Center-of-mass angular momentum and memory effect in asymptotically flat spacetimes

Gravitational-wave (GW) memory effects are constant changes in the GW strain and its time integrals, which are closely connected to changes in the charges that characterize asymptotically flat spacetimes. The first GW memory effect discovered was a lasting change in the GW strain. It can occur when GWs or massless fields carry away 4-momentum from an isolated source. Subsequently, it was shown that fluxes of intrinsic angular momentum can generate a new type of memory effect called the spin memory, which is an enduring change in a portion of the time integral of the GW strain. In this paper, we note that there is another new type of memory effect. We call it the center-of-mass (CM) memory effect, because it is related to changes in the CM part of the angular momentum of a spacetime. We first examine a few properties of the CM angular momentum. Specifically, we describe how it transforms under the supertranslation symmetry transformations of the Bondi-Metzner-Sachs group, and we compute a new expression for the flux of CM angular momentum carried by GWs in terms of a set of radiative multipole moments of the GW strain. We then turn to the CM memory effect. The CM memory effect appears in a quantity which has units of the time integral of the GW strain. We define the effect in asymptotically flat spacetimes that start in a stationary state, radiate, and settle to a different stationary state. We show that it is invariant under infinitesimal supertranslation symmetries in this context. To determine the magnitude of the flux of CM angular momentum and the CM memory effect, we compute these quantities for nonspinning, quasicircular compact binaries in the post-Newtonian approximation. The CM memory effect arises from terms in the gravitational waveform for such binaries beginning at third and fourth post-Newtonian order for unequal- and equal-mass binaries, respectively. [Abstract abridged]Comment: v2: 26 pages; updated to match version published in Phys. Rev.

An Attempt to Reshape Capitalism’s Image

John Stuart Mill claimed to be a disciple of both Jeremy Bentham and David Ricardo. This was a strange proclamation because each man advocated a competing theory of value; Bentham’s utilitarianism laid the foundation for the utility theory of value and Ricardo developed the labor theory of value. Mill’s goal in attempting to unify these theories of value was to provide a solution for the growing class conflict that plagued capitalism. Class conflict arose as feudalism was phased out and industrial capitalism replaced merchant capitalism as the dominant economic system. The Corn Laws symbolized this competition between classes. Capitalists were against the Corn Laws because the subsequent tariffs would lower their rate of profit. Landowners supported the Corn Laws because they increased the rent on land. Even Karl Marx held spoke out against the Corn Laws on behalf of the working class. Capitalism fostered persistent antagonism between classes as each struggled to gain or maintain power; no class was immune from this contest. Class conflict was therefore ubiquitous in capitalist society and generated widespread scrutiny and debate over capitalism. Jeremy Bentham and David Ricardo took opposing sides in this debate. Bentham was initially supported it but died a reformist. Class conflict was resolvable but not under the current form of capitalism. Ricardo’s labor theory of value promoted the view that class division occurred naturally in a capitalist society. And since capitalism was the best possible economic system, class division was a necessary evil and could not be remedied. Both Ricardo and Bentham acknowledged that class conflict was inherent in capitalism but each treated it differently. In claiming to be a disciple of both men, Mill hoped to show that capitalism could exist alongside social harmony. His goal was to change the nature of capitalism. [excerpt

Hybrid method for understanding black-hole mergers: Inspiralling case

We adapt a method of matching post-Newtonian and black-hole-perturbation theories on a timelike surface (which proved useful for understanding head-on black-hole-binary collisions) to treat equal-mass, inspiralling black-hole binaries. We first introduce a radiation-reaction potential into this method, and we show that it leads to a self-consistent set of equations that describe the simultaneous evolution of the waveform and of the timelike matching surface. This allows us to produce a full inspiral-merger-ringdown waveform of the l=2, m=±2 modes of the gravitational waveform of an equal-mass black-hole-binary inspiral. These modes match those of numerical-relativity simulations well in phase, though less well in amplitude for the inspiral. As a second application of this method, we study a merger of black holes with spins antialigned in the orbital plane (the superkick configuration). During the ringdown of the superkick, the phases of the mass- and current-quadrupole radiation become locked together, because they evolve at the same quasinormal-mode frequencies. We argue that this locking begins during the merger, and we show that if the spins of the black holes evolve via geodetic precession in the perturbed black-hole spacetime of our model, then the spins precess at the orbital frequency during the merger. In turn, this gives rise to the correct behavior of the radiation, and produces a kick similar to that observed in numerical simulations

Properties of an affine transport equation and its holonomy

An affine transport equation was used recently to study properties of angular momentum and gravitational-wave memory effects in general relativity. In this paper, we investigate local properties of this transport equation in greater detail. Associated with this transport equation is a map between the tangent spaces at two points on a curve. This map consists of a homogeneous (linear) part given by the parallel transport map along the curve plus an inhomogeneous part, which is related to the development of a curve in a manifold into an affine tangent space. For closed curves, the affine transport equation defines a "generalized holonomy" that takes the form of an affine map on the tangent space. We explore the local properties of this generalized holonomy by using covariant bitensor methods to compute the generalized holonomy around geodesic polygon loops. We focus on triangles and "parallelogramoids" with sides formed from geodesic segments. For small loops, we recover the well-known result for the leading-order linear holonomy ($\sim$ Riemann $\times$ area), and we derive the leading-order inhomogeneous part of the generalized holonomy ($\sim$ Riemann $\times$ area$^{3/2}$). Our bitensor methods let us naturally compute higher-order corrections to these leading results. These corrections reveal the form of the finite-size effects that enter into the holonomy for larger loops; they could also provide quantitative errors on the leading-order results for finite loops.Comment: 18 pages, 4 figures, new short section (Sec. 5) in v3; updated to match article published in GR

Observer dependence of angular momentum in general relativity and its relationship to the gravitational-wave memory effect

We define a procedure by which observers can measure a type of special-relativistic linear and angular momentum $(P^a, J^{ab})$ at a point in a curved spacetime using only the spacetime geometry in a neighborhood of that point. The method is chosen to yield the conventional results in stationary spacetimes near future null infinity. We also explore the extent to which spatially separated observers can compare the values of angular momentum that they measure and find consistent results. We define a generalization of parallel transport along curves which gives a prescription for transporting values of angular momentum along curves that yields the correct result in special relativity. If observers use this prescription, then they will find that the angular momenta they measure are observer dependent, because of the effects of spacetime curvature. The observer dependence can be quantified by a kind of generalized holonomy. We show that bursts of gravitational waves with memory generically give rise to a nontrivial generalized holonomy: there is, in this context, a close relation between the observer dependence of angular momentum and the gravitational-wave memory effect.Comment: 19 pages, 2 figures. Matches version published in Phys. Rev. D with errors in Appendix A correcte

Boundary operators in the O(n) and RSOS matrix models

We study the new boundary condition of the O(n) model proposed by Jacobsen and Saleur using the matrix model. The spectrum of boundary operators and their conformal weights are obtained by solving the loop equations. Using the diagrammatic expansion of the matrix model as well as the loop equations, we make an explicit correspondence between the new boundary condition of the O(n) model and the "alternating height" boundary conditions in RSOS model.Comment: 29 pages, 4 figures; version to appear in JHE

Supersymmetry on Jacobstahl lattices

It is shown that the construction of Yang and Fendley (2004 {\it J. Phys. A: Math.Gen. {\bf 37}} 8937) to obtainsupersymmetric systems, leads not to the open XXZ chain with anisotropy $\Delta =-{1/2}$ but to systems having dimensions given by Jacobstahl sequences.For each system the ground state is unique. The continuum limit of the spectra of the Jacobstahl systems coincide, up to degeneracies, with that of the $U_q(sl(2))$ invariant XXZ chain for $q=\exp(i\pi/3)$. The relation between the Jacobstahl systems and the open XXZ chain is explained.Comment: 6 pages, 0 figure

Thermal vacuum testing techniques for spacecraft

Cesium frequency standards are to be flown on the NTS-2 satellite which is a program conducted to develop technology and time standards for NAVSTAR Global Positioning System. Mission requirements for the thermal design of this frequency standard called for a low nominal temperature (15 C) and the removal of most of the heat generated by the standard from the spacecraft. The test program run to determine the thermal properties of the frequency standard is described. A simulator was constructed for these tests. Special mathematical analysis techniques were developed and were used to predict the thermal environment for different orbital conditions. Thermal vacuum tests of the flight frequency standard and the integrated spacecraft demonstrated the validity of this technique

Oceanographic satellite remote sensing: Registration, rectification, and data integration requirements

The problem of data integration in oceanography is discussed. Recommendations are made for technique development and evaluation, understanding requirements, and packaging techniques for speed, efficiency and ease of use. The primary satellite sensors of interest to oceanography are summarized. It is concluded that imaging type sensors make image processing an important tool for oceanographic studies