Past Relativity Seminar

The Kerr solutions to Einstein's equations describe rotating black holes. For the wave equation in flat-space and outside the non-rotating, Schwarzschild black holes, one method for proving decay is the vector-field method, which uses the energy-momentum tensor and vector-fields. Outside the Schwarzschild black hole, a key intermediate step in proving decay involved proving a Morawetz estimate using a vector-field which pointed away from the photon sphere, where null geodesics orbit the black hole. Outside the Kerr black hole, the photon orbits have a more complicated structure. By using the hidden symmetry of Kerr, we can replace the Morawetz vector-field by a fifth-order operator which, in an appropriate sense, points away from the photon orbits. This allows us to prove the necessary Morawetz estimate. From this we can prove a decay estimate of almost $t^{-1}$ for fixed $r$ and the corresponding decay rates at the event horizon and null infinity. The major innovation in this result is that, by using the hidden symmetries with the energy-momentum, we can avoid taking Fourier tranforms in time.

This is joint work with Lars Andersson.

I will review our current mathematical understanding of waves on black hole backgrounds, starting with the classical boundedness theorem of Kay and Wald on Schwarzschild space-time and ending with recent boundedness and decay theorems on a wider class of black hole space-times.

A major issue in general relativity, from its earliest days to the

present, is how to extract physical information from any solution or

class of solutions to the Einstein equations. Though certain

information can be obtained for arbitrary solutions, e.g., via geodesic

deviation, in general, because of the coordinate freedom, it is often

hard or impossible to do. Most of the time information is found from

special conditions, e.g., degenerate principle null vectors, weak

fields close to Minkowski space (using coordinates close to Minkowski

coordinates) or from solutions that have symmetries or approximate

symmetries. In the present work we will be concerned with

asymptotically flat space times where the approximate symmetry is the

Bondi-Metzner-Sachs (BMS) group. For these spaces the Bondi

four-momentum vector and its evolution, found from the Weyl tensor at

infinity, describes the total energy-momentum of the interior source

and the energy-momentum radiated. By generalizing certain structures

from algebraically special metrics, by generalizing the Kerr and the

charged-Kerr metric and finally by defining (at null infinity) the

complex center of mass (the real center of mass plus 'i' times the

angular momentum) with its transformation properties, a large variety

of physical identifications can be made. These include an auxiliary

Minkowski space viewed from infinity, kinematic meaning to the Bondi

momentum, dynamical equations of motion for the center of mass, a

geometrically defined spin angular momentum and a conservation law with

flux for total angular momentum.

In this talk I shall review analytical and numerical results on equilibrium configurations of rotating fluid bodies within Einstein's theory of gravitation.

I will start by reviewing the current status of the stability

problem for black holes in general relativity. In the second part of the

talk I will focus on a particular (symmetry) class of five-dimensional

dynamical black holes recently introduced by Bizon et al as a model to

study gravitational collapse in vacuum. In this context I state a recent

result establishing the asymptotic stability of the five dimensional

Schwarzschild metric with respect to vacuum perturbations in the given

class.

> There is currently tremendous interest in geometric PDE, due in part
> to the geometric flow program used successfully to attack the Poincare
> and Geometrization Conjectures.  Geometric PDE also play a primary
> role in general relativity, where the (constrained) Einstein evolution
> equations describe the propagation of gravitational waves generated by
> collisions of massive objects such as black holes.
> The need to validate this geometric PDE model of gravity has led to
> the recent construction of (very expensive) gravitational wave
> detectors, such as the NSF-funded LIGO project.  In this lecture, we
> consider the non-dynamical subset of the Einstein equations called the
> Einstein constraints; this coupled nonlinear elliptic system must be
> solved numerically to produce initial data for gravitational wave
> simulations, and to enforce the constraints during dynamical
> simulations, as needed for LIGO and other gravitational wave modeling efforts.
>
> The Einstein constraint equations have been studied intensively for
> half a century; our focus in this lecture is on a thirty-year-old open
> question involving existence of solutions to the constraint equations
> on space-like hyper-surfaces with arbitrarily prescribed mean
> extrinsic curvature.  All known existence results have involved
> assuming either constant (CMC) or nearly-constant (near-CMC) mean
> extrinsic curvature.
> After giving a survey of known CMC and near-CMC results through 2007,
> we outline a new topological fixed-point framework that is
> fundamentally free of both CMC and near-CMC conditions, resting on the
> construction of "global barriers" for the Hamiltonian constraint.  We
> then present such a barrier construction for case of closed manifolds
> with positive Yamabe metrics, giving the first known existence results
> for arbitrarily prescribed mean extrinsic curvature.  Our results are
> developed in the setting of a ``weak'' background metric, which
> requires building up a set of preliminary results on general Sobolev
> classes and elliptic operators on manifold with weak metrics. 
> However, this allows us to recover the recent ``rough'' CMC existence
> results of Choquet-Bruhat
> (2004) and of Maxwell (2004-2006) as two distinct limiting cases of
> our non-CMC results.  Our non-CMC results also extend to other cases
> such as compact manifolds with boundary.
>
> Time permitting, we also outline some new abstract approximation
> theory results using the weak solution theory framework for the
> constraints; an application of which gives a convergence proof for
> adaptive finite element methods applied to the Hamiltonian constraint.

This is joint work with Gabriel Nagy and Gantumur Tsogtgerel.

 

Current numerical relativity codes model neutron star matter as a perfect fluid, with an unphysical "atmosphere" surrounding the star to avoid the breakdown of the equations at the fluid-vacuum interface at the surface of the star. To design numerical methods that do not require an unphysical atmosphere, it is useful to know what a generic sound wave looks near the surface. After a review of relevant mathematical methods, I will present results for low (finite) amplitude waves that remain smooth and, perhaps, for high amplitude waves that form a shock.

In the case of Einstein's equations coupled to a non-linear scalar field with a suitable exponential potential, there are solutions for which the expansion is accelerated and of power law type. In the talk I will discuss the future global non-linear stability of such models. The results generalize those of Mark Heinzle and Alan Rendall obtained using different methods.

We outline a method to solve the stationary Einstein equations with source a body in rigid rotation consisting of elastic matter.

This is work in progress by R.B., B.G.Schmidt, and L.Andersson

: I will review various constructions and properties of complete constant scalar curvature metrics. I will emphasize the role played by the so called "Fowler's solutions" which give rise to metrics with cylindrical ends. I will also draw the parallel between these constructions and similar constructions which surprisingly (or not) appear in a different context : constant mean curvature surfaces and more recently the Allen-Cahn equation and some equation in the biological theory of pattern formation.

One knows, for example by proving well-posedness for an initial value problem with data at the singularity, that there exist many cosmological solutions of the Einstein equations with an initial curvature singularity but for which the conformal metric can be extended through the singularity. Here we consider a converse, a local extension problem for the conformal structure: given an incomplete causal curve terminating at a curvature singularity, when can one extend the conformal structure to a set containing a neighbourhood of a final segment of the curve?

We obtain necessary and sufficient conditions based on boundedness of tractor curvature components. (Based on work with Christian Luebbe: arXiv:0710.5552, arXiv:0710.5723.)

In this talk I will look at a definition of the energy-momentum for the dynamical horizon of a black hole. The talk will begin by examining the role of a special class of observers at null infinity determined by Bramson's concept of frame alignment. It is shown how this is given in terms of asymptotically constant spinor fields and how this framework may be used together with the Nester-Witten two form to give a definition of the Bondi mass at null infinity.

After reviewing Ashtekar's concept of an isolated horizon we will look at the propagation of spinor fields and show how to introduce spinor fields for the horizon which play the role of the asymptotically constant spinor fields at null infinity, giving a concept of alignment of frames on the horizon. It turns out that the equations satisfied by these spinor fields give precisely the Dougan-Mason holomorphic condition on the cross sections of the horizon, together with a simple propagation equation along the generators. When combined with the Nester-Witten 2-form these equations give a quasi-local definition of the mass and momentum of the black hole, as well as a formula for the flux across the horizon. These ideas are then generalised to the case of a dynamical horizon and the results compared to those obtained by Ashtekar as well as to the known answers for a number of exact solutions.

Static vacuum data and their conformal classes play an important role in the discussion of the smoothness of gravitational fields at null infinity. We study the question under which conditions such data admit non-trivial conformal rescalings which lead again to such data. Some of the restrictions implied by this requirement are discussed and it is shown that there exists a 3-parameter family of static vacuum data which are not conformally flat and which admit non-trivial rescalings.

I will discuss ongoing work to provide a proof for the following

conjecture: if the development of a time symmetric, conformally flat

initial data set admits a smooth null infinity, then the initial data

is Schwarzschildean in a neighbourhood of infinity. The strategy

to construct a proof consists in a detailed analysis of a

certain type of expansions that can be obtained using H. Friedrich's

"cylinder at infinity" formalism. I will also discuss a toy model for

the analysis of the Maxwell field near the

spatial infinity of the Schwarzschild spacetime

It has been known for some time that in more than 4 spacetime dimensions, there is a considerably larger variety of black "hole" solutions, having e.g. different horizon topology. In particular, they are no longer fully characterized by their asymptotic charges (mass, angular momenta) alone. We give a partial classification theorem for higher dimensions, for solutions with sufficiently many axial Killing fields. We show that higher dimensional black holes may be fully characterized by their asymptotic charges, together with certain "moduli" and "winding numbers" that are analogous to those of Seiffert fibrations. In particular, we find constraints on the possible horizon topologies. In 5 dimensions, they may be either a black "hole" (sphere), black "ring", or a black "lens".

  I am going to discuss a special class of logarithmic solutions to WDVV equations. This type of solutions appeared in Seiberg-Witten theory is defined by a finite set of covectors, the V-systems. The V-systems introduced by Veselov have remarkable properties. They contain Coxeter root systems, and they are closed under taking subsystems and restrictions. The corresponding solutions are almost dual in Dubrovin's sense to the Frobenius manifolds structures on the orbit spaces of Coxeter groups and their restrictions to discriminants. Another source of V-systems is generalized root systems. The talk will be based on joint work with Veselov.