1. Albert-Einstein-Institut www.aei-potsdam.mpg.de Black Hole Initial Data for Evolution Distorted Black Holes: “Brill Wave plus Black Hole” (NCSA model) –ds 2 =  4 (e 2q (dr 2 +r 2 d  2 )+ r 2 sin 2  d  2 ) q(r  ) --> true 3D distorted BH –Good model for late stage of BH merger Binary IVP: Multiple Wormhole Model –Misner 2BH: equal mass, time symmetric, colliding BHs, variations –Cook et al fully general merger data Binary IVP: Multiple “Punctures” –Brandt-Brügmann general merger data –Now evolving... More coming: Meudon/AEI/Jena S1S1 S2S2 P1P1 P2P2 S1S1 S2S2 P2P2 P1P1 S Brill Wave

2. Albert-Einstein-Institut www.aei-potsdam.mpg.de Why are Black Holes so Difficult? Collapsing Star Horizon Singularity t=150 t=100 t=50 t=0 Fundamental Problem with Black Holes Stretching of hypersurfaces leads to pathologies in metric functions Why not cut singularity away if surrounded by horizon??? Crash! g rr

3. Albert-Einstein-Institut www.aei-potsdam.mpg.de A Little Lesson in Black Hole Physics Black Hole Perturbation Theory –What happens when a BH is perturbed? –How can this be used in numerical work? –Going beyond linear theory through numerical relativity...

4. Albert-Einstein-Institut www.aei-potsdam.mpg.de What happens when a black hole is perturbed? Take existing black hole (Schwarzschild solution) –Analytic solution known since 1916! –Perturb by tossing pebble into it Is it stable? –Perturb metric tensor g  ds 2 = -(1-2M/r) dt 2 + dr 2 /(1-2M/r) + r 2 (d  2 + sin 2  d  2 ) by adding  h  (Y lm ), expand to first order in  –Discover (after 30 years study!) … –Scattering off potential barrier Find resonance frequencies of this potential barrier –  ~ exp(i  (t-x)) –  resonances are complex: get damped sinusoids –Frequency depends on mass and spin of BH, that’s all! In all theoretical studies, these modes are excited –Collapse of matter to a BH, Distorted, Colliding BH’s... V(r)  + V(r)  = 0 Black hole pebble Horizon

5. Albert-Einstein-Institut www.aei-potsdam.mpg.de Black Hole Normal Modes Ringing modes: damped sinusoid ~e i  t Measure this, can determine mass and spin of BH that created it Questions, Questions: what happens when we go beyond linear theory?

6. Albert-Einstein-Institut www.aei-potsdam.mpg.de Colliding BH Roadmap: A patchwork to success Time Post Newt inspiral Final Plunge Ringdown t ~ 500 + M t ~ 100 M t ~ 30 M Merger Phase Time Scale Technique Post N Perturbative Excision: making progress Standard Numrel: Exciting new results, but will break down gap Need Post-N BH Initial data

7. Albert-Einstein-Institut www.aei-potsdam.mpg.de Start with ADM Evolution Equations (used almost exclusively for last 30 years…) The 3+1 evolution equations used in numerical relativity are normally written as: These equations are highly non-unique: add arbitrary multiples of constraints, obtain new evolution equations that are just as valid. New equations: same physical solutions, but very different mathematical properties, different solutions away from constraint hypersurface (“off-shell”). Highly computationally intensive: want larger computers than exist, must perform many, many developmental tests: very slow! “Arnowitt-Deser-Misner” (or simply “ADM”) evolution equations.

8. Albert-Einstein-Institut www.aei-potsdam.mpg.de First attempt to go beyond axisymmetric, non-orbital data Brandt-Brügmann Puncture data Unequal mass, spin, orbital J Maximal slicing, no shift Nested grids to get boundary away from holes Merger of AH First True 3D Grazing Black Hole Collision Bernd Brügmann 97 Single outer AH appears as holes merge MTSs inside S1S1 S2S2 P2P2 P1P1 M1M1 M2M2 ADM evolution to about t=7M but then crash!

9. Albert-Einstein-Institut www.aei-potsdam.mpg.de Very important new thing: The BSSN Formulation All recent simulations use the Baumgarte-Shapiro (BS) Shibata- Nakamura (SN) reformulation of the EEs. This BSSN formulation is based on a conformal decomposition of the standard ADM equations: A crucial ingredient of the BSSN formulation is the introduction of the conformal connection functions as independent variables: The BSSN formulation has been found to be extremely stable when compared to standard ADM in a large variety of cases, both with and without matter, so it is our preferred choice. Will apply to NS, too!!

10. Albert-Einstein-Institut www.aei-potsdam.mpg.de Return to Brügmann Grazing Collision… Alcubierre, Allen, Benger, Brügmann,Lanfermann, Nerger, ES, Takahashi Could never do this before 1999 BSSN –Spent 2 years understanding BSSN (Alcubierre…) –Focused on pure waves (demanding, but w/o singularity complications) Then applied to BH problem –Big Boost! 5x as far! Finally doing real (toy?) physics with 3D numerical relativity… Next: NS-NS

11. Albert-Einstein-Institut www.aei-potsdam.mpg.de Gauge-Invariant waveform extraction: Extract physics, predict rotation and mass of final BH QNM’s seen at late times –Good fit for two lowest a/M = 0.73 Kerr QN modes –Fit improves with resolution –Fit poor if use different a/M values! Energy radiated in all modes of order 1% M ADM Energy Estimate: –M ir ≈ 3.0 –M AH ≈ 3.3 Compare –M ADM = 3.22 Have done parameter studies –Low, med, high spin cases Convergence of waveform Fit to Kerr QNM’s t/M  22 even  22 even  22 even good better best QNM fit (lowrez) QNM fit (medrez) QNM fit (highrez)

12. Albert-Einstein-Institut www.aei-potsdam.mpg.de Going Further: Black Hole Excision (Alcubierre, Brügmann, Pollney, Takahashi, ES) Computational domain horizon Excised region singularity Two Ingredients –Excise a region inside the AH. –(Superluminal) Shift vector! Hard! –Spherical topology, ill adapted to cartesian coords –Large shifts can cause instabilities: causal differencing –Moving across grid?? Everything from here forward unpublished so far… Unruh, ‘84, ES, Suen, ‘92, Alcubierre, Brügmann, ‘00, many others Crash!

13. Albert-Einstein-Institut www.aei-potsdam.mpg.de Shift Conditions (Alcubierre, et al…) New shift condition obtained by making the conformal connection functions to be time-independent: “Gamma-freezing” shift condition closely related to “minimal distortion” shift condition, but related to fundamental variables in BSSN! Obtain hyperbolic conditions by making second time derivatives of the shift proportional to the elliptic operator contained in the above condition. VERY important: will apply to NS, too!

14. Albert-Einstein-Institut www.aei-potsdam.mpg.de Schwarzschild: Horizon Mass M ADM =2,  x = 0.2, 128 3 grid points 3D run, excision+shift 2D run, no excision, no shift, high resolution Crash! 3D run, no excision, no shift Crash! Very robust No fine tuning! Remember: started with –  = 1 –  i = 0 It just works naturally… This is very new in the community…

15. Albert-Einstein-Institut www.aei-potsdam.mpg.de How about rotating, distorted BH?: Waveforms (  4 ) Mimics final stages of BBH Coalescence M ADM =7.54, a/M=0.62,  x = 0.5, 192 3 points 2D runs crashes! Remarkable agreement between 2D and 3D! Crash! S No fine tuning! It just works… very naturally as gauges drive system static… Shift has min. distortion character: like Boyer- Lindquist for Kerr so keeps coords OK Even waves are fine… Lots of other examples…

16. Albert-Einstein-Institut www.aei-potsdam.mpg.de Grazing Collision with shift and excision!! Starting to put it together Could never do this before… Only excise final BH Just a test, only 195 3 –Horizons great –Waveforms, too –Runs “forever” now Will be able to do 512 3,-768 3 Plenty of parameter tuning to do How far can this go? Move into ISCO and beyond… New, low res test simulation w/shift!! M AH Grazing results in press…

17. Albert-Einstein-Institut www.aei-potsdam.mpg.de Preliminary Result: Plunge from the ISCO using new shift, excision grid: 195x195x100 h = 0.083 excision of final BH

18. Albert-Einstein-Institut www.aei-potsdam.mpg.de The Evolution of the Evolution of 3D Black Holes DistortGrazing t(M) Evolution times for robust, accurate evolutions, with solid horizon physics, waveforms Lazarus Full non- Linear??? Pre-ISCO??

19. Albert-Einstein-Institut www.aei-potsdam.mpg.de Conclusions Main message: unusual progress, will benefit entire Network I have waited many years to see such results –1D broke through barrier in 1987 –2D in 1993-5 –3D got stuck until last year… Why is all this happening now? –We have a great team! (Critical mass, talent, focus, collaboration) –Developed much better theoretical understanding/practical experience. –We developed great collaborative technology (otherwise not possible.) –We have much better computers (need even more access) 3+1 codes have smashed through the t = 30M barrier –Shift to cure grid-stretching –Evolutions orders of magnitude better than last year All this applies to NS-NS and other problems! You get this for free!

20. Albert-Einstein-Institut www.aei-potsdam.mpg.de Hot off the Presses: Most Recent Waveform Result