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D. Tsiklauri

Publications and source records attributed to D. Tsiklauri.

At least 19 recordsLinked to original sources

A 2D Hydrothermodynamic Analytical Model for Rapid Tumor Ablation using High-Intensity Focused Ultrasound

We establish a self-consistent 2D hydrothermodynamic analytical model for high-intensity focused ultrasound tumor ablation. Expanding compressible Navier-Stokes equations to second order demonstrates that a stationary cellular matrix suppresses acoustic streaming ($\mathbf{v}_2 = 0$). This constraint forces the absorbed wave momentum flux to convert entirely into localized, time-averaged static pressure gradients ($\nabla \langle p_2 \rangle = \mathbf{F}_2$), bridging non-linear hydrodynamics with thermodynamic dissipation. Solving the non-diffusive Pennes bioheat equation under a $1.0\,\text{s}$ top-hat pulse reveals that a spherically focusing geometry ($\propto 1/r^2$) overrides exponential damping past a critical geometric threshold ($r_{\text{crit}} = 2x_0$), preventing upstream skin overheating. We derive an optimization criterion where the absorption coefficient matches half the inverse target depth ($\alpha = 1/2x_0$). Solving the non-isothermal Arrhenius integral yields a sharp lesion boundary radius at $r_b = 0.75\,w_0$, where the volume average reaches $72.1^\circ\text{C}$ while the core peaks at $90.0^\circ\text{C}$. Post-pulse 2D free-space Green's function convolution confirms immediate monotonic thermal decay ($\partial \theta/\partial t' < 0$) outside this boundary. This closed-form framework provides explicit scaling laws for non-invasive wave-matter thermal confinement, bypassing computationally heavy numerical simulations.

physics.med-ph

Exact 1D Nonlinear Solutions for Proton-Driven Plasma Wakefields: Benchmarking Against AWAKE Data Envelopes

The analytical modeling of a plasma wakefield driven by a relativistic proton beam is an element in optimizing advanced plasma-based acceleration schemes. In this work, we present a 1D nonlinear fluid framework under the quasi-static approximation to describe the wake potential excited by a positively charged proton driver. We examine our model using a two-bunch pump-probe configuration, demonstrating close agreement between the analytical invariants and adaptive numerical integrations. The distinct geometric curvature changes observed at the micro-bunch boundaries are shown to be physical consequences of step-discontinuities in the second derivative of the wake potential across the beam interfaces. Furthermore, by scaling this numerical framework to a train of $N=100$ micro-bunches undergoing seeded self-modulation (SSM), we model the physical parameters of the CERN AWAKE facility ($n_0 = 7.0 \times 10^{14}\text{ cm}^{-3}$). Our model replicates the characteristic linear growth envelope and matches the calibrated field envelope boundaries of approximately $\pm 0.75\text{ GV/m}$ inferred from the experiment. This piece-wise framework provides a computationally efficient foundation for investigating customized, asymmetric micro-bunch profiles designed to optimize the transformer ratio beyond the fundamental symmetric limit of 2.

physics.plasm-ph

Unpinning of trapped oil droplets via non-resonant acoustic streaming in capillary tubes

We establish self-consistent analytical model demonstrating that trapped non-wetting liquid phases in narrow capillary channels can be successfully unpinned via non-resonant, second-order acoustic streaming coupled with background static drive gradients. Moving away from boundary-guided or resonant mechanisms, our approach exploits the bulk acoustic-wind force density generated by the steady-state momentum flux of attenuated first-order linear wave interactions. By expanding the hydrodynamic equations up to second order, we determine the critical assisted acoustic wave amplitude required to break capillary pinning thresholds and derive an explicit formulation for steady transport velocity under viscous wall constraints. Furthermore, incorporating both boundary-layer wall effects and bulk core thermo-viscous dissipation reveals a natural mathematical optimum condition where the spatial absorption coefficient matches half the inverse distance to the target droplet ($\alpha = 1/(2x_0)$). This condition is then numerically validated and cross-correlated against legacy industrial frequency baselines, providing a fundamental theoretical framework for minimizing transducer power requirements while maximizing localized mobilization velocities in geological pore networks. Finally, we demonstrate that this optimal operational frequency scales inversely with the transmission distance, providing an analytical framework to optimize downhole acoustic tools according to spatial damping constraints of the specific formation rather than relying on rigid hardware parameters.

physics.flu-dyn

Phase-mixing of acoustic waves: From the solar tachocline to marine vessel hydroacoustics

We adapt the \textit{magnetohydrodynamic} wave phase-mixing paradigm [Tsiklauri et al. (2003)] to investigate harmonic wave, Gaussian pulse, and hyperbolic pulse propagation and damping in media governed by transverse sound speed gradients. This universal mechanism is applied to two distinct problems using the harmonic wave phase-mixed solutions. First, we resolve the 26-year-old helioseismic mystery of low-degree global $p$-mode linewidth anomalies observed by BiSON above $\nu \approx 3000\,\mu\text{Hz}$, demonstrating that a localised, non-turbulent sound speed gradient in the solar tachocline shear zone acts as the necessary high-efficiency energy sink. Second, we translate this formalism into a terrestrial metamaterial fluid engineering design. We show that an engineered microstructured mesh or stern cowl generating a controlled radial sound speed gradient induces severe near-field phase-mixing. This collapses the traditional bulk viscous damping length of $100\text{-kHz}$ propeller acoustic signatures from several kilometres down to a practical design envelope of approximately $10\text{ metres}$, providing an actionable paradigm for compact stealth shielding. Finally, as an independent theoretical extension, we establish a new power-law scaling governing a hyperbolic secant-squared pulse evolution: under developed-stage phase-mixing, its peak wave envelope decays as $\max(P_1) \propto x^{-9/2}$.

astro-ph.SR

The Effect of Anomalous Resistivity on Tearing Instability

We study the modification of classical tearing instability due to anomalous resistivity by incorporating a variable, second-order resistivity model into the resistive magnetohydrodynamics (MHD) framework. We evaluate the resulting {weakly non-linear boundary-layer scaling laws under a localized current-feedback mechanism}. By extending the {inner-layer analysis to capture localized current feedback}, we resolve localized spatial singularities ($\delta$ and $\delta'$) at the threshold boundary. These singularities generate unexpected matching jump conditions, demonstrating an early-stage phase-slip layer that forces a hyperbolic, time-dependent growth rate divergence prior to macroscopic saturation. Physical estimates for fusion devices and solar flares prove that this {consistent weakly non-linear matching formulation} triggers an abrupt transition into the explosive reconnection regime, offering an exact analytical resolution to the long-standing solar and tokamak flare/disruption ``trigger problem,'' respectively. Finally, a comparative analysis using a truncated linear expansion of the threshold model regularizes the singular behavior, confirming that the explosive finite-time singularity is uniquely driven by the higher-order non-linear current feedback.

physics.plasm-ph

Peristaltic Flow in Compressible, Ideal Magnetohydrodynamics: A Mechanism For Solar Spicules

We present analytical model for peristaltic transport within compressible, ideal magnetohydrodynamics (MHD). By employing small-amplitude perturbation expansion, under thin-tube long-wavelength approximation with a uniform axial background magnetic field, we study non-linear coupling between thermodynamic pressure variations and Maxwell's magnetic tension stresses. The resulting net time-averaged volumetric flow rate $\langle Q \rangle$ is calculated. When applied to solar chromospheric spicules under equipartition constraints ($\beta \sim 1$), where sound speed matches the Alfv{\'e}n speed, we find $\langle Q \rangle = 4\epsilon^2/(M^2-1)$. Because the denominator remains positive across all operational supersonic Mach numbers ($M \approx 2\text{--}10$), upward-propagating mechanical disturbances drive a highly directional, collimated upward flow which we interpret as a spicule. Estimates show that for observationally realistic magnetosonic waves with amplitudes of $\approx 10\%$, the peristaltic mechanism generates a localized mass flux $\approx 100$ times that of solar wind. We propose an explicit observational signature of this mechanism, wherein the launch of individual spicular jets is directly preceded by magnetosonic wave trains detectable as localized intensity modulations. Beyond solar chromospheric application, the model may be applicable to traveling magnetic field pinches in laboratory plasma devices and astrophysical mass-loading processes in stellar winds and inner regions of magnetized accretion disks.

astro-ph.SR

Interaction of a spatially uniform electron beam with a rotational magnetic hole in a form of a Harris current sheet

In this work we use particle-in-cell (PIC) numerical simulations to study interaction of a spatially uniform electron beam with a rotational magnetic hole in a form of a Harris current sheet. We vary width of the Harris current sheet to investigate how this affects the quasi-linear relaxation, i.e. plateau formation of the bump-on-tail unstable electron beam. We find that when width of the Harris current sheet approaches and becomes smaller than the electron gyro-radius, quasi-linear relaxation becomes hampered and a positive slope in the electron velocity distribution function (VDF) persists. We explain this by the effects of non-conservation of electron magnetic moment, which, as recent works suggest, can maintain the positive slope of the VDF. In part, this can explain why some electron beams (the ones that interact with narrow magnetic holes with sharp boundaries, represented in our study by a Harris current sheet) in the solar wind travel much longer distances than predicted by the quasi-linear theory, at least in those cases when the electron beams slide along the current sheets that are abundant when the different-speed solar wind streams interact with each other.

astro-ph.SR

Two dimensional modelling of the interaction between electromagnetic waves and plasma-metamaterial composite structures using the particle-in-cell method

In this work we (i) extend previous 1D studies of electromagnetic (EM) wave propagation in an over-dense plasma-metamaterial composite into two spatial dimensions and (ii) study blocking of EM waves by the composite 2D structures (barriers). Such barriers are formed when metamaterial spatially co-exists with a plasma density depletion in a form of a slab or two-dimensional density rectangular depletions (DRDs). This is analogous to EM wave trapping by preformed density cavities in near-critical density plasmas, studied before. We find that plasma-metamaterial composite allows to block EM waves by both slab and DRD configurations, thus forming a standing wave at the edge of an opaque region. The standing wave subsequently damps which offers applications such as heat deposition or substrate materials (micro)machining depending on EM wave intensity. The established results may find future applications such as: more efficient plasma vapour deposition, controlling EM wave propagation (EM wave blocking) in invisibility cloaks and alike. The EM wave blocking conditions are elucidated by a set of particle-in-cell (PIC) numerical simulations.

physics.plasm-ph

The effect of external magnetic field on electron scale Kelvin-Helmholtz instability

We use particle-in-cell, fully electromagnetic, plasma kinetic simulation to study the effect of external magnetic field on electron scale Kelvin-Helmholtz instability (ESKHI). The results are applicable to collisionless plasmas when e.g. solar wind interacts with planetary magnetospheres or magnetic field is generated in AGN jets. We find that as in the case of magnetohydrodynamic KHI, in the kinetic regime, presence of external magnetic field reduces growth rate of the instability. In MHD case there is known threshold magnetic field for KHI stabilization, while for ESKHI this is to be analytically determined. Without a kinetic analytical expression, we use several numerical simulation runs to establish an empirical dependence of ESKHI growth rate, $Γ(B_0)ω_{\rm pe}$, on the strength of applied external magnetic field. We find the best fit is hyperbolic, $Γ(B_0)ω_{\rm pe}=Γ_0ω_{\rm pe}/(A+B\bar B_0)$, where $Γ_0$ is the ESKHI growth rate without external magnetic field and $\bar B_0=B_0/B_{\rm MHD}$ is the ratio of external and two-fluid MHD stability threshold magnetic field, derived here. An analytical theory to back up this growth rate dependence on external magnetic field is needed. The results suggest that in astrophysical settings where strong magnetic field pre-exists, the generation of an additional magnetic field by the ESKHI is suppressed, which implies that the Nature provides a "safety valve" -- natural protection not to "over-generate" magnetic field by ESKHI mechanism. Remarkably, we find that our two-fluid MHD threshold magnetic field is the same (up to a factor $\sqrt{γ_0}$) as the DC saturation magnetic field, previously predicted by fully kinetic theory.

physics.plasm-ph

Particle acceleration by sub-proton cyclotron frequency spectrum of dispersive Alfven waves in inhomogeneous solar coronal plasmas

The problem of explaining observed soft X-ray fluxes during solar flares, which invokes acceleration of large fraction of electrons, if the acceleration takes places at the solar coronal loop-top, can potentially be solved by postulating that flare at loop-top creates dispersive Alfven waves (DAWs) which propagate towards the foot-points. As DAWs move in progressively denser parts of the loop (due to gravitational stratification) the large fraction of electrons is no longer needed. Here we extend our previous results by considering $f ^{-1}$ frequency spectrum of DAWs and add ${\rm He^{++}}$ ions using fully kinetic particle-in-cell (PIC) simulations. We consider cases when transverse density gradient is in the range ${ 4-40} c/ω_{\rm { pe}}$ and DAW driving frequency is $0.3-0.6ω_{\rm { cp}}$. We find that (i) The frequency spectrum case does not affect electron acceleration fraction in the like-to-like cases, but few times larger percentage of ${\rm He^{++}}$ heating is seen due to ion cyclotron resonance; (ii) In cases when counter propagating DAWs collide multiple-times, much larger electron and ion acceleration fractions are found, but the process is intermittent in time. This is because intensive heating (temperature increase) makes the-above-thermal-fraction smaller; Also more isotropic velocity distributions are seen; (iii) Development of kink oscillations occurs when DAWs collide; (iv) Scaling of the magnetic fluctuations power spectrum steepening in the higher-density regions is seen, due to wave refraction. Our PIC runs produce much steeper slopes than the orginal spectrum, indicating that the electron-scale physics has a notable effect of DAW spectrum evolution.

astro-ph.SR

Prediction of short stellar activity cycles using derived and established empirical relations between activity and rotation periods

In our previous work, we investigated the occurrence rate of super-flares on various types of stars and their statistical properties, with a particular focus on G-type dwarfs, using entire Kepler data. The said study also considered how the statistics change with stellar rotation period, which in turn, had to be determined. Using such new data, as a by-product, we found 138 Kepler IDs of F and G types main sequence stars with rotation periods less than a day ($P_{\rm rot}<1$ d). On one hand, previous studies have revealed short activity cycles in F-type and G-type stars and the question investigated was whether or not short-term activity cycles are a common phenomenon in these stars. On the other hand, extensive studies exist which establish empirical connection between a star's activity cycle and rotation periods. In this study, we compile all available Kepler data with $P_{\rm rot}<1$ d, derive and use, established empirical relation between $P_{\rm cyc}$ and $P_{\rm rot}$ with the aim to provide predictions for very short $5.09\leq P_{\rm cyc}\leq 38.46$ d cases in a tabular form. We propose an observation to measure $P_{\rm cyc}$ using monitoring program of stellar activity (e.g. activity-related chromospheric emission S-index) or similar means for the Kepler IDs found in this study in order put to test the derived here empirical relations between $P_{\rm cyc}$ and $P_{\rm rot}$. We also propose an alternative method for measuring very short $P_{\rm cyc}$, using flare-detection algorithms applied to future space mission data.

astro-ph.SR

New cases of super-flares on slowly rotating solar-type stars and large amplitude super-flares in G- and M-type main-sequence stars

In our previous work, we searched for super-flares on different types of stars while focusing on G-type dwarfs using entire Kepler data to study statistical properties of the occurrence rate of super-flares. Using these new data, as a by-product, we found fourteen cases of super-flare detection on thirteen slowly rotating Sun-like stars with rotation periods of 24.5 to 44 days. This result supports earlier conclusion by others that the Sun may possibly have a surprise super-flare. Moreover, we found twelve and seven new cases of detection of exceptionally large amplitude super-flares on six and four main-sequence stars of G- and M-type, respectively. No large-amplitude flares were detected in A, F, or K main-sequence stars. Here we present preliminary analysis of these cases. The super-flare detection, i.e. an estimation of flare energy, is based on a more accurate method compared to previous studies. We fit an exponential decay function to flare light curves and study the relation between e-folding decay time, $τ$, vs. flare amplitude and flare energy. We find that for slowly rotating Sun-like stars, large values of $τ$ correspond to small flare energies and small values of $τ$ correspond to high flare energies considered. Similarly, $τ$ is large for small flare amplitudes and $τ$ is small for large amplitudes considered. However, there is no clear relation between these parameters for large amplitude super-flares in the main sequence G- and M-type stars, as we could not establish clear functional dependence between the parameters via standard fitting algorithms.

astro-ph.SR

Main-sequence star super-flares based on entire Kepler data

We wrote and used an automated flare detection Python script to search for super-flares on main-sequence stars of types A, F, G, K, and M in Kepler's long-cadence data from Q0 to Q17. We studied the statistical properties of the occurrence rate of super-flares. For the G-type data set, we compared our results with the previous results of Okamoto et al. 2021 by splitting the data set into four rotational bands. We found similar power law indices for the flare frequency distribution. Hence, we show that inclusion of high-pass filter, sample biases, gyrochronology and completeness of flare detection is of no significance, as our results are similar to Okamoto et al. 2021. We estimated that a super-flare on G-type dwarfs of energy of $10^{35}$ erg occurs on a star once every 4360 years. We found 4637 super-flares on 1896 G-type dwarfs. Moreover, we found 321, 1125, 4538 and 5445 super-flares on 136, 522, 770 and 312 dwarfs of types A, F, K and M, respectively. We found that the occurrence rate ($dN/dE$) of super-flares versus flare energy, $E$, shows a power-law distribution with $dN/dE \propto E^{-α}$, where $α\simeq$ 2.0 to 2.1 for the spectral types from F-type to M-type stars. In contrast, the obtained $α\simeq$ 1.3 for A-type stars suggests that the flare conditions differ from the rest spectral-type stars. We note an increase in flare incidence rate in F-type to M-type stars and a decrease in A-type to F-type stars.

astro-ph.SR

The effect of particle gas composition and boundary conditions on triboplasma generation: a computational study using the particle-in-cell method

Two dimensional particle in cell simulations of free charge creation by collisional ionization of C12 and C60 molecules immersed in plasma for the parameters of relevance to plasma gasification are presented. Our main findings are that (i) in uniform plasmas with smooth walls two optimal values which emerge for free electron production by collisional ionization (i.e. a most efficient discharge condition creation) are $C60:C12$ fractions of $10:90$ and $80:20$, (ii) in plasmas with rough walls, modelled by comb-like electric field at the boundary, the case of tangential electric field creates significant charge localization in C12+ and C60+ species, again creating most favorable discharge condition for tribo-electrically generated plasma. The numerical simulation results are discussed with reference to recent triboelectric plasma experiments and are corroborated by suitable analytical models.

physics.plasm-ph

Particle-in-cell simulations of the relaxation of electron beams in inhomogeneous solar wind plasmas

Previous theoretical considerations of electron beam relaxation in inhomogeneous plasmas have indicated that the effects of the irregular solar wind may account for the poor agreement of homogeneous modelling with the observations. Quasi-linear theory and Hamiltonian models based on Zakharov's equations have indicated that when a level of density fluctuations is above a given threshold, density irregularities act to de-resonate the beam-plasma interaction, restricting Langmuir wave growth on the expense of beam energy. This work presents the first fully kinetic particle-in-cell (PIC) simulations of beam relaxation under the influence of density irregularities. We aim to independently determine the influence of background inhomogeneity on the beam-plasma system, and to test theoretical predictions and alternative models using a fully kinetic treatment. We carry out 1D PIC simulations of a bump-on-tail unstable electron beam in the presence of increasing levels of background inhomogeneity using the fully electromagnetic, relativistic EPOCH PIC code. We find that in the case of homogeneous background plasma density, Langmuir wave packets are generated at the resonant condition and then quasi-liear relaxation leads to a dynamic increase of wavenumbers generated. No electron acceleration is seen - unlike in the inhomogeneous experiments, all of which produce high-energy electrons. For the inhomogeneous experiments we also observe the generation of backwards propagating Langmuir waves, which is shown directly to be due to the refraction of the packets off the density gradients. Our fully kinetic PIC simulations broadly confirm the findings of quasi-linear theory and the Hamiltonian model based on Zakharov's equations. Strong density fluctuations modify properties of excited Langmuir waves altering their dispersion properties.

physics.plasm-ph

Collisionless, phase-mixed, dispersive, Gaussian Alfven pulse in transversely inhomogeneous plasma

In the previous works harmonic, phase-mixed, Alfven wave dynamics was considered both in the kinetic and magnetohydrodynamic regimes. Up today only magnetohydrodynamic, phase-mixed, Gaussian Alfven pulses were investigated. In the present work we extend this into kinetic regime. Here phase-mixed, Gaussian Alfven pulses are studied, which are more appropriate for solar flares, than harmonic waves, as the flares are impulsive in nature. Collisionless, phase-mixed, dispersive, Gaussian Alfven pulse in transversely inhomogeneous plasma is investigated by particle-in-cell (PIC) simulations and by an analytical model. The pulse is in inertial regime with plasma beta less than electron-to-ion mass ratio and has a spatial width of 12 ion inertial length. The linear analytical model predicts that the pulse amplitude decrease is described by the linear Korteweg de Vries (KdV) equation. The numerical and analytical solution of the linear KdV equation produces the pulse amplitude decrease in time as $t^{-1}$. The latter scaling law is corroborated by full PIC simulations. It is shown that the pulse amplitude decrease is due to dispersive effects, while electron acceleration is due to Landau damping of the phase-mixed waves. The established amplitude decrease in time as $t^{-1}$ is different from the MHD scaling of $t^{-3/2}$. This can be attributed to the dispersive effects resulting in the different scaling compared to MHD, where the resistive effects cause the damping, in turn, enhanced by the inhomogeneity. Reducing background plasma temperature and increase in ion mass yields more efficient particle acceleration.

astro-ph.SR

Alfvén wave phase-mixing in flows: Why over-dense, solar coronal, open magnetic field structures are cool?

The motivation for this study is to include the effect of plasma flow in Alfvén wave (AW) damping via phase mixing and to explore the observational implications. Our magnetohydrodynamic (MHD) simulations and analytical calculations show that, when a background flow is present, mathematical expressions for the AW damping via phase mixing are modified by the following substitution: $C_A^\prime(x) \to C_A^\prime(x)+V_0^\prime(x)$, where $C_A$ and $V_0$ are AW phase and the flow speeds, and the prime denotes a derivative in the direction across the background magnetic field. In uniform magnetic fields and over-dense plasma structures, where $C_A$ is smaller than in the surrounding plasma, the flow, which is confined to the structure and going in the same direction as the AW, reduces the effect of phase-mixing, because on the edges of the structure $C_A^\prime$ and $V_0^\prime$ have opposite signs. Thus, the wave damps by means of slower phase-mixing compared to the case without the flow. This is the result of the co-directional flow that reduces the wave front stretching in the transverse direction. We apply our findings to addressing the question why over-dense solar coronal open magnetic field structures (OMFS) are cooler than the background plasma. Observations show that the over-dense OMFS (e.g. solar coronal polar plumes) are cooler than surrounding plasma and that, in these structures, Doppler line-broadening is consistent with bulk plasma motions, such as AW. If over-dense solar coronal OMFS are heated by AW damping via phase-mixing, we show that, co-directional with AW, plasma flow in them reduces the phase-mixing induced-heating, thus providing an explanation of why they appear cooler than the background.

astro-ph.SR

Self-consistent particle-in-cell simulations of fundamental and harmonic plasma radio emission mechanisms

Aims. The simulation of three-wave interaction based plasma emission, thought to be the underlying mechanism for Type III solar radio bursts, is a challenging task requiring fully-kinetic, multi-dimensional models. This paper aims to resolve a contradiction in past attempts, whereby some studies indicate that no such processes occur. Methods. We self-consistently simulate three-waved based plasma emission through all stages by using 2D, fully kinetic, electromagnetic particle-in-cell simulations of relaxing electron beams using the EPOCH2D code. Results. Here we present the results of two simulations; Run 1 (nb/n0 = 0.0057, vb/Δvb = vb/Ve = 16) and Run 2 (nb/n0 = 0.05, vb/Δvb = vb/Ve = 8), which we find to permit and prohibit plasma emission respectively. We show that the possibility of plasma emission is contingent upon the frequency of the initial electrostatic waves generated by the bump-in-tail instability, and that these waves may be prohibited from participating in the necessary three-wave interactions due to frequency conservation requirements. In resolving this apparent contradiction through a comprehensive analysis, in this paper we present the first self-consistent demonstration of fundamental and harmonic plasma emission from a single-beam system via fully kinetic numerical simulation. We caution against simulating astrophysical radio bursts using unrealistically dense beams (a common approach which reduces run time), as the resulting non-Langmiur characteristics of the initial wave modes significantly suppresses emission. Comparison of our results also indicates that, contrary to the suggestions of previous authors, an alternative plasma emission mechanism based on two counter-propagating beams is unnecessary in an astrophysical context.

astro-ph.SR