Gravitational Wave Astrophysics Theory, Simulation, Observation
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1 Gravitational Wave Astrophysics Theory, Simulation, Observation Rainer Spurzem + Silk Road Team (Li Shuo, Peter Berczik, Thijs Kouwenhoven Long Wang, Maxwell Cai, Shu Qi,...) NAOC/CAS KIAA/PKU ARI/ZAH spurzem@nao.cas.cn
2 GW Detection Abott et al. 2016
3 GW Detection Abott et al. 2016
4 Kupi, G., Amaro-Seoane, P., Spurzem, R., object clusters: a post-newtonian study, Dynamics of compact 2006, MNRAS 371, L45 Berentzen, I., Preto, M., Berczik, P., Merritt, D., Spurzem, R., Binary Black Hole Merger in Galactic Nuclei: PostNewtonian Simulations, 2009, ApJ 695, 455
5 J. Downing VESF Fellow Heidelberg MNRAS 2010 MNRAS 2010 MNRAS 2011
6 Downing et al. 2011
7 Black holes in star clusters/nuclei Some theory Gravitational Wave Observations
8 Galaxies merge, hierarchical Structure formation, their centres? Black Holes? Volonteri
9 Galactic Nuclei, Black Holes Sesana et al Extending study of Volonteri et al. 03: Rate of expected Black Hole Mergers in Galaxies
10 Simulations of Binary Black Holes Z Black Holes in Dense Stellar Clusters: N-Body Problem with General Relativity (Post-Newtonian) Y Two equal-mass black holes in central core of simplified galaxy (up to 4 million particles) X
11 Post-Newtonian Dynamics... and they merge! Berentzen, Preto, Berczik, Merritt, Spurzem, 2009, ApJ
12 Simulations with stars and dark matter
13 Box Size 4 kpc 40 Myr after galaxy merger Simulations with stars and dark matter, Khan et al. 2012
14 Simulations with gas and dark matter Khan, Berentzen, Berczik, Just, Mayer, Nitadori, Callegari, ApJ 756, 30 (2012) See also Khan, Holley-Bockelmann, Berczik, Just, ApJ 2013 And Khan, Holley-Bockelmann, Berczik, ApJ 2015 milli-pc separation predicted two years before observation Fazeel Mahmood Khan ARI Heidelberg
15 (Khan et al. 2012) LISA band Full Model from Merger To SMBH coalescence 6 orders in separation! GW Emission from Pulsar Timing to LISA band modelled Pulsar Timing SMBH Bin. Eccentricity 1 / SMBH Bin. Separation Pulsar Timing Also Worked on SMBH Triples! Amaro-Seoane, Sesana,Benacquista, Spurzem MNRAS 2010! LISA band Fazeel Mahmood Khan ARI Heidelberg
16 Sobolenko, Berczik, Spurzem, in prep 2016
17 Sobolenko,Berczik,Spurzem, in prep 2016
18 Black holes in star clusters/nuclei Some theory Gravitational Wave Observations
19 Approaches: Quasi-Newtonian Source compute far-field grav. radiation, Einstein quadrupole formula, Landau-Lifschitz. from energy loss compute orbital change Tyson & Giffard 1978 Pioneers: Peters & Mathews 1963, Peters 1964
20 Note: dipole moment conserved due to linear momentum conservation Tyson & Giffard 1978
21 Tyson & Giffard 1978
22 Sources In Luminosity Tyson & Giffard Ann. Rev. Astr. Astroph. 1978!! PMO-Nanjing-2012
23 Relativistic Orbital Decay initial orbital ecc. determines ecc. at final merger; waveforms and emitted frequency of G.W. changes! Peters, P.C., Phys. Rev. 1964, 136, 1224 Peters, P.C., Mathews, J., 1963, Phys. Rev. 131, 435
24 Peters & Mathews 1963: Distribution of Power in Harmonics for Eccentric Orbits
25 Indirect Proof by Hulse and Taylor, binary pulsar (Nobel prize 1993)
26 Slide by P. Laguna
27 Slide by P. Laguna
28 Slide by P. Laguna
29 Post-Newtonian Dynamics r;v : relative distance, velocity μ = m1m2/m : reduced mass ( M = m1 + m2 ) ν=μ/m : mass ratio n = r / r : unit vector in radial direction Perihel shift... higher order... Grav. Radiation Schäfer, Gauge Theor. Grav. 36, 2223 (2004) Memmesheimer, Gopakumar, Schäfer, Phys. Rev.D 70, (2004) Blanchet, Luc; Living Reviews 2002, llr
30
31
32 Gravity Waves What happens afterwards? Post-Newton Order Kupi, Amaro-Seoane & Spurzem 2006
33 Post-Newtonian Dynamics Brem, Amaro-Seoane, Spurzem, MNRAS 2013 Include Spin-Orbit Spin-Spin PN3, PN3.5 Spin Dynamics By Patrick Brem (Diploma Thesis Univ. Heidelberg) 1PN 2PN + 1.5PN SO 3PN + 2.5PN SO 2.5PN + 2PN SS 3.5PN
34 Post-Newtonian Dynamics Spin-Orbit Interaction S / Spin-Spin SS Faye, Blanchet, Buonanno 2006
35 Rezzolla Final Spin Formula Brem, Amaro-SeoaneS, Spurzem, MNRAS 2013
36 PostNewtonian Dynamics Gravitational Wave Templates Handle spin-orbit and spin-spin coupling (P.Brem, R. Spurzem, Univ. Heidelberg)
37 Black holes in star clusters/nuclei Some theory Gravitational Wave Observations
38 Observable Properties of Gravity Waves Luminosity L = (Asymm.) v G M L= 5 c 5 a 5 (1 e 2 )7/2 Frequency f = 2π/ T Orbital Frequency of System Lowest Order Gravity Wave Frequency: from f to about 10f circular orbit: 2f Polarisation Amplitude h Two Polarisations in Einstein s Theory: + und x
39 Observable Properties of Gravity Waves Summary: Property Variation with Distance from Source Observable ============================================== Amplitude 1/r direct Luminosity 1/r^2 not direct Frequency constant Data analysis Polarisation constant Data analysis
40
41 VIRGO Detector in Cascina near Pisa, Italy LISA = Laser Space Interferometer Antenna
42 VIRGO Pisa 3km LIGO Livingston, LA Hanford, WA 4km GEO600 Hannover 600m KAGRA - Japan Advanced: Outreach to 50 Millionen light years (Neutron Stars)
43 VIRGO near Pisa, Italy (also: LIGO, GEO600): Laser-Interferometer Technique Largest Vacuum on Earth Distance Measurement < 10^(-15) cm (proton diameter)
44 Now: KAGRA
45 Pulsars: ACase Study Pulsars discovered in Galactic Census also provide network of arms of a huge cosmic gravitational wave detector Perturbation in space-time can be detected in timing residuals PTA: Pulsar Timing Array Sensitivity: dimensionless strain Slide by: M. Kramer σ TOA hc (f )~ T FAST!!
46 Moore et al. 2015
47
48 Moore's Law for Direct N-Body GRAPE/GPU Clusters 10**6 Wang, Sp, Aarseth,..15 Heggie et al. 15 Makino, Baumg. Merritt..., Baumgardt, Heggie, Hut Baumgardt, Makino GRAPE Vector Computers 2010 by D.C. Heggie Via added new cits. Spurzem
49 DRAGON Simulation One million stars direct simulation, biggest and most realistic direct N-Body simulation of globular star clusters. With stellar mass function, single and binary stellar evolution, regularization of close encounters, tidal field (NBODY6++GPU). (NAOC/Silk Road/MPA collaboration). Wang, Spurzem, Aarseth, Naab et al. MNRAS, 2015 Wang, Spurzem, Aarsteh Naab, et al. MNRAS 2016
50 GW Detection Frequency Time Diagram Top: Our simulation (Sobolenko Veles, Wang, Berczik, Spurzem, et al. In prep.) Down: Abott et al LIGO measurement
51 2011 AMSS/NAOC (Silk Road) collaboration 2015
52 Chinese Space Mission Case Study ALIA Gong, Lau, Amaro-Seoane, Spurzem et al. 2015
53 ALIA Hand Drawn Estimate Sesana 2016 Our DRAGON Black Hole Binary
54 64 Kepler K20 Request: New Supercomputer Laohu: 2009/2013 (Kepler GPU) 100 Tflop/s 150k cores Need: ~100 Pascal GPU 1.5 Pflop/s 300k cores Compare: AEI Hannover B. Allen MPG Garching Hydra
55 Slide of: Long Wang
56 Summary Gravitational Wave Sources: Time Varying Quadrupole Moment Binary Black Holes / Neutron Stars / w.dw. Asymmetric Collapse of Supernova Cores Big Bang? We can do the modelling of astrophysical GW sources at NAOC! Current Observation Technique: Laser Interferometry Ground Based High Frequency ( Hz) Space Based Low Frequency ( Hz) Pulsar Timing Arrays (ultra low frequency) We have (soon) FAST and possibly ALIA/eLISA (coop?)! Multi-Messenger Observations (future): GW observation triggers EM GW = gravitational wave EM = electromagnetic
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