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Six types of shock wave interference resulting from the impingement of an incident shock on a bow shock are revisited by examining the sub-types that arise between the canonical types. Several new sub-types are predicted based on the theories of weak shock reflection and double-wedge shock interference, and verified via numerical simulations. Two additional types, Type IIw and Type IIs, are identified between Type II and Type III, whereas a Type Vw emerges between Type IV and Type V. These types originate from the transformation of the Mach reflection at the triple point, which evolves through weak shock reflections (von Neumann reflection, Vasilev reflection, Guderley reflection) before disappearing. The transition from Type III to Type IV is further shown to mirror sequences of double-wedge shock interference. Two additional types (Type IIIb and Type IVt) are found. Meanwhile, it is found that under large incoming flow Mach number ($M_0$ = 5), Types III, IV and their sub-types dominate, whereas Type II is absent; under small incoming flow Mach number ($M_0$ = 2.5), Types III and IV vanish and a modified Type Va emerges. This study adds seven new sub-types to the existing six types of shock interference. These work extend the classical six types of shock interferences into six-plus shock interference, a picture that shed new insight into shock interference.
Recently, Alfvénic ion temperature gradient (AITG) modes have been observed in the core plasma on the HL-2A tokamak. Only when electron cyclotron resonance heating (ECRH) and neutral beam injection are simultaneously injected into the deuterium plasma do the AITG modes become unstable. The instability is electromagnetic and localised in the core plasma with an internal transport barrier. Dynamic evolution of AITG modes is greatly affected by the off-axis ECRH. Theoretical analysis suggests that there is a strong dependence of the AITG modes on $\eta _i\simeq \boldsymbol{\nabla }\ln T_i/\boldsymbol{\nabla }\ln n_i$, where $n_i$ is the ion density. It is also found that ECRH can enhances AITG modes by causing a drop of electron density and an increase of $\tau =T_e/T_i$; here $T_e$ and $T_i$ are the electron and ion temperatures, respectively. Besides, high-power ECRH may also change the safety factor or magnetic shear and then contribute to the mitigation of AITG modes. The new findings can not only enrich scientific knowledge for pressure gradient-driven instability, but also be beneficial to active control of core-localised electromagnetic modes in future fusion devices.
The linear stability of nanofluid boundary-layer flow over a flat plate is investigated using a two-phase formulation that incorporates the Brinkman (1952 J. Chem. Phys., vol. 20, pp. 571–581) model for viscosity along with Brownian motion (BM) and thermophoresis (TP), building upon the earlier work of Buongiorno (2006 J. Heat Transfer, vol. 128, pp. 240–250). Solutions to the steady boundary-layer equations reveal a thin nanoparticle concentration layer near the plate surface, with a characteristic thickness of $O({\textit{Re}}^{-1/2}{\textit{Sc}}^{-1/3})$, for a Reynolds number ${\textit{Re}}$ and Schmidt number ${\textit{Sc}}$. When BM and TP are neglected, the governing equations reduce to the standard Blasius formulation for a single-phase fluid, and the nanoparticle concentration layer disappears, resulting in a uniform concentration across the boundary layer. Neutral stability curves and critical conditions for the onset of the Tollmien–Schlichting (TS) wave are computed for a range of nanoparticle materials and volume concentrations. Results indicate that while the effects of BM and TP are negligible, the impact of nanoparticle density is significant. Denser nanoparticles, such as silver and copper, destabilise the TS wave, whereas lighter nanoparticles, like aluminium and silicon, establish a small stabilising effect. Additionally, the viscosity model plays a crucial role, with alternative formulations leading to different stability behaviour. Finally, a high Reynolds number asymptotic analysis is undertaken for the lower branch of the neutral stability curve.
Runaway electrons (REs), generated during plasma disruptions in tokamaks, pose significant challenges due to the risk of causing damage to the first wall of a device. Understanding the interaction between REs and magnetohydrodynamic (MHD) instabilities is crucial for predicting a safe operation of large future tokamak devices in which RE generation will be drastically enhanced due to the high plasma current. In this work, we introduce a hybrid fluid–kinetic model within the three-dimensional nonlinear MHD code JOREK (Hoelzl et al. 2021 Nucl. Fusion, vol. 61, 065001; 2024 Nucl. Fusion, vol. 64, 112016), treating REs kinetically using a relativistic guiding-centre approach, while describing the background plasma by ansatz-based reduced MHD equations. At first, comprehensive benchmark studies are conducted regarding the two-dimensional equilibrium force balance with $J_{total}= J_{RE}$, and the linear stability of three-dimensional tearing modes (TMs), verifying the accuracy of the model against analytical predictions and other numerical methods, e.g. the full-orbit approach in JOREK and the fluid model in M3D-C1. These benchmark studies build a solid foundation for applying our model to more complex nonlinear scenarios. In this respect, we confirm that the nonlinear saturation of TMs is significantly influenced by the presence of REs. Previous analytical studies (Helander et al. 2007 Phys. Plasmas vol. 14, 122102) suggest that in the case of small $\varDelta ^\prime$, the saturation width of the magnetic island driven by REs is roughly 1.5 times larger than in the otherwise identical Ohmic current scenario. Our simulations are quantitatively in line with this prediction. Moreover, REs alter the energy evolution within the magnetic reconnection process and decouple the bulk plasma and magnetic fields. In summary, RE-driven magnetic reconnection leads to larger magnetic islands but weaker reconnection flows.
We present a mathematical model for tsunami and induced magnetic anomalies originating from a time-dependent seabed deformation in an otherwise quiescent ocean over a conductive seafloor. The deformation is assumed to be a slender fault, whose lateral extension is much larger than the longitudinal scale. Using a perturbative method with multiple time scales and Green’s function approach, we examine the slow evolution of the wave field and induced magnetic anomaly over transoceanic distances from the fault. The model is validated against deep-ocean observations from the 2011 Tōhoku-oki tsunami. Our study reveals that lateral propagation in two horizontal dimensions decreases the period of both the surface wave and induced magnetic signal compared with one-horizontal-dimension scenarios. Over time, initially longitudinal wave propagation alters as wave fronts bend and stretch, affecting the magnetic signal accordingly. Interestingly, the magnetic anomaly gradually separates from the leading tsunami wave and travels ahead of the tsunami by a distance proportional to the fault’s longitudinal scale. We show that increased lateral propagation reduces the detectability of magnetic anomalies. Finally, we derive an asymptotic formula valid for the long leading wave that travels ahead of the dispersive group over transoceanic distances. This formula holds promise for the rapid assessment of tsunami risk. These findings advance fundamental understanding and may inform the development of future tsunami early warning systems relying on magnetic field detection.
We study transverse profiles and time fluctuations of turbulence dissipation rate, turbulence kinetic energy and integral length scales by means of high-speed stereoscopic particle image velocimetry in the turbulent wake of a 6 : 1 prolate spheroid that has its principal axis aligned with the incoming non-turbulent flow. This turbulent wake of a slender body differs from turbulent bluff body wakes in terms of transverse non-homogeneity of turbulence dissipation rate and because it is not axisymmetric even though it nominally is. Even so, both transverse profiles and time fluctuations of turbulence dissipation rate coefficients (inverse ratio between the rate with which the large scales lose energy and the rate with which the small scales dissipate energy) and of the Taylor length-based Reynolds number (ratio between the turbulent kinetic energy mostly in the large scales and the turbulent kinetic energy at the smallest scales) obey self-regulating non-equilibrium, as previously found in various other turbulent flows. However, the power law relating the transverse variations and the time fluctuations of these two ratios differs from previously reported self-regulating non-equilibrium power law scalings in other turbulent flows.
The coupling between Rayleigh–Taylor (R–T) and Saffman–Taylor (S–T) instabilities, when a gas displaces a high-viscosity liquid, remains challenging to elucidate due to the unclear roles of density and viscosity contrasts. Counterintuitively, our radial Hele-Shaw cell experiments revealed that viscosity contrast – typically considered a damping factor – serves as the primary driver of instability. We observed that the glycerin–air interface, despite its higher viscosity, exhibits significantly greater instability than the water–air interface. This anomalous behaviour arises from the S–T mechanism, which accelerates the onset of nonlinearity and induces an early transition to fingering. We applied a unified model to decouple the competing influences of surface tension oscillation and viscous damping on R–T instability and the S–T destabilisation. Moreover, we proposed criteria for either mostly enhancing or completely freezing the instability. These findings offer valuable insights into manipulating hydrodynamic instabilities in contracting/expanding geometries through surface tension and viscosity.
High-intensity focused ultrasound (HIFU) is a non-invasive alternative to traditional surgery for detection and treatment. When HIFU targets a specific area, ultrasonic cavitation occurs with mechanical stress, causing tissue damage, a process that is significantly influenced by the surroundings. This paper presents a numerical study on the cavitation initiation and evolution mechanisms under focused ultrasonic waves considering the influence of a solid surface. Firstly, the dynamic property of focused ultrasonic waves and the generation of diffraction waves is explained based on the Huygens–Fresnel principle, and the prefocused phenomenon is analysed. Notably, the scenario considering the existence of a solid wall is discussed, with the corresponding cavitation clouds in a ‘tree-like’ pattern that can be generally divided into three or four subregions. The different initiation mechanisms of the near-wall cavitation clouds under a different relative distance between the theoretical focal point and the solid wall are discussed in detail. Finally, by considering the effects of the incident waves, scattered waves and their reflected waves on the solid wall, a wave superposition model is established that can clearly explain the distribution characteristics of the near-wall cavitation clouds with different modes. The understanding of the ultrasonic cavitation mechanism may support precise control in future HIFU applications.
This paper presents the first experimental measurement of the Prandtl–Meyer function in the non-ideal compressible flow regime. Planar contoured nozzle profiles expand the flow to the supersonic regime, providing a uniform parallel flow of siloxane MM (hexamethyldisiloxane, $\textrm{C}_{6}\textrm{H}_{18}\textrm{OSi}_{2}$). Prandtl–Meyer expansions are then generated at sharp convex corners, for discrete flow deflection angles from 5$^\circ$ to 30$^\circ$. Stagnation pressures and temperatures are measured in the settling chamber, immediately upstream of the test section, to estimate the level of non-ideality of the investigated flows, ranging from mild non-ideal conditions to dilute ideal-gas states. Non-ideal thermodynamic effects through the expansions are characterised by means of independent measurements of Mach number by schlieren visualisations, and static pressure. Experimental comparisons across different thermodynamic states confirm the role of the compressibility factor evaluated at total conditions as a similarity parameter for moderately high non-ideal flows. To extract values of the Prandtl–Meyer function from the measurements, a simplified analytical model for the Prandtl–Meyer function dependency on the Mach number is formulated. The recovered values agree with Prandtl–Meyer theory, complemented with state-of-the-art thermodynamic models, for all the examined operating conditions.
Cluster environments influence galaxy evolution by curtailing star formation activity, notably through ram-pressure stripping (RPS). This process can leave observable signatures—such as gas tails and truncated gas disks—that are crucial for understanding how RPS affects galaxies. In this study, using spatially resolved spectroscopic data from the SAMI Galaxy Survey, we identify galaxies undergoing or recently affected by RPS in eight nearby clusters (0.029 < z < 0.058), through a visual classification scheme based on the ionised gas (Hα +[NII]λ6584) morphologies, split into “unperturbed”, “asymmetric”, and “truncated”. Alongside, we measure non-parametric structural parameters (concentration, asymmetry, and offset between gas and stars) to quantify the ionised gas morphologies. We find that combinations of parameters such as concentration, shape asymmetry, and stellar–ionised gas centre offsets are useful in categorising the degree of RPS in line with their ionised gas morphologies. The projected phase-space analysis shows that asymmetric galaxies are found in a narrow region in cluster-centric distance (0.1 < R/R200 < 0.6, where R200 is the characteristic cluster radius) and have a larger dispersion in line-of-sight velocity (, with σ200 being the cluster velocity dispersion within R200), compared to the truncated and unperturbed samples that are more broadly distributed and predominantly located at larger cluster-centric distances. This suggests that asymmetric galaxies are likely recent infallers—having crossed within 0.5 R200 in the past ∼1 Gyr. In terms of star formation activity, we find that the resolved star-forming main sequence (rSFMS; ΣSFR –Σ*) of unperturbed and RPS candidates (asymmetric and truncated) differ. RPS candidates yield a much steeper rSFMS relation compared to the unperturbed counterparts, primarily emerging from having lower ΣSFR values for the low mass density regime (i.e., log Σ* ≲ 8 M⊙ kpc–2), with the steepest gradient deriving from the truncated sample. Moreover, radial specific star formation rate profiles introduce different trends for unperturbed and RPS candidates. Star formation in RPS candidates is suppressed in the outskirts relative to unperturbed galaxies and is more prominent for the truncated sample compared to the asymmetric counterparts. In contrast, central (i.e., r/reff < 0.5) star formation activity in RPS candidates is comparable with that in their unperturbed and field counterparts, suggesting no elevated activity. Taken together, this suggests an evolutionary trend linked to the RPS stage, where unperturbed galaxies likely represent recently accreted systems (pre-RPS), while asymmetric and truncated galaxies may correspond to populations undergoing RPS and post-RPS phases, respectively, favouring outside-in quenching.
Double white dwarf (DWD) binaries are natural outcomes of binary stellar evolution and key sources for future space-based gravitational wave (GW) observatories such as Laser Interferometer Space Antenna (LISA). We investigate how different binary interaction channels shape the physical and orbital properties of DWD systems, focusing on component masses, orbital separations, core compositions, and mass transfer rates. Using the binary population synthesis code COMPAS, we evolve 107 binaries with physically motivated initial distributions of binary parameters. Our simulations reproduce the strong bimodality in the final orbital separations, including a pronounced deficit of systems around 100−500 R⊙, arising from distinct evolutionary pathways: wide DWDs predominantly originate from stable Roche lobe overflow (RLOF), while close DWDs form through unstable RLOF leading to at least one common envelope (CE) phase. Moreover, we show that the core compositions of WDs provide a powerful tracer of evolutionary history: He-core WDs are strongly concentrated in close systems, whereas CO-core WDs span the full separation range and exhibit a small mass gap in wide binaries. We further identify a correlation between the accreted mass and the final orbital separation, highlighting the impact of non-conservative mass transfer on the resulting orbital configuration of DWD systems. These results underscore the links among evolutionary channels, chemical composition, and mass transfer rates; thereby provide a unique framework for interpreting Gaia DWD samples and forecasting the joint electromagnetic and GW population accessible to LISA.
The effect of a smooth surface hump on laminar–turbulent transition over a swept wing is investigated using direct numerical simulation (DNS), and results are compared with wind tunnel measurements. When the amplitude of incoming crossflow (CF) perturbation is relatively low, transition in the reference (without hump) case occurs near $53\,\%$ chord, triggered by the breakdown of type I secondary instability. Under the same conditions, no transition is observed in the hump case within the DNS domain, which extends to $69\,\%$ chord. The analysis reveals a reversal in the CF velocity component downstream of the hump’s apex. Within this region, the structure and orientation of CF perturbations are linearly altered, particularly near the wall. These perturbations gradually recover their original state further downstream. During this recovery phase, the lift-up mechanism is weakened, reducing linear production, which stabilises the stationary CF perturbations and weakens spanwise gradients. Consequently, the neutral point of high-frequency secondary CF instability modes shifts downstream relative to the reference case, leading to laminar–turbulent transition delay in the presence of the surface hump. In contrast, when the amplitude of the incoming CF perturbation is relatively high, a pair of stationary counter-rotating vortices forms downstream of the hump. These vortices locally deform the boundary layer and generate regions of elevated spanwise shear. The growth of secondary instabilities in these high-shear regions leads to a rapid advancement of transition towards the hump, in agreement with experimental observations.
Neutral atoms recycled from wall interaction interact with confined plasma, thereby refuelling it, most strongly in the region closest to the wall. This occurs near the X-point in diverted configurations, or else near the wall itself in limited configurations. A progression of analytic models is developed for neutral density in the vicinity of a planar or linear source in an ionising domain. First-principles neutral transport simulations with DEGAS2 are used throughout to test the validity and limits of the model when using equivalent sources. The model is further generalised for strong plasma gradients or the inclusion of charge exchange. An important part of the problem of neutral fuelling from recycling is thereby isolated and solved with a closed-form analytic model. A key finding is that charge exchange with the confined plasma can be significantly simplified with a reasonable sacrifice of accuracy by treating it as a loss. The several assumptions inherent to the model (and the simulations with which it is compared) can be adapted according to the particular behaviour of neutrals in the divertor and the manner in which they cross the separatrix.
Understanding the connection between active galactic nuclei and star-formation (the AGN-SF connection) is one of the longest standing problems in modern astrophysics. In the age of large integral field unit (IFU) surveys, studies of the AGN-SF connection greatly benefit from spatially resolving AGN and SF contributions to study the two processes independently. Using IFU data for 54 local active galaxies from the S7 sample, we present a new method to separate emission from AGN activity and SF using mixing sequences observed in the [NII]$\unicode{x03BB}$6 584 Å/${\mathrm{H}}\unicode{x03B1}$ vs. [OIII]$\unicode{x03BB}$5 007 Å/${\mathrm{H}}\unicode{x03B2}$ Baldwin–Phillips–Terlevich diagram. We use the new decomposition method to calculate the ${\mathrm{H}}\unicode{x03B1}$ star-formation rate and AGN [OIII] luminosity for the galaxies. Our new method is robust to outliers in the line ratio distribution and can be applied to large galaxy samples with little manual intervention. We infer star-formation histories using pPXF, conducting detailed recovery tests to determine the quantities that can be considered robust. We test the correlation between the AGN Eddington ratio, using the proxy $L\mathrm{[O{III}]}/\sigma_*^4$, and star-formation properties. We find a moderately strong correlation between the Eddington ratio and the star-formation rate. We also observe marginally significant correlations between the AGN Eddington ratio and the light-weighted stellar age under 100 Myr. Our results point to higher AGN accretion being associated with young nuclear star-formation under 100 Myr, consistent with timelines presented in previous studies. The correlations found in this paper are relatively weak; extending our methods to larger samples, including radio-quiet galaxies, will help better constrain the physical mechanisms and timescales of the AGN–SF connection.
Quantum many-body systems are a central feature of condensed matter physics, relevant to important, modern research areas such as ultrafast light-matter interactions and quantum information. This book offers detailed coverage of the contour Green's function formalism – an approach that can be successfully applied to solve the quantum many-body and time-dependent problems present within such systems. Divided into three parts, the text provides a structured overview of the relevant theoretical and practical tools, with specific focus on the Schwinger-Keldysh formalism. Part I introduces the mathematical frameworks that make use of Green's functions in normal phase states. Part II covers fermionic superfluid phases with discussion of topics such as the BCS-BEC crossover and superconducting systems. Part III deals with the application of the Schwinger-Keldysh formalism to various topics of experimental interest. Graduate students and researchers will benefit from the book's comprehensive treatment of the subject matter and its novel arrangement of topics.
We investigate the occurrence of flow circulation in an open triangular cavity filled with a gas at highly rarefied conditions. The cavity is subject to an external shear flow that is in either the circular or linear direction at its inlet. The problem is studied analytically in the free-molecular limit and numerically based on the direct simulation Monte Carlo (DSMC) method. The corner walls are modelled based on the Maxwell boundary condition, as either specular or diffuse. The results are obtained for arbitrary values of the outer flow speed and corner angle. Remarkably, it is found that multiple recirculation zones occupy the corner domain in the absence of molecular interactions. In the specular-corner set-up, such topologies occur at non-large outer-flow speeds and distinct corner-angle intervals of $[\pi /(n+1),\pi /n]$ with $n=3,5,\ldots$. In the diffuse-wall case, the cavity flow field contains two recirculation zones at sufficiently low corner angles for both circular and straight outer flows. With increasing angles, the straight-flow configuration differs, reducing the number of vortices to one and then none. The results are rationalised based on ballistic particle kinematics, suggesting insight into the relation between the microscopic description and the hydrodynamic (observed) generation of circulation. The effects of molecular collisions on the corner flow pattern, as well as more elaborate gas-surface interaction models, are inspected based on DSMC calculations, indicating visible impacts on the macroscopic flow structure at large Knudsen numbers.
The hydrodynamic performance of oscillating elastic plates with tapered and uniform thickness in an incompressible Newtonian fluid at varying Reynolds numbers is investigated numerically using a fully coupled fluid–structure interaction computational model. By leveraging the acoustic black hole effect, tapered plates can generate bending patterns that vary from standing wave to travelling wave oscillations, whereas plates with uniform thickness are limited to standing wave oscillations. Simulations reveal that although both standing and traveling wave oscillation modes can produce high thrust, travelling waves achieve significantly higher hydrodynamic efficiency, and this advantage is more pronounced at higher Reynolds numbers. Furthermore, regardless of the oscillation mode, tapering leads to greater hydrodynamic performance. The enhanced hydrodynamic efficiency of travelling wave propulsion is associated with the reduced amount of vorticity generated by tapered plates, while maintaining high tip displacements. The results have implications for the development of highly efficient biomimetic robotic swimmers, and more generally, the better understanding of the undulatory aquatic locomotion.