in this paper.
  • domain assumption PIV velocity distributions are fit to Maxwell-Boltzmann to define effective dust temperature.
    Standard PIV analysis, but a non-equilibrium, expanding cloud may not be Maxwellian; contributes to systematic uncertainty in T.
  • domain assumption Microgravity and ground conditions are otherwise identical (same scripts, pressure, current).
    Needed for attribution of differences to gravity; camera height and sheath position differ on the ground.
  • domain assumption Before switching, the effective screening length equals the electron Debye length and remains representative of plasma density changes after.
    Initial condition for the MD and for interpreting the fitted screening lengths; kDe comes from Pustylnik et al.

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Cite this review

Pith. "Pith review of Experiments and modeling of dust particle heating resulting from changes in polarity switching in the PK-4 microgravity laboratory." pith.science (2026). https://pith.science/paper/ZR3Q2ZKW

@misc{pith2026250112248,
  author       = {Pith},
  title        = {Pith review of: Experiments and modeling of dust particle heating resulting from changes in polarity switching in the PK-4 microgravity laboratory},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ZR3Q2ZKW}},
  note         = {Machine review of arXiv:2501.12248}
}
read the original abstract

In the presence of gravity, the micron-sized charged dust particles in a complex (dusty) plasma are compressed into thin layers. However, under the microgravity conditions of the Plasma Kristall-4 (PK-4) experiment on the International Space Station (ISS), the particles fill the plasma, allowing us to investigate the properties of a three-dimensional (3D) multi-particle system. This paper examines the change in the spatial ordering and thermal state of the particle system created when dust particles are stopped by periodic oscillations of the electric field, known as polarity switching, in a dc glow discharge plasma. Data from the ISS is compared against experiments performed using a ground-based reference version of PK-4 and numerical simulations. Initial results show substantive differences in the velocity distribution functions between experiments on the ground and in microgravity. There are also differences in the motion of the dust cloud, in microgravity there is an expansion of the dust cloud at the application of polarity switching which is not seen in the ground-based experiments. It is proposed that the dust cloud in microgravity gains thermal energy at the application of polarity switching due to this expansion. Simulation results suggest that this may be due to a modification in the effective screening length of the dust at the onset of polarity switching, which arises from a configuration energy between the charged particles. Experimental measurements and simulations show that an extended time (much greater than the Epstein drag decay) is required to dissipate this energy.

Figures

Figures reproduced from arXiv: 2501.12248 by the authors.

Figure 1
Figure 1. (c) of Ivlev et al. This change in ion-wakes could correspond to a change in the potential energy structure of the system. Dust particle interactions can be described using a Yukawa-like dust–dust interaction model,9 seen in the following equation: UDustDustðÞr ¼ Q 4p0r e  r kD ; (1) where U is the interparticle electric potential, 0 is the vacuum permit￾tivity constant, kD is the relevant screening (Debye) leng… view at source ↗
Figure 2
Figure 2. FIG. 2 [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. (a), that quantifies the particle motion in the field of view of the camera. These vector fields are used to generate velocity distributions in each vector direction and fit using a Maxwell–Boltzmann distribu￾tion, fvðÞ ¼ ffiffiffiffiffiffiffi m 2kBT q e  mvv ðÞ drift 2 2kBT , to extract the drift velocity, vdrift, and the kinetic temperature of the dust, T. Representative distributions are seen in Figs. 3(b) and … view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: FIG. 4 [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 6
Figure 6. Figure 6: FIG. 6 [PITH_FULL_IMAGE:figures/full_fig_p007_6.png]
Figure 5
Figure 5. Figure 5: FIG. 5 [PITH_FULL_IMAGE:figures/full_fig_p007_5.png]
Figure 7
Figure 7. Figure 7: FIG. 7 [PITH_FULL_IMAGE:figures/full_fig_p009_7.png]

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Anisotropic anomalous diffusion in microgravity dusty plasma. Part One: Nonextensive Statistical Analysis

    physics.plasm-ph 2024-11 conditional novelty 5.0 of 10

    Dust diffusion in the ISS PK-4 plasma is strongly anisotropic and non-Gaussian, with axial superdiffusion that may cross into Lévy behavior at higher pressure.

Reference graph

Works this paper leans on

8 extracted references · 8 canonical work pages · cited by 1 Pith paper

  1. [1]

    Dust acoustic waves in strongly coupled dusty plasmas,

    1M. Rosenberg and G. Kalman, “Dust acoustic waves in strongly coupled dusty plasmas,” Phys. Rev. E 56(6), 7166–7173 (1997). 2C. Thompson, A. Barkan, N. D ’Angelo, and R. L. Merlino, “Dust acoustic waves in a direct current glow discharge, ” Phys. Plasmas 4(7), 2331 –2335 (1997). 3J. Goree, B. Liu, M. Y. Pustylnik, H. M. Thomas, V. E. Fortov, A. M. Lipaev,...

    work page 1997

  2. [2]

    Plasmakristall-4: New complex (dusty) plasma laboratory on board the International Space Station,

    Lavrenko, G. I. Padalka, E. O. Serova, A. M. Samokutyayev, and S. Christoforetti, “Plasmakristall-4: New complex (dusty) plasma laboratory on board the International Space Station, ” Rev. Sci. Instrum. 87(9), 093505 (2016). 12P. Hartmann, M. Rosenberg, Z. Juhasz, L. S. Matthews, D. L. Sanford, K

    work page 2016

  3. [3]

    Ionization waves in the PK-4 direct current neon discharge,

    Vermillion, J. C. Reyes, and T. W. Hyde, “Ionization waves in the PK-4 direct current neon discharge, ” Plasma Sources Sci. Technol. 29, 115014 (2020). 13L. Scott, E. Thomas, Jr., J. D. Williams, T. W. Hyde, and L. S. Matthews, private communications (2019). 14A. V. Ivlev, G. E. Morfill, H. M. Thomas, C. R €ath, G. Joyce, P. Huber, R

    work page 2020

  4. [4]

    First observation of electrorheological plasmas,

    Kompaneets, V. E. Fortov, A. M. Lipaev, V. I. Molotkov, T. Reiter, M. Turin, and P. Vinogradov, “First observation of electrorheological plasmas, ” Phys. Rev. Lett. 100(9), 095003 (2008). 15T. Antonova, C.-R. Du, A. V. Ivlev, B. M. Annaratone, L.-J. Hou, R

    work page 2008

  5. [5]

    Microparticles deep in the plasma sheath: Coulomb ‘explosion’,

    Kompaneets, H. M. Thomas, and G. E. Morfill, “Microparticles deep in the plasma sheath: Coulomb ‘explosion’,” Phys. Plasmas 19(9), 093709 (2012). 16P. S. Epstein, “On the resistance experienced by spheres in their motion through gases,” Phys. Rev. 23(6), 710–733 (1924). 17B. Liu, J. Goree, V. Nosenko, and L. Boufendi, “Radiation pressure and gas drag forc...

    work page 2012

  6. [6]

    Complex plasma laboratory PK-3 Plus on the International Space Station,

    Lipaev, T. Hagl, H. Rothermel, S. A. Khrapak, R. K. Suetterlin, M. Rubin-Zuzic, O. F. Petrov, V. I. Tokarev, and S. K. Krikalev, “Complex plasma laboratory PK-3 Plus on the International Space Station, ” New J. Phys. 10(3), 033036 (2008). 20M. Y. Pustylnik, B. Klumov, M. Rubin-Zuzic, A. M. Lipaev, V. Nosenko, D

    work page 2008

  7. [7]

    Influence of Temporal Variations in Plasma Conditions on the Electric Potential Near Self-Organized Dust Chains

    Erdle, A. D. Usachev, A. V. Zobnin, V. I. Molotkov, G. Joyce, H. M. Thomas, M. H. Thoma, O. F. Petrov, V. E. Fortov, and O. Kononenko, “Three-dimen- sional structure of a string-fluid complex plasma, ” Phys. Rev. Res. 2(3), 033314 (2020). 21A. V. Ivlev, M. H. Thoma, C. R €ath, G. Joyce, and G. E. Morfill, “Complex plas- mas in external fields: The role of...

    work page Pith review arXiv 2020

  8. [8]

    Effect of ionization waves on dust chain formation in a DC discharge,

    Zobnin, M. H. Thoma, O. F. Petrov, H. M. Thomas, and O. V. Novitskiy, “Effect of ionization waves on dust chain formation in a DC discharge, ” J. Plasma Phys. 87(6), 905870618 (2021). 36J. K. Meyer and R. L. Merlino, “Evolution of dust clouds in afterglow plasmas, ” IEEE Trans. Plasma Sci. 44(4), 473–478 (2016). 37N. Chaubey and J. Goree, “Coulomb expansi...

    work page 2021

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Reviewed August 10, 2026 · model on record in the stance chip above.