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This text on general relativity and its modern applications is suitable for an intensive one-semester course on general relativity, at the level of a PhD student in physics. Assuming knowledge of classical mechanics and electromagnetism at an advanced undergraduate level, basic concepts are introduced quickly, with greater emphasis on their applications. Standard topics are covered, such as the Schwarzschild solution, classical tests of general relativity, gravitational waves, Arnowitt, Deser, Misner parametrization, relativistic stars, and cosmology, as well as more advanced standard topics such as vielbein–spin connection formulation, trapped surfaces, the Raychaudhuri equation, energy conditions, the Petrov and Bianchi classifications, and gravitational instantons. More modern topics, including black hole thermodynamics, gravitational entropy, effective field theory for gravity, the parametrized post- Newtonian expansion, the double copy, and fluid-gravity correspondence are also introduced using the language understood by physicists, without mathematics that is too abstract mathematics, proven theorems, or the language of pure mathematics.
Recent experiments aiming to measure phenomena predicted by strong-field quantum electrodynamics (SFQED) have done so by colliding relativistic electron beams and high-power lasers. In such experiments, measurements of collision parameters are not always feasible. However, precise knowledge of these parameters is required to accurately test SFQED.
Here, we present a novel Bayesian inference procedure that infers collision parameters that could not be measured on-shot. This procedure is applicable to all-optical non-linear Compton scattering experiments investigating radiation reaction. The framework allows multiple diagnostics to be combined self-consistently and facilitates the inclusion of known information pertaining to the collision parameters. Using this Bayesian analysis, the relative validity of the classical, quantum-continuous and quantum-stochastic models of radiation reaction was compared for several test cases, which demonstrates the accuracy and model selection capability of the framework and highlight its robustness if the experimental values of fixed parameters differ from their values in the models.
We consider relativistic stars and find the equations of gravitational collapse. In particular, we write the Tolman–Oppenheimer–Volkov (TOV) equation. We define general stellar models. We find the Chandrasekhar limit for white dwarfs to break electron degeneracy pressure and collapse to a neutron start, and the TOV limit for neutron stars to break neutron degeneracy pressure and collapse to a black hole. Finally, we describe a simple model (Oppenheimer–Snyder) for collapse to a black hole, and the resulting Penrose diagram.
A stochastic wavevector approach is formulated to accurately represent compressible turbulence subject to rapid deformations. This approach is inspired by the incompressible particle representation model of Kassinos & Reynolds (1994), and preserves the exact nature of compressible rapid distortion theory (RDT). The adoption of a stochastic – rather than Fourier – perspective simplifies the transformation of statistics to physical space and serves as a starting point for the development of practical turbulence models. We assume small density fluctuations and isentropic flow to obtain a transport equation for the pressure fluctuation. This results in four fewer transport equations compared with the compressible RDT model of Yu & Girimaji (Phys. Fluids, vol. 19, 2007, 041702). The final formulation is closed in spectral space and only requires numerical approximation for the transformation integrals. The use of Monte Carlo for unit wavevector integration motivates the representation of the moments as stochastic variables. Consistency between the Fourier and stochastic representation is demonstrated by showing equivalency between the evolution equations for the velocity spectrum tensor in both representations. Sample clustering with respect to orientation allows for different techniques to be used for the wavevector magnitude integration. The performance of the stochastic model is evaluated for axially compressed turbulence, serving as a simplified model for shock–turbulence interaction, and is compared with linear interaction approximations and direct numerical simulation (DNS). Pure and compressed sheared turbulence at different distortion Mach numbers are also computed and compared with RDT/DNS data. Finally, two additional deformations are applied and compared with solenoidal and pressure-released limits to demonstrate the modelling capability for generic rapid deformations.
We consider some general properties of black holes and event horizons, of causality and topology. We define trapped surfaces, congruence, convergence, and show an example of a marginally trapped surface different than the event horizons. We prove the existence of an horizon for de Sitter spacetime, via its Penrose diagram. We then define Rindler spacetime, as the accelerated Minkowski spacetime, that gains an event horizon and mimics what happens for a black hole.
We consider parallel plane (pp) waves, solutions of Einstein’s equations for which the linearized equation is exact. We describe the Penrose theorem, for the Penrose limit, saying that in the neighborhood of a null geodesic, any space looks like a pp wave. We exemplify it for AdS3 × S3. We then consider gravitational shockwaves, an example of pp waves, in flat space, and in other backgrounds. Finally, we describe the Khan–Penrose interacting solution, for the head-on collision of two gravitational shockwaves.
Travelling wave charges lying on the insulating walls of an electrolyte-filled capillary give rise to oscillatory modes which vanish when averaged over the period of oscillation. They also give rise to a zero mode (a unidirectional, time-independent velocity component) which does not vanish. The latter is a nonlinear effect caused by continuous symmetry breaking due to the quadratic nonlinearity associated with the electric body force in the time-dependent Stokes equations. In this paper, we provide a unified view of the effects arising in boundary-driven electrokinetic flows (travelling wave electroosmosis) and establish the universal behaviour exhibited by the observables. We show that the incipient velocity profiles are self-similar implying that those obtained with a single experimental configuration can be employed again to attain further insights without the need of repeating the experiment. Certain results from the literature are recovered as special cases of our formulation and we resolve certain paradoxes having appeared in the past. We present simple theoretical expressions, depending on a single-fit parameter, that reproduce these profiles, which could thus provide a rapid test of consistency between our theory and future experiment. The effect becomes more pronounced when reducing the transverse dimension of the system, relative to the velocity direction, and increasing the excitation wavelength, and can therefore be employed for unidirectional transport of electrolytes in thin and long capillaries. General relations, expressing the zero mode velocity in terms of the electric potential and the geometry of the system only, can thus be easily adapted to alternative experimental settings.
Large-eddy simulation (LES) is performed to study the tip vortex flow in a ducted propulsor geometry replicating the experiments of Chesnakas & Jessup (2003, pp. 257–267), Oweis et al. (2006a J. Fluids Engng128, 751–764) and Oweis et al. (2006b J. Fluids Engng128, 751–764). Inception of cavitation in these marine propulsion systems is closely tied to the unsteady interactions between multiple vortices in the tip region. Here LES is used to shed insight into the structure of the tip vortex flow. Simulation results are able to predict experimental propeller loads and show agreement with laser Doppler velocimetry measurements in the blade wake at design advance ratio, $J=0.98$. Results show the pressure differential across the blade produces a leakage vortex which separates off the suction side blade tip upstream of the trailing edge. The separation sheet aft of the primary vortex separation point is shown to take the form of a skewed shear layer which produces a complex arrangement of unsteady vortices corotating and counter-rotating with the primary vortex. Blade tip boundary layer vortices are reoriented to align with the leakage flow and produce instantaneous low-pressure regions wrapping helically around the primary vortex core. Such low-pressure regions are seen both upstream and downstream of the propeller blade trailing edge. The trailing edge wake is found to only rarely have a low-pressure vortex core. Statistics of instantaneous low pressures below the minimum mean pressure are found to be concentrated downstream of the blade’s trailing edge wake crossing over the primary vortex core and continue in excess of 40 % chord length behind the trailing edge. The rollup of the leakage flow duct boundary layer behind the trailing edge is also seen to produce counter-rotating vortices which interact with the primary leakage vortex and contribute to strong stretching events.
We consider inflationary cosmology, but only general relativistic aspects of it. We first show some of the important problems with standard (Hot Big Bang) cosmology before inflation. Then we describe the general paradigm of inflation, and how it solves the cosmological problems. We specialize to inflation with a single scalar field, and moreover to slow-roll inflation. Finally, we calculate the fluctuations spectrum during inflation.
After a general description of event horizons, and the definition of the surface gravity of a horizon, we find some formulae valid at horizons. Finally, we calculate the Raychaudhuri equation for the convergence of a black hole, defining the fact that gravity is always convergent. We apply it to horizons, defined by null geodesics, where the equation is slightly modified.
We define the laws of black hole thermodynamics by first reviewing the laws of regular thermodynamics, and seeing what the analog of the zeroth, first, second, and third laws are. After stating them, we show some partial proofs. As part of this, we show a simple proof and a general argument for the Hawking radiation and the Hawking temperature of a black hole, and the corresponding Bekenstein–Hawking entropy of the black hole. We finish by defining the gravitational thermodynamic potential.
We define gravitoelectric and gravitomagnetic fields, that is, splitting the gravitational field into “electric” and “magnetic” components. We first use an electromagnetic analogy for perturbative fields, which however only works in the static case. Next, we use a covariant formulation, first defining it by using Weyl tensor components. But the best definition, that is found to be in complete analogy to the electromagnetic case, is by using the Riemann tensor components, to define tidal tensor, for the tidal effect on neighboring geodesics. To define the analogy, we first define tidal tensors in electromagnetism and write the Maxwell’s equations in terms of them, then define the tidal tensors in gravity, and find that the Einstein’s equations are also written in terms of the gravitational tidal tensors. As a first application, we find the Lense–Thirring effect, for the precession of satellites in orbit due to “frame-dragging,” and as a second application, the clock effect, for the effect of the period of the clocks in orbit.
In this study, the propagation behaviour of detonation waves in a channel filled with stratified media is analysed using a detailed chemical reaction model. Two symmetrical layers of non-reactive gas are introduced near the upper and lower walls to encapsulate a stoichiometric premixed H2–air mixture. The effects of gas temperature and molecular weight of the non-reactive layers on the detonation wave’s propagation mode and velocity are examined thoroughly. The results reveal that as the non-reactive gas temperature increases, the detonation wave front transitions from a ‘convex’ to a ‘concave’ shape, accompanied by an increase in wave velocity. Notably, the concave wave front comprises detached shocks, oblique shocks and detonation waves, with the overall wave system propagating at a velocity exceeding the theoretical Chapman–Jouguet speed, indicating the emergence of a strong detonation wave. Furthermore, when the molecular weight of non-reactive layers varies, the results qualitatively align with those obtained from temperature variations. To elucidate the formation mechanism of different detonation wave front shapes, a dimensionless parameter $\eta$ (defined as a function of the specific heat ratio and sound speed) is proposed. This parameter unifies the effects of temperature and molecular weight, confirming that the specific heat ratio and sound speed of non-reactive layers are the primary factors governing the detonation wave propagation mode. Additionally, considering the effect of mixture inhomogeneity on the detonation reaction zone, the stream tube contraction theory is proposed, successfully explaining why strong detonation waves form in stratified mixtures. Numerical results show good agreement with theoretical predictions, validating the proposed model.
We define the canonical formalism for gravity. After a quick review of the Dirac formalism for constrained systems, we use it for gravity, and find the Hamiltonian constraint and the momentum constraint. We use them for defining the Wheeler–de Witt equation, the quantum version of the Einstein equations, and their solution, the wave function of the Universe, in the Hawking “no-boundary boundary condition” and the Villenkin “tunneling from nothing” versions, with their corresponding interpretations. We also define the Brown–York stress tensor in AdS background. Finally, we define Ashtekar variables, and the corresponding quantization in Dirac formalism for canonical gravity.
The flow behind impulsively started circular and polygonal plates is investigated experimentally, using particle image velocimetry at several azimuthal angles. Observing plates accelerating up to a steady Reynolds number $Re=27\,000$, the three invariants of the motion, circulation $\Gamma$, hydrodynamic impulse $I$ and kinetic energy $E$, were scaled against four candidate lengths: the hydraulic diameter, perimeter, circumscribed diameter and the square root of the area. Of these, the square root of the area was found to best collapse all the data. Investigating the three-dimensionality of the flow, it is found that, while a single-plane measurement can provide a reasonable approximation for $\Gamma$ behind plates, multiple planes are necessary to accurately estimate $E$ and $I$.
We describe the Newman–Penrose formalism for gravity in four dimensions. We first define some relations for covariant derivatives, then define some basis vectors and the spin coefficients, for the spin connection in this basis. Then commutation relations and the transport relations for basis vectors, and the Newman–Penrose field equations, for the action of covariant derivatives on spin coefficients. We then show how we can change null frames, and the important case of the spinorial notation for the Newman–Penrose formalism. Finally, we describe some applications of the formalism.
We describe the fluid-gravity correspondence. After defining the equations for viscous relativistic fluids and for conformal fluids in particular, we consider the case of most interest, of conformal fluids described by black holes in asymptotically AdS space, that is, the fluid-gravity correspondence. We also describe it via the membrane paradigm, which was initially defined in asymptotically flat space, but makes sense in asymptotically AdS space. Finally, we take the nonrelativistic Navier–Stokes scaling limit of the equations, obtaining the Navier–Stokes equations.
The (Riemannian) curvature is based on the notion of a Riemann tensor. Actions in general relativity are found as a generalization of special relativity actions. The action for gravity, the Einstein–Hilbert action, is the simplest nontrivial action compatible with general relativity. Matter is described by the energy-momentum tensor, generalized from special relativity. The equations of motion obtained from the action are the Einstein’s equations.