Numerical study For comparable mass binary systems,the inspiral phase could be well modeled by post-Newtonian(PN)theory and numerical relativity. For EMRIs(~10-6),BH perturbation theory(Teukolsky formalism) For IMRACs,not very clear!A hybrid approach,PN Teukolsky formalism Kludge waveform model 006.e2008. However,the kludge waveform model is developed to compute waveform templates rapidly,without a high precision 口·三色，至990
. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Numerical study For comparable mass binary systems, the inspiral phase could be well modeled by post-Newtonian(PN) theory and numerical relativity. For EMRIs (q ∼ 10−6 ), BH perturbation theory (Teukolsky formalism) For IMRACs, not very clear! A hybrid approach, PN + Teukolsky formalism Kludge waveform model Babak et.al. 2006, Huerta et.al. 2008... However, the kludge waveform model is developed to compute waveform templates rapidly, without a high precision Analytic study?
Numerical study For comparable mass binary systems,the inspiral phase could be well modeled by post-Newtonian(PN)theory and numerical relativity. For EMRIs(g~10-6),BH perturbation theory (Teukolsky formalism) For IMRACs,not very clear!A hybrid approach,PN+Teukolsky formalism Kludge waveform model 2006.He200. However,the kludge waveform model is developed to compute waveform templates rapidly,without a high precision Analytic study? 4口◆4回t1三1声，￥QC
. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Numerical study For comparable mass binary systems, the inspiral phase could be well modeled by post-Newtonian(PN) theory and numerical relativity. For EMRIs (q ∼ 10−6 ), BH perturbation theory (Teukolsky formalism) For IMRACs, not very clear! A hybrid approach, PN + Teukolsky formalism Kludge waveform model Babak et.al. 2006, Huerta et.al. 2008... However, the kludge waveform model is developed to compute waveform templates rapidly, without a high precision Analytic study?
Analytic study on high spin BH Consider the case thethe central object is a maximally spinning Kerr black hole. Type I IMRAC:IMBH is a near-extreme BH 口·三色，至990
. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Analytic study on high spin BH Consider the case the the central object is a maximally spinning Kerr black hole. Type I IMRAC: IMBH is a near-extreme BH Type II IMRAC: the central object is a Gargantua Gargantua: the supermassive BH which is nearly maximal spinning K. Thorne ”Interstellar” X-ray observations: 7 out of 22 AGNs are candidates for being high spin BH Brenneman 1309.6334 Why a near extreme Kerr BH special? Enhanced scaling symmetry in the near horizon region
Analytic study on high spin BH Consider the case the the central object is a maximally spinning Kerr black hole. Type I IMRAC:IMBH is a near-extreme BH Type II IMRAC:the central object is a Gargantua Gargantua:the supermassive BH which is nearly maximal spinning K.Thore "interstellar" X-ray observations:7 out of 22 AGNs are candidates for being high spin BH Brenneman 1300.6334 4口◆4回t1三1声，￥QC
. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Analytic study on high spin BH Consider the case the the central object is a maximally spinning Kerr black hole. Type I IMRAC: IMBH is a near-extreme BH Type II IMRAC: the central object is a Gargantua Gargantua: the supermassive BH which is nearly maximal spinning K. Thorne ”Interstellar” X-ray observations: 7 out of 22 AGNs are candidates for being high spin BH Brenneman 1309.6334 Why a near extreme Kerr BH special? Enhanced scaling symmetry in the near horizon region
Analytic study on high spin BH Consider the case the the central object is a maximally spinning Kerr black hole. Type I IMRAC:IMBH is a near-extreme BH Type II IMRAC:the central object is a Gargantua Gargantua:the supermassive BH which is nearly maximal spinning K.ThoeRe "Interstellar" X-ray observations:7 out of 22 AGNs are candidates for being high spin BH Brenneman 1309.6334 Why a near extreme Kerr BH special? Enhanced scaling symmetry in the near horizon region. 口卡4三色至习QC
. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Analytic study on high spin BH Consider the case the the central object is a maximally spinning Kerr black hole. Type I IMRAC: IMBH is a near-extreme BH Type II IMRAC: the central object is a Gargantua Gargantua: the supermassive BH which is nearly maximal spinning K. Thorne ”Interstellar” X-ray observations: 7 out of 22 AGNs are candidates for being high spin BH Brenneman 1309.6334 Why a near extreme Kerr BH special? Enhanced scaling symmetry in the near horizon region