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Black hole binary mergers: recent developments in numerical relativity First-term presentation By Nikos Fanidakis Supervisors: Carlton Baugh, Shaun Cole, Carlos Frenk 13/12/2007
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Outline Brief introduction to gravitational waves Black hole (BH) binary mergers in numerical relativity Astrophysical implications: recoil kicks Discussion – conclusions
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3 Quantum Fluctuations in the Early Universe Merging super-massive black holes (SMBHs) at galactic cores Capture of BHs and compact stars by SMBH Merging binary NSs and BHs in distant galaxies NS quakes and magnetars Gravitational wave radiation Gravitational Waves: ripples of space-time curvature propagating at the speed of light. Gravitational wave sources: any source with nonzero quadrupole moment. Amplitude h ≈ (GM/Rc 2 )(R/D) =10 -23 -10 -21
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BH mergers in numerical relativity: 1964-2005 Image courtesy: Kip Thorne BHs are strong sources of gravitational waves! A merge of two equal mass BHs releases ~ 10 56 ergs/s Accurate gravitational waveforms are essential for LISA First attempt by Hahn – Lindquist (1964): inspiral (!) → merger(??) → ringdown (!) ?
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BH mergers in numerical relativity: 2005-2007 time amplitude inspiral merger ringdown Baker et al. 2006 1. The technique: “3+1” decomposition 3-d hypersurfaces. Evolution of hypersurface through time using 17 nonlinear, coupled differential eqns! 2. The breakthrough (Baker et al. 2006): Fixed “puncture” representation of the BH Comoving coordinates
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Astrophysical implications: recoil kicks Centrella et al. 2007 Asymmetric BH mergers impart a recoil kick to the final remnant (ejection from host structure?) Unequal-mass BH merger simulation (Gonzalez et al. 2007): o Initial binary: m 1 =0.36m 2 u kick ~ 176 km/s Highly-spinning BH merger simulation (Herrmann et. 2007): o Initial binary: equal-mass BHs with anti-aligned equal spins u kick =475 km/s M-σ relation constraint ≈ 500 km/s If spin not perpendicular to orbital plane u kick up to 2000 km/s (Campanelli et al. 2007)
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Discussion – conclusions known
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