In the following you can find useful material for research or even public presentations. The data and routines are freely available, but we would appreciate if you reference the original work.

Contents:
Ringdown data
Ringdown routines
Nonlinear solutions
Presentations
Movies

Ringdown data

Ringdown Routines

Nonlinear solutions

Presentations

Black hole collisions
Workshop on BHs and Higher Dimensions, 2010, Imperial College, London.
Hunting black holes
BHs III, 2010, Braga.
Nas Fronteiras da Gravitação
Public lecture for Lecture Series “Nas Fronteiras do Universo”, 2010, Gulbenkian, Lisbon.
Canonical formulation of spinning objects in general relativity from an action approach
GR19, 2010, Mexico City, Mexico. (talk received a James B. Hartle Award)
Canonical formulation of spinning objects in general relativity
2010, DPG Spring Meeting, Germany.
The PN Approximation beyond Point-Masses
2011, CENTRA, IST, Lisbon.
Energy extraction from BHs
Recent advances in numerical and analytical methods for BH dynamics, 2012, YITP, Kyoto.
Black hole bombs
Exploring AdS/CFT Dualities in Dynamical Settings, 2012, Perimeter Institute.
Perturbations of slowly-rotating black holes
2012, SISSA (Trieste).
Superradiant Instabilities
IRSES Meeting 2012, Aveiro.
Black hole dynamics in generic spacetimes
Recent advances in numerical and analytical methods for BH dynamics, 2012, YITP, Kyoto.
Inverse scattering construction of dipole black rings
Relativity and Gravitation, 100 Years after Einstein in Prague, 2012, Czech Republic.
Relatividade, buracos negros, censura e paradoxos
Prepared for outreach directed at high school students, 2013, Lisbon. (In portuguese.)
Massive spin-2 fields on black hole spacetimes
GR20, 2013, Warsaw, Poland.

Movies

1) High energy black hole collisions




The collision of two boosted black holes (v=0.75c in the center of mass frame), with a finite impact parameter in asymptotically flat spacetime. About 24% of the center of mass frame can be released as radiation, for this collision. The final hole is nearly maximally spinning. The intensity of the color refers to the amplitude of the gravitational waves as measured by Ψ₄.

Ref: Sperhake et al, Phys.Rev.Lett.103:131102(2009); arXiv:0907.1252 [gr-qc]

2) Black holes in a box



The inspiral and coalescence of two black holes, with total mass M, inside a confining box of radius 48 M. Out- and in-going waves are measured respectively by Ψ₄ and Ψ₀.

Ref: Witek et al, Phys.Rev.D82:104037 (2010) ; e-Print: arXiv:1004.4633

3) Black hole bombs I. Scalar fields



The time evolution of a massive scalar field around a highly spinning black holes. The scalar field is initially in a bound state, and continues to be for thousands of orbital periods. Colors depict field intensity. For details see

Ref: Witek et al, submitted for publication; e-Print: arXiv:1212.0551

4) Black hole bombs II. Vector fields



The time evolution of a massive vector field around a highly spinning black holes. The vector field is initially a generic gaussian. Colors depict field intensity. For details see

Ref: Witek et al, submitted for publication; e-Print: arXiv:1212.0551

5) Black hole collisions in de Sitter spacetime



Two black holes of sufficiently large mass in de Sitter spacetime would, upon merger, give rise to too large a black hole to fit in its cosmological horizon, resulting in a naked singularity. We here test such a configuration. Even though the initial separation is very small, we find that the holes move away from each other, with a proper separation increasing as the simulation progresses (the apparent decrease in separation is due to a "Ref: Witek et al, in preparation (2013) ; zoom" out motion of the observer). Further into the evolution, distorted common apparent (cosmological) horizons appear surrounding each black hole (in blue), and remain for as long as the simulation lasts. The evolution therefore indicates that the spacetime becomes, to an excellent approximation, empty de Sitter space for the observer at z=0 and that the black holes are not in causal contact.. For details see

Ref: Zilhao et al, Phys.Rev.D85:104039(2012) ; e-Print: arXiv:1204.2019 [gr-qc]