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Flame–wall interaction (FWI) of lean premixed hydrogen/air flames is critical in wall-bounded combustors, where thermodiffusive instabilities strongly influence quenching. To capture these effects efficiently in realistic configurations, reduced-order combustion models such as flamelet tabulation are desirable, as they lower resolution requirements and computational cost. In this study, advanced flamelet manifolds incorporating a mixture-averaged species diffusion model and thermal diffusion are developed to represent the FWI of thermodiffusively unstable lean hydrogen/air flames. A central challenge is the simultaneous capture of intrinsic instabilities and heat losses, each complex in itself. Separate manifolds addressing these effects are first introduced, providing the foundation for joint manifolds that capture both simultaneously. In this context, the choice of flamelet databases is examined by comparing freely propagating flames with exhaust gas recirculation, commonly used in flamelet modelling to represent enthalpy variations, with one-dimensional head-on quenching (HOQ) flames, which are essential for accurate prediction of wall heat flux and pollutant formation in hydrocarbon flames. The models are evaluated through both a-priori and a-posteriori analyses across increasingly complex configurations, culminating in the HOQ of a thermodiffusively unstable flame, where both instability and quenching must be captured simultaneously. Results show excellent agreement with reference simulations using detailed chemistry, accurately reproducing key features of the flame front, thermochemical state and global flame properties such as consumption speed and quenching wall heat flux. This marks a key advance in modelling hydrogen combustion and provides a robust foundation for studying safety-critical phenomena such as flame flashback linked to near-wall flame propagation.
This chapter discusses how a classical universe arises out of the quantum wave function of the universe. The process of decoherence is described, first in general and then applied to cosmology. The classicalization of the background spacetime (and the associated reduction in interference between saddle points) as well as the classicalization of long-wavelength perturbation modes is discussed, by studying an example of interactions between background and fluctuations, as well as interaction between perturbation modes of different wavelengths. Comments on the interpretation of the wave function are included.
Reconstructing near-wall turbulence from wall-based measurements is a critical yet inherently ill-posed problem in wall-bounded flows, where limited sensing and spatially heterogeneous flow–wall coupling challenge deterministic estimation strategies. To address this, we introduce a novel generative modelling framework based on conditional flow matching for synthesising instantaneous velocity fluctuation fields from wall observations, with explicit quantification of predictive uncertainty. Our method integrates continuous-time flow matching with a probabilistic forward operator trained using stochastic weight-averaging Gaussian, enabling zero-shot conditional generation without model re-training. We demonstrate that the proposed approach not only recovers physically realistic, statistically consistent turbulence structures across the near-wall region but also effectively adapts to various sensor configurations, including sparse, incomplete and low-resolution wall measurements. The model achieves robust uncertainty-aware reconstruction, preserving flow intermittency and structure even under significantly degraded observability. Compared with classical linear stochastic estimation and deterministic convolutional neural network methods, our stochastic generative learning framework exhibits superior generalisation for unseen realisations under same flow conditions and resilience under measurement sparsity with quantified uncertainty. This work establishes a robust semi-supervised generative modelling paradigm for data-consistent flow reconstruction and lays the foundation for uncertainty-aware, sensor-driven modelling of wall-bounded turbulence.
In this study, experimental deep reinforcement learning (DRL) control of a supersonic cavity flow is conducted for the first time at Mach 2, with the aim of mixing enhancement. A 4 $\times$ 5 pulsed-arc plasma actuator (PAPA) matrix with independently controlled columns and a supersonic hot-wire probe placed at the cavity midline serve as the flow disturber and state observer, respectively. The control law parametrised by a radial basis function network is executed on a field-programmable gate array at 5 kHz loop frequency. Results show that DRL is capable of finding a converged closed-loop control law in less than 10 s, and the resulting cavity velocity fluctuation is three times higher than periodic open-loop control. The control benefits earned by DRL increase with the number of activated columns, yet reduce with the cavity back-wall inclination angle. Using the same number of actuator columns, variable-formation actuation mode allows the DRL to find a more effective control with much less actuator power consumption, when compared with fixed-formation actuation mode. The final control law obtained by DRL can be interpreted as a threshold control conditional on the location of the state vector, and the improvement of total reward is ascribed to both the elevation of occurrence probabilities of high-reward clusters and the ubiquitous increase of the reward expectation at each cluster. Physically, mixing enhancement in the cavity flow is traced back to the thermal bulbs and shock waves produced by the PAPA, which induce a meandering motion of the shear layer.
This chapter starts with a description of quantum tunneling as a process taking place in imaginary or even complex time. This physical picture can be extended to include gravity, which leads to a description of Coleman–DeLuccia instantons and the nucleation of bubble universes. The mathematical analysis is complemented by a derivation of negative modes, which puts the tunneling process on a firm theoretical footing. Very similar methods can also describe the decay of spacetime via bubbles of nothing. A semiclassical view of spacetime may also lead to the existence of wormholes, of both the Lorentzian and the Euclidean variety. Their properties as well as associated puzzles are discussed in detail.
Provides a review of how the standard model of cosmology is built up, emphasizing the interplay between theory and observations. The Robertson–Walker line element is derived and used to find the Friedmann equations. Elementary solutions are discussed. In this way the hot big bang model emerges. Its implications are discussed, especially the thermal history of the universe and the existence of the cosmic microwave background radiation. The chapter concludes with a discussion of the main puzzles of the hot big bang model.
How can one describe the appearance of space and time? This chapter reviews the no-boundary proposal, which allows for a concrete calculation of the nucleation of space and time from nothing. After providing heuristic motivations for this idea, concrete examples are presented, and the stability of solutions as well as the numerical methods required to find generic solutions are discussed. A general prescription for characterizing no-boundary instantons is developed, before examining explicit minisuperspace models. A special emphasis is put on the appropriate boundary conditions, both in the path integral formalism and in the Wheeler–DeWitt equation. The robustness of solutions upon the inclusion of expected quantum gravity corrections is discussed, as well as the question of which kinds of complex metrics should be allowed. This leads to a discussion of both postdictions and predictions of the proposal.
A variational principle for gravity, based on the Einstein–Hilbert action, is presented and augmented with a discussion of surface terms and boundary conditions. The ADM or Hamiltonian formalism is introduced, and gravity is rewritten in a (1+3)-dimensional decomposition. The theory is canonically quantized, which leads to the Wheeler–DeWitt equation. The properties of this equation are discussed, as well as those of JWKB semiclassical solutions. In this way it is shown how time is recovered in a semiclassical setting.
A link between horizons, imaginary time, and temperature is developed at the heuristic level first, before being made precise in the following sections with the use of Bogolyubov transformations. This leads to the derivation of the Unruh effect, which shows that an accelerated observer experiences a temperature. Analogous methods allow one to derive the phenomenon of Hawking radiation by which black holes can evaporate, and an explicit calculation of the closely related Hawking–Page transition is provided via path integral methods in which the background spacetime is also quantized. It is further shown that due to the existence of a horizon, one may in the same way associate a temperature with de Sitter spacetime. An explicit discussion of de Sitter mode functions is included, because it relates directly to the quantization of inflationary fluctuations.
After an overview of the observed properties of the cosmic microwave background, we turn to attempts at their explanation. First it is shown that classical statistical fluctuations are not suitable for explaining the primordial perturbations inferred from the temperature fluctuations in the CMB. Then it is shown how to quantize inflationary perturbations, after taking care of diffeomorphism invariance. Exact constant-equation-of-state and approximate slow-roll solutions are derived, both for scalar and tensor fluctuations, and shown to potentially be in accord with observations, if the inflationary model is chosen suitably. A brief discussion of the transition from quantum to effectively classical fluctuations is also included. The chapter concludes with a discussion of the open questions related to inflation.
In the final chapter, the basics of string cosmology are introduced. After a lightning review of string theory, the potential existence of extra dimensions is discussed in some detail. A special emphasis is put on the possible observational signatures of towers of massive Kaluza–Klein modes due to their effects during inflation and in the early universe in general. Then branes are presented as solutions to low-energy approximations to string theory. The difficulties with constructing models of brane inflation are illustrated with a specific example. Finally, a collision of end-of-the-world branes as a model of the big bang is analyzed.
Direct numerical simulation (DNS) of temporally developing natural convection boundary layers is conducted at $ \textit{Pr} =4.16$ and $ \textit{Pr} =6$. Results are compared with an existing DNS dataset for $ \textit{Pr} =0.71$ (Ke et al. J. Fluid Mech. 964, 2023, p. A24) to enable a direct assessment of Prandtl number effects across the range $0.71\leqslant \textit{Pr} \leqslant 6$. The analysis reveals that the $ \textit{Pr}$ affects the flow through buoyancy forcing, which acts not only as the driving force but also modulates the local shear distribution via coupling with the momentum equation, thereby shifting the onset Rayleigh number of transition from the laminar regime. This transition is found to be characterised by the thermal boundary layer thickness $\delta _\theta$, which provides a robust prediction of the critical Rayleigh number across $ \textit{Pr}$, indicating a buoyancy instability consistent with the stability analysis (Ke et al. J. Fluid Mech. 988, 2024, p. A44; Ke et al. Intl J. Heat Mass Transfer 241, 2025, p. 126670). Further analysis in the turbulent regime suggests that while heat transfer becomes effectively independent of $ \textit{Pr}$, the near-wall turbulence structure remains sensitive to $ \textit{Pr}$ due to persistent buoyancy effects. The skin friction coefficient scaling shows clear transition from a linear scaling with the bulk Reynolds number in the weakly turbulent regime to a log-law-type scaling with the bulk Reynolds number in the ultimate turbulent regime (Grossmann & Lohse J. Fluid Mech. 407, 2000, pp. 27–56). The premultiplied velocity spectra confirms the development of near-wall streaks that are characteristic of canonical shear-driven turbulence in this ultimate turbulent regime, with their spanwise spacing systematically broadening with increasing $ \textit{Pr}$ due to persistent buoyancy effects; while the spectral signature of the outer plume-like region appears largely $ \textit{Pr}$-independent.