Metal Ejection Research Articles

Reactivity of Zinc Fingers in Oxidizing Environments: Insight from Molecular Models Through Activation Strain Analysis.

The reactivity of Zn2+ tetrahedral complexes with H2O2 was investigated in silico, as a first step in their disruption process. The substrates were chosen to represent the cores of three different zinc finger protein motifs, i. e., a Zn2+ ion coordinated to four cysteines (CCCC), to three cysteines and one histidine (CCCH), and to two cysteines and two histidines (CCHH). The cysteine and histidine ligands were further simplified to methyl thiolate and imidazole, respectively. H2O2 was chosen as an oxidizing agent due to its biological role as a metabolic product and species involved in signaling processes. The mechanism of oxidation of a coordinated cysteinate to sulfenate-κS and the trends for the different substrates were rationalized through activation strain analysis and energy decomposition analysis in the framework of scalar relativistic Density Functional Theory (DFT) calculations at ZORA-M06/TZ2P ae // ZORA-BLYP-D3(BJ)/TZ2P. CCCC is oxidized most easily, an outcome explained considering both electrostatic and orbital interactions. The isomerization to sulfenate-κO was attempted to assess whether this step may affect the ligand dissociation; however, it was found to introduce a kinetic barrier without improving the energetics of the dissociation. Lastly, ligand exchange with free thiolates and selenolates was investigated as a trigger for ligand dissociation, possibly leading to metal ejection; molecular docking simulations also support this hypothesis.

Plasma characteristics and material erosion mechanism in multi-channel wire electrical discharge machining

Multi-channel wire electrical discharge machining (MC-WEDM) is an advanced and high-efficiency machining technology, but its material erosion mechanism remains unclear. In this study, dual-channel wire electrical discharge machining was utilized as a case study to investigate the impact of the plunging current on both the plasma characteristics and material erosion under complex discharge conditions. Force analysis was conducted on the charged particles in the plasma, revealing that the plunging current can influence the trajectory of the plasma by modifying the self-magnetic field. The particle tracking method was employed to simulate the motion of electrons, revealing that in MC-WEDM, electrons exhibited a larger and more uniform distribution. The evolution of the plasma within a single-pulse discharge was observed using high-speed photography technology, and the discharge signals collected from different channels were analyzed. It was observed that the plasma in MC-WEDM experienced more intense back-and-forth sweeping on the workpiece surface, facilitating the ejection of molten metal from the molten pool. The oscillating plasma exhibits a larger processing area and a more uniform distribution of energy, resulting in the formation of larger and shallower discharge craters. Furthermore, the influence of the amplitude and time point of the plunging current on the volume and area of the discharge craters was summarized. Finally, MC-WEDM significantly reduced the occurrence of holes and micro-cracks and exhibited a thinner recast layer in the continuous discharge experiment.

Ultrasonic vibration micro-jet ejection for metal additive manufacture

In comparison to laser additive manufacturing, metal droplet deposition technology presents substantial cost benefits by obviating the necessity for costly metal powders and high-power lasers. Nonetheless, prevalent metal droplet deposition methodologies often grapple with challenges such as intricate drive architectures, substantial droplet volumes, and diminished jetting frequencies. This paper proposes an ultrasonic vibration micro-jet ejection technique and constructs a prototype for metal additive manufacturing. Utilizing ultrasonic vibration of a tool rod, the technique generates a high-frequency acoustic pressure field within the crucible, which facilitates the ejection of molten metal from the nozzle. The study explores two operational modes: continuous jet and on-demand jet. It was determined that the tool rod's amplitude must exceed a certain threshold to initiate metal ejection. As the amplitude further increases, the droplet jetting behavior transitions from uniform to non-uniform ejection states. To enhance formability quality, the study examined the influence of various process parameters on single-pass and three-dimensional forming. The examination of jetted parts revealed that both uniform and non-uniform jets provide satisfactory formability and mechanical performance. This research presents a new direction for achieving efficient metal droplet jetting forming.

Casting of Thin Aluminum Alloy Wire Using a Single Wheel Caster

Thin aluminum alloy (Al-4.7%Mg) wire was cast using a single-wheel caster. The target cross-sectional area of the thin wire was less than 20 mm2. Use of a copper wheel with a groove and a molten metal ejection nozzle was proposed to cast thin wire. The molten metal ejection nozzle was used to eject a small cross-sectional area of the melt into the narrow groove on the wheel. The relationship among wheel speed, nozzle size, melt ejection speed, stability of the melt on the wheel, and cross-sectional area of the wire was investigated. When the diameter of the nozzle hole was 1.5 or 2 mm, the target was attained. When the nozzle diameter was larger than 3 mm, the cross-sectional area was greater than 20 mm2. When the diameter of the nozzle hole was smaller than 1 mm, the melt flow was unstable. A round wire could be cast at wheel speeds ranging from 9 m/min to 14 m/min. The smallest wire cross-sectional area was 4.7 mm2.

SIMULATION OF THE PROCESS OF FILLING POLYSTYRENE FOAM FOUNDRY MOLD WITH THE METAL

Modern approaches to prefabrication production consist in the maximum approximation of the shape and size of the blanks to the finished part, which essentially makes the final part cheaper. One of the methods of precision casting is casting in gasified models, or foam models. The basis is the task of developing a theoretical model of filling a polystyrene foam model with liquid metal. The analysis of the process of filling the mold with a gasified model and the process of filling the mold with a closed sprue system are considered. The analysis of the obtained solutions shows that the movement of the metal has the character of aperiodic oscillations. The speed of metal in quantity is maximum at the initial moment of metal processing in the form and happens as it is filled. The pressure of the steam-gas mixture at the initial moment of time exceeds the pressure of the weak metal in the riser, which provides the possibility of metal ejection from the bowl. At the same time, the pressure in the mold cavity changes little with the increase in gas permeability of the mold, which is explained by the small gap between the melting front of the model and the metal mirror. However, with an increase in gas permeability due to a decrease in back pressure, the speed of the metal in the mold cavity and the path traveled by it increase. The analysis of the system of equations allows predicting the behavior of metal during the design of molds for the summer, which reduces the probability of production defects.

How much metal did the first stars provide to the ultra-faint dwarfs?

Numerical simulations of dwarf galaxies have so far failed to reproduce the observed metallicity-luminosity relation, down to the regime of ultra-faint dwarfs (UFDs). We address this issue by exploring how the first generations of metal-free stars (Pop III) could help increase the mean metallicity ([Fe/H]) of those small and faint galaxies. We ran zoom-in chemo-dynamical simulations of 19 halos extracted from a Λ Cold Dark Matter (CDM) cosmological box and followed their evolution down to redshiftz = 0. Models were validated not only on the basis of galaxy global properties, but also on the detailed investigation of the stellar abundance ratios ([α/Fe]). We identified the necessary conditions for the formation of the first stars in mini-halos and derived constraints on the metal ejection schemes. The impact of Pop III stars on the final metallicity of UFDs was evaluated by considering different stellar mass ranges for their initial mass function (IMF), the influence of pair-instability supernovae (PISNe), and their energetic feedback, as well as the metallicity threshold that marks the transition from the first massive stars to the formation of low-mass long-lived stars. The inclusion of Pop III stars with masses below 140 M⊙, and a standard IMF slope of −1.3 does increase the global metallicity of UFDs, although these are insufficient to resolve the tension with observations. The PISNe with progenitor masses above 140 M⊙do allow the metal content of UFDs to further increase. However, as PISNe are very rare and sometimes absent in the faintest UFDs, they have a limited impact on the global faint end of the metallicity-luminosity relation. Despite a limited number of spectroscopically confirmed members in UFDs, which make the stellar metallicity distribution of some UFDs uncertain, our analysis reveals that this is essentially the metal-rich tail that is missing in the models. The remaining challenges are thus both observational and numerical: (i) to extend high-resolution spectroscopy data samples and confirm the mean metallicity of the faintest UFDs; and (ii) to explain the presence of chemically enriched stars in galaxies with very short star formation histories.

Fiber laser cutting of steel materials with twin spot beam-twin spot setting in kerf width direction

In laser cutting, the temperature distribution would have significant influence on cutting characteristics, and the intensity distribution of a laser beam has a possibility to improve the cutting quality. In this study, a fiber laser beam of Gaussian distribution was divided into two beams by a roof axicon lens, and the cutting characteristics were investigated by using the twin spot Gaussian beam setting in the kerf directions. The cutting experiment of a cold-rolled steel plate with a thickness of 3.2 mm was carried out by a 3 kW fiber laser with a nitrogen assist gas, and the Gaussian mode of 114 μm spot and the twin Gaussian mode of two 110 μm spots were used with the variation of power ratio in twin spot processing. At the exit side of kerf by the twin spot process, the width of the cutting front in the low intensity side became wider than that in the high intensity side, and the dross could be reduced in the low intensity side due to sufficient ejection of the molten metal from the front wall rather than the side wall of kerf. The twin spot process could reduce the dross height below 18 μm in the low intensity side, which is smaller than that by the single Gaussian beam process.

Top-heavy stellar mass distribution in galactic nuclei inferred from the universally high abundance ratio of [Fe/Mg

ABSTRACT Recent observations of active galactic nuclei (AGNs) have shown a high Fe ii/Mg ii line-flux ratio in their broad-line regions, nearly independent of redshift up to z ≳ 6. The high flux ratio requires rapid production of iron in galactic nuclei to reach an abundance ratio of [Fe/Mg] ≳ 0.2 as high as those observed in matured galaxies in the local universe. We propose a possible explanation of rapid iron enrichment in AGNs by massive star formation that follows a top-heavy initial mass function (IMF) with a power-law index of Γ larger than the canonical value of Γ = −2.35 for a Salpeter IMF. Taking into account metal production channels from different types of SNe, we find that the high value of [Fe/Mg] ≳ 0.2 requires the IMF to be characterized with Γ ≳ −1 (Γ ≳ 0) and a high-mass cutoff at Mmax ≃ 100–150 M⊙ (Mmax ≳ 250 M⊙). Given the conditions, core-collapse SNe with M* ≳ 70 M⊙ and pair-instability SNe give a major contribution for iron enrichment. Such top-heavy stellar IMFs would be a natural consequence from mass growth of stars formed in dense AGN discs under Bondi-like gas accretion that is regulated by feedback at M* ≳ 10 M⊙. The massive stellar population formed in AGN discs also leave stellar-mass black hole remnants, whose mergers associated with gravitational-wave emission account for at most 10 per cent of the merger rate inferred from LIGO/Virgo observations to simultaneously explain the high [Fe/Mg] ratio with metal ejection.

Study of Hypervelocity Impingement for Cu Nanoparticles on CuCr Alloy Target Electrodes in Initiating Vacuum Breakdown

The metal particles in vacuum gaps with a strong electric field would be accelerated to hypervelocity and impinge on target electrodes, which could trigger electric breakdown in the vacuum gaps. The objective of this article is to study the hypervelocity impingement phenomena between Cu nanoparticles and CuCr alloy target electrodes based on molecular dynamics (MD) method. The impingement phenomena in the cases of Cu nanoparticle and Cu target, Cu nanoparticle and Cr target, Cu nanoparticle and CuCr interface target with the impact velocities 5, 8, and 10 km/s are studied, respectively. Furthermore, the various effects associated with the hypervelocity impingement and their significance on vacuum breakdown are also discussed. The results show that the impingement could cause severe plastic deformation and thermal ionization on the impacting materials, deform a crater on the target, and release a cloud of metal vapor and ejection of secondary particles in the vacuum gap and it would lead to the vacuum breakdown. The impact materials and the impact velocities would have significant influence on the impingement phenomena and even on the vacuum breakdown initiated by the impingement.

The role of gas kinematics in setting metallicity gradients at high redshift

ABSTRACT In this work, we explore the diversity of ionized gas kinematics (rotational velocity vϕ and velocity dispersion σg) and gas-phase metallicity gradients at 0.1 ≤ z ≤ 2.5 using a compiled data set of 74 galaxies resolved with ground-based integral field spectroscopy. We find that galaxies with the highest and the lowest σg have preferentially flat metallicity gradients, whereas those with intermediate values of σg show a large scatter in the metallicity gradients. Additionally, steep negative gradients appear almost only in rotation-dominated galaxies (vϕ/σg > 1), whereas most dispersion-dominated galaxies show flat gradients. We use our recently developed analytical model of metallicity gradients to provide a physical explanation for the shape and scatter of these observed trends. In the case of high σg, the inward radial advection of gas dominates over metal production and causes efficient metal mixing, thus giving rise to flat gradients. For low σg, it is the cosmic accretion of metal-poor gas diluting the metallicity that gives rise to flat gradients. Finally, the reason for intermediate σg showing the steepest negative gradients is that both inward radial advection and cosmic accretion are weak as compared to metal production, which leads to the creation of steeper gradients. The larger scatter at intermediate σg may be due in part to preferential ejection of metals in galactic winds, which can decrease the strength of the production term. Our analysis shows how gas kinematics play a critical role in setting metallicity gradients in high-redshift galaxies.

Waveform Optimization of Piezoelectric Micro-Jet for the Control of Metal Micro-Droplet Ejection

On-demand metal droplet ejection is a critical technical branch in industrial electronics. Among them, high temperature and surface tension are the mainly limited factors affecting the single droplet ejection of hot-melt metal. To this end, this article proposed a waveform optimization scheme based on a piezoelectric micro-jet device (PMJD) actuated by a piezoelectric stack and a flexible hinge amplifier for liquid metal. The structure and operation principle of the PMJD is presented and analyzed. The numerical simulation model for hot-melt metal is established; the ejection mechanism and boundary condition of metal droplet are analyzed in detail by a direct fluid-thermal-structure interactions numerical method, which reveals two operation modes of metal droplet ejection under trapezoidal driving waveform. The driving waveform for the PMJD is designed and optimized to allow metal droplets to be ejected, and the variation of the initial velocity and shape of droplets are also analyzed based on the designed waveform. Furthermore, the critical value of satellite droplets generation with fracture of liquid bridge is discussed by simulation, and the optimized waveforms can also be used to suppress satellite droplets.

Failure Analysis of Premature Corrosion of HF Seam-Welded Steel Pipe in Central Heating System

Premature corrosion in the form of longitudinal cracking in a high-frequency (HF) induction seam-welded steel pipe occurred after just 24 months in service. The failed pipe was investigated to reveal the main cause of its failure, and the results of microstructural examinations (light optical microscopy, scanning electron microscopy with energy-dispersive spectrometry) suggest that the failure resulted from an HF induction welding process defect—a so-called cast weld, that is, a huge number of iron oxides in the weld line caused by insufficient ejection of the molten metal from the bond line.

Bioremediation of heavy metals from pharmaceutical industry sewages using bimetallic nanoparticles of Eichorniacrassipes

Biosorption remains one of the most productive and safe technologies that could be received particularly with green algae as biosorbent in the ejection of heavy metals from the effluent. Bimetallic nanoparticles were synthesized from Eichorniacrassipies utilizing the mix of both gold chloride and silver nitrate (3:1). Ultraviolet–visible spectroscopy (UV–vis), Scanning Electron Microscopy (SEM), Infrared Spectroscopy (FTIR) and Infrared Spectroscopy (FTIR) were used in the evaluation of the Nanoparticles. The bimetallic nanoparticles wereutilized as a biosorbent for particular heavy metals (lead, zinc, copper and manganese) present in a pharmaceutical effluent. The nanoparticles were brought into the effluent at various concentrations (1mg, 5mg and 10mg) and time intervals of 24h, 48h and 72h. The decrease in concentration of each metal was determined utilizing Inductively Coupled Plasma Atomic Emission Spectroscopy (ICP-OES). The synthesis of NPs was affirmed by colour change in the blend from light green to lilac after 5min of incubation. The UV-visible spectroscopy adsorption spectrum for bimetallic nanoparticles of E.crassipes (EC-AuAgNPs) was at 398nm while SEM micrograph shown spherical and cube shaped particles with size ranging from 0.31nm- 1.077nm. The FTIR absorbance peaks were available at 3263.93 (O-H), 2107.11 (-C≡C-), 1631.16 (C═C), 1338 (C-N), and 1034.96 cm−1 (C-O). The most extreme rate decrease acquired for each metal was; Copper (67.25%, 10 mg at 72 h); Zinc (61.13%, 1mg at 72 h); Lead (93.37%, 1 mg at 72 h) and Manganese (69.26, 10 mg at 72 h).The biosorption of heavy metals by EC-AuAgNPs was contact time dependent for all the metals and biosorbent concentration dependent for only copper and manganese.

Galactic 26Al traces metal loss through hot chimneys

ABSTRACT Radioactive 26Al is an excellent tracer for metal ejection in the Milky Way, and can provide a direct constraint on the modelling of supernova feedback in galaxy evolution. Gamma-ray observations of the 26Al decay line have found high velocities and hence require a significant fraction of the Galactic 26Al in the hot component. At the same time, meteoritic data combined with simulation results suggest that a significant amount of 26Al makes its way into stars before decay. We investigated the distribution into hot and cold channels with a simulation of a Milky-Way-like galaxy with massive-star feedback in superbubbles and with ejecta traced by 26Al. About 30–40 per cent of the ejecta remain hot, with typical cooling times of the order Gyr. 26Al traces the footpoints of a chimney-fed outflow that mixes metals turbulently into the halo of the model galaxy on a scale of at least 50 kpc. The rest diffuses into cold gas ≲ 104 K, and may therefore be quickly available for star formation. We discuss the robustness of the result by comparison to a simulation with a different global flow pattern. The branching ratio into hot and cold components is comparable to that of longer term average results from chemical evolution modelling of galaxies, clusters, and the intracluster medium.

Damped Ly α absorbers and atomic hydrogen in galaxies: the view of the GAEA model

ABSTRACT Using the GAEA semi-analytic model, we analyse the connection between Damped Ly α systems (DLAs) and H i in galaxies. Our state-of-the-art semi-analytic model is tuned to reproduce the local galaxy H i mass function, and that also reproduces other important galaxy properties, including the galaxy mass–gas metallicity relation. To produce catalogues of simulated DLAs we throw 105 random lines of sight in a composite simulated volume: dark matter haloes with log$(\frac{M_{200}}{ {\rm M}_{\odot }}) \ge 11.5$ are extracted from the Millennium Simulation, while for $9.2 \le \log (\frac{M_{200}}{ \mathrm{M}_{\odot }})\lt 11.5$ we use the Millennium II, and for $8 \le \log (\frac{M_{200}}{\mathrm{M}_{\odot }}) \lt 9.2$ a halo occupation distribution model. At 2 < z < 3, where observational data are more accurate, our fiducial model predicts the correct shape of the column density distribution function, but its normalization falls short of the observations, with the discrepancy increasing at higher redshift. The agreement with observations is significantly improved increasing both the H i masses and the disc radii of model galaxies by a factor of 2, as implemented ‘a posteriori’ in our 2M−2R model. In the redshift range of interest, haloes with $M_{200} \ge {10}^{11} \, \mathrm{M}_{\odot }$ give the major contribution to ΩDLA, and the typical DLA host halo mass is $\sim \!{10}^{11} \, \mathrm{M}_{\odot }$. The simulated DLA metallicity distribution is in relatively good agreement with observations, but our model predicts an excess of DLAs at low metallicities. Our results suggest possible improvements for the adopted modelling of the filtering mass and metal ejection in low-mass haloes.

On thermal axisymmetric liquid-metal divertors

Abstract Motivated by liquid-metal divertor concepts, we consider a detailed model of a thin liquid-metal film flowing down a toroidally-symmetric solid substrate, driven by gravity as well as thermal and mechanical interaction with the SOL. In the relevant physical limit where the film is thin relative to the divertor extent, and the induced magnetic field is weaker than the applied field, the governing equations may be approximated asymptotically to yield tractable reduced-order dynamics. The analysis incorporates gravitational, thermocapillary and thermoelectric forces, and reveals several nontrivial findings. Firstly, we find that the influence on the liquid metal flow of the toroidal component of the applied field is negligible compared to that of the poloidal component. This has important ramifications for the behaviour of the liquid metal. Secondly, we identify a “spiral-type flow” due to a flow component in the toroidal direction. This flow has been previously reported in the literature in the isothermal case when using extreme parameters. Our analysis explains why these extreme parameter choices were required to observe the isothermal flow, and reveals that, for typical parameters in the thermal case, the flow becomes significant due to thermoelectric forces. Thirdly, we deduce full dimensional velocity scalings. Finally, we present a case study that employs the reduced-order model to explore the effects of sweeping the plasma strike point up and down the divertor. We simulate fully transient dynamics within the divertor and demonstrate how, in some regions of parameter space, the sweeping might promote dry-out or droplet ejection of the liquid metal. We discuss how the case study can inform both divertor material choice as well as tokamak operating parameters.

A Model of a Source of Shock Wave Metal Ejection Based on Richtmyer-Meshkov Instability Theory

A Model of a Source of Shock Wave Metal Ejection Based on Richtmyer-Meshkov Instability Theory

Spatially Resolved Metal Loss from M31

Abstract As galaxies evolve, they must enrich and exchange gas with the surrounding medium, but the timing of these processes and how much gas is involved remain poorly understood. In this work, we leverage metals as tracers of past gas flows to constrain the history of metal ejection and redistribution in M31. This roughly L* galaxy is a unique case where spatially resolved measurements of the gas-phase and stellar metallicity, dust extinction, and neutral interstellar gas content are all available, enabling a census of the current metal mass. We combine spatially resolved star formation histories from the Panchromatic Hubble Andromeda Treasury survey with a metal production model to calculate the history of metal production in M31. We find that 1.8 × 109 M ⊙ of metals, or 62% of the metal mass formed within r < 19 kpc, is missing from the disk in our fiducial model, implying that the M31 disk has experienced significant gaseous outflows over its lifetime. Under a conservative range of model assumptions, we find that between 3% and 88% of metals have been lost (1.9 × 107–6.4 × 109 M ⊙), which means that metals are missing even when all model parameters are chosen to favor metal retention. We show that the missing metal mass could be harbored in the circumgalactic medium of M31 if the majority of the metals reside in a hot gas phase. Finally, we find that some metal mass produced in the past 1.5 Gyr in the central ∼5 kpc has likely been redistributed to larger radii within the disk.

Spectroscopy of Supergiants with Infrared Excess: Results of 1998–2018

The results of our second stage (1998-2018) of the detailed spectroscopy of peculiar supergiants identified with galactic infrared sources, performed mainly at the 6-meter BTA telescope are summarized. The main aspect of the program is a search for the evolutionary variations in the chemical composition of stars, past the AGB stage and the TDU, as well as an analysis of spectral manifestations of kinematic processes in their extended, often unstable, atmospheres and in the envelopes. The most significant result is detection of the s-process element excesses in seven single post-AGB stars, which confirms the theory of evolution of this type of stars. In three of these stars we for the first time discovered the ejection of the s-process heavy metals to the circumstellar envelopes. A lithium excess was found in the atmospheres of two peculiar supergiants V2324 Cyg and V4334 Sgr. The results of investigation of the kinematical state of atmospheres and envelopes will clarify the equilibrium of matter produced by stars in the AGB and post-AGB stages and delivered to the interstellar medium.

Observation of ejecta tin particles into polymer foam through high-energy X-ray radiograpy using high-intensity short-pulse laser

Micron-scale fragment ejection of metal is a kind of surface dynamic fragmentation phenomenon upon shock loading. The study of ejecta is crucial in many fields, such as inertial confinement fusion and pyrotechnics. Due to the particular advantages of laser experiments, a lot of studies of ejecta by strong laser-induced shock loading have been conducted in recent years. The shapes, size and mass of particle can be obtained via static soft recovery technique with foam. However, the stagnation and succedent mixing of the ejecta in the foam could not be deduced by this technique. To study the mixing between the ejecta and foam, a radiography experiment is performed by using the X-ray generated through the irradiation of picosecond laser on the golden wire. This radiography technique has not only high spatial resolution but also high temporal resolution. Two kind of experiments are designed and performed. In the first one, the tin sample and the foam are close to each other while a vacuum gap is arranged between them in the other one. The mixing process is analyzed with the determined areal density and volume density, as well as the results of recovery. The areal density of the front mixing area is similar to the scenario in the case with a vacuum gap, suggesting that the ejecta have not underwent a secondary fragmentation due to the collision with foam. Furthermore, the static recovery results show a different characteristic of penetration depth for the ejecta in the foam. When the tin sample is not close to the foam, the penetration depth in the foam increases with the loading pressure increasing. However, the penetration depth begins to decrease at a critical pressure after a brief increase, which is attributed to the interaction between the shock and the foam before the ejecta coming, and also to the ejecta size and composition. The shock pressure is high enough to change the foam performance, thus enhancing the stagnation ability for ejecta penetration. Moreover, the size and composition vary with loading pressure, thereby leading to the momentum change of the ejecta related to the penetration depth. In the future work, we will improve the field of view of the X-ray radiography to achieve a direct comparison between the dynamic results and the recovery results. Moreover, we will arrange perturbations at the interface to study the mixing between the micro-jetting and the foam and the interface instability.