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Recent Developments in Black Hole Binary Mergers and Gravitational Waves

This presentation explores advancements in numerical relativity focusing on black hole binary mergers, gravitational wave radiation, and astrophysical implications like recoil kicks. It discusses merging binary neutron stars, black holes, and super-massive black holes in galaxies, as well as phenomena like NS quakes and quantum fluctuations in the early universe. The talk covers the evolution of numerical simulations from 1964 to 2007 and highlights key breakthroughs, techniques, and implications for astrophysics. The importance of accurate gravitational waveforms for projects like LISA is emphasized.

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Recent Developments in Black Hole Binary Mergers and Gravitational Waves

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  1. Black hole binary mergers: recent developments in numerical relativityFirst-term presentationBy Nikos FanidakisSupervisors: Carlton Baugh, Shaun Cole, Carlos Frenk13/12/2007

  2. Outline • Brief introduction to gravitational waves • Black hole (BH) binary mergers in numerical relativity • Astrophysical implications: recoil kicks • Discussion – conclusions

  3. Merging binary NSs and BHs in distant galaxies Capture of BHs and compact stars by SMBH Merging super-massive black holes (SMBHs) at galactic cores NS quakes and magnetars Quantum Fluctuations in the Early Universe 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/Rc2)(R/D) =10-23-10-21

  4. BH mergers in numerical relativity: 1964-2005 • BHs are strong sources of gravitational waves! • A merge of two equal mass BHs releases ~1056 ergs/s • Accurate gravitational waveforms are essential for LISA • First attempt by Hahn – Lindquist (1964): inspiral (!) → merger(??) → ringdown (!) ? Image courtesy: Kip Thorne

  5. BH mergers in numerical relativity: 2005-2007 • 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 merger ringdown inspiral amplitude time Baker et al. 2006

  6. Astrophysical implications: recoil kicks • Asymmetric BH mergers impart a recoil kick to the final remnant (ejection from host structure?) • Unequal-mass BH merger simulation (Gonzalez et al. 2007): • Initial binary: m1=0.36m2 • ukick~176 km/s • Highly-spinning BH merger simulation (Herrmann et. 2007): • Initial binary: equal-mass BHs with anti-aligned equal spins • ukick =475 km/s • M-σrelation constraint≈ 500km/s • If spin not perpendicular to orbital plane ukick up to 2000 km/s (Campanelli et al. 2007) Centrella et al. 2007

  7. Discussion – conclusions known

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