北京大学：Spin and Quadrupole Couplings of IMRACs（主讲：陈斌）

Spin and Quadrupole Couplings of IMRACs 陈斌 北京大学 ICTS-USTC,2019年4月28日 Based on arXiv:1901.05370 with G.Compere,Y.Liu(ULB),J.Long(APCTP)and X.A.Zhang(PKU) ,口++，，2，生。卷QC

. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Spin and Quadrupole Couplings of IMRACs 陈斌 北京大学 ICTS-USTC, 2019 年 4 月 28 日 Based on arXiv: 1901.05370 with G. Compère, Y. Liu(ULB), J. Long(APCTP) and X.A. Zhang(PKU)

IMBH:intermediate-mass black holes MBH ~102 -105Mo IMBHs could be primordial,generated in the early Universe,or they may form in center of dense globular clusters through runaway stellar collision. They are thought to be the seeds from which SMBHs grow. Astrophysical problems:galaxy formation and growth,BH accretion and the reionisation .. Accumulated evidence:X-ray and optical observation No reliable way to determine its mass and spin →Gravitational wave? 4口◆4回t1三1声，￥QC

. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . IMBH: intermediate-mass black holes MBH ∼ 102 − 105M⊙ IMBHs could be primordial, generated in the early Universe, or they may form in center of dense globular clusters through runaway stellar collision. They are thought to be the seeds from which SMBHs grow. Astrophysical problems: galaxy formation and growth, BH accretion and the reionisation ... Accumulated evidence: X-ray and optical observation No reliable way to determine its mass and spin ⇒ Gravitational wave?

IMRAC:intermediate mass-ratio coalescence Mc010-2-10-4. q一MBH In the literature,it was often termed intermediate mass-ratio inspiral (IMRI). 口卡4三色至习QC

. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . IMRAC: intermediate mass-ratio coalescence q = MCO MBH ∼ 10−2 − 10−4 . In the literature, it was often termed intermediate mass-ratio inspiral (IMRI). Two types of IMRACs: 1. Type I: the stellar mass compact object orbiting around IMBH 2. Type II: IMBH orbiting around a supermassive black hole in the center of galaxies

IMRAC:intermediate mass-ratio coalescence Mc0≈10-2-10-4. q≠MBH In the literature,it was often termed intermediate mass-ratio inspiral (IMRI).Two types of IMRACs: 1.Type I:the stellar mass compact object orbiting around IMBH 2.Type Il:IMBH orbiting around a supermassive black hole in the center of galaxies 口4回4左+1色，生QC

. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . IMRAC: intermediate mass-ratio coalescence q = MCO MBH ∼ 10−2 − 10−4 . In the literature, it was often termed intermediate mass-ratio inspiral (IMRI). Two types of IMRACs: 1. Type I: the stellar mass compact object orbiting around IMBH 2. Type II: IMBH orbiting around a supermassive black hole in the center of galaxies

GW from IMRACs Depending on their orbital parameters,IMRACs in clusters can be detectable not only by the planned space-based gravitational wave observatories,including LISA,太极/天琴，，but also by the ground-based observatories,LIGO/Virgo,KAGRA or ET.AmaSeoane 20.Audley et.al.2017,Huerta et.al.2011 口·三色，至990

. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . GW from IMRACs Depending on their orbital parameters, IMRACs in clusters can be detectable not only by the planned space-based gravitational wave observatories, including LISA, 太极/天琴,..., but also by the ground-based observatories, LIGO/Virgo, KAGRA or ET. Amaro-Seoane 2018, Audley et.al. 2017, Huerta et.al. 2011 In particular, for IMRACs with a total mass ≤ 2000M⊙ and initial eccentricities up to 0.999 (nearly a circular orbit), the gravitational waves can be detected first by LISA one year in advance such that the ground-based observatories can get a warning. Amaro-Seoane 2018 Event rate: a few hundred per yearGair et.al 2010 The second type of IMRAC would be a very loud source in the LISA band. The GW signal may have a large signal-to-noise ratio (SNR) and can be detectable during the end of inspiral without the need for matched filteringMiller et.al. 2004. Event rate: a few to a few hundred per year Miller et.al. 2004, Gair 2010 Analytic and numerical studies are highly expected

GW from IMRACs Depending on their orbital parameters,IMRACs in clusters can be detectable not only by the planned space-based gravitational wave observatories,including LISA,太极/天琴，，but also by the ground-based observatories,LIGO/Virgo,KAGRA or ET.Amar-Seoane 20.Audley et.al.2017,Huerta et.al.2011 In particular,for IMRACs with a total mass 2000M and initial eccentricities up to 0.999(nearly a circular orbit),the gravitational waves can be detected first by LISA one year in advance such that the ground-based observatories can get a warning.Amaro-seone0 Event rate:a few hundred per yeardair et.a 2010 口◆4回4三+1声，￥8C

. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . GW from IMRACs Depending on their orbital parameters, IMRACs in clusters can be detectable not only by the planned space-based gravitational wave observatories, including LISA, 太极/天琴,..., but also by the ground-based observatories, LIGO/Virgo, KAGRA or ET. Amaro-Seoane 2018, Audley et.al. 2017, Huerta et.al. 2011 In particular, for IMRACs with a total mass ≤ 2000M⊙ and initial eccentricities up to 0.999 (nearly a circular orbit), the gravitational waves can be detected first by LISA one year in advance such that the ground-based observatories can get a warning. Amaro-Seoane 2018 Event rate: a few hundred per yearGair et.al 2010 The second type of IMRAC would be a very loud source in the LISA band. The GW signal may have a large signal-to-noise ratio (SNR) and can be detectable during the end of inspiral without the need for matched filteringMiller et.al. 2004. Event rate: a few to a few hundred per year Miller et.al. 2004, Gair 2010 Analytic and numerical studies are highly expected

GW from IMRACs Depending on their orbital parameters,IMRACs in clusters can be detectable not only by the planned space-based gravitational wave observatories,including LISA,太极/天琴，，but also by the ground-based observatories,LIGO/Virgo,KAGRA or ET.AmaSeoane 20.Audley et.al.2017,Huerta et.al.2011 In particular,for IMRACs with a total mass 2000Mo and initial eccentricities up to 0.999(nearly a circular orbit).the gravitational waves can be detected first by LISA one year in advance such that the ground-based observatories can get a warning.Amaro-seone0 Event rate:a few hundred per yearcalr t 2010 The second type of IMRAC would be a very loud source in the LISA band.The GW signal may have a large signal-to-noise ratio(SNR)and can be detectable during the end of inspiral without the need for matched filteringer200. Event rate:a few to a few hundred per year Miller eta 2004.Gair 2010 口卡+·三4色，在习80

. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . GW from IMRACs Depending on their orbital parameters, IMRACs in clusters can be detectable not only by the planned space-based gravitational wave observatories, including LISA, 太极/天琴,..., but also by the ground-based observatories, LIGO/Virgo, KAGRA or ET. Amaro-Seoane 2018, Audley et.al. 2017, Huerta et.al. 2011 In particular, for IMRACs with a total mass ≤ 2000M⊙ and initial eccentricities up to 0.999 (nearly a circular orbit), the gravitational waves can be detected first by LISA one year in advance such that the ground-based observatories can get a warning. Amaro-Seoane 2018 Event rate: a few hundred per yearGair et.al 2010 The second type of IMRAC would be a very loud source in the LISA band. The GW signal may have a large signal-to-noise ratio (SNR) and can be detectable during the end of inspiral without the need for matched filteringMiller et.al. 2004. Event rate: a few to a few hundred per year Miller et.al. 2004, Gair 2010 Analytic and numerical studies are highly expected

GW from IMRACs Depending on their orbital parameters,IMRACs in clusters can be detectable not only by the planned space-based gravitational wave observatories,including LISA,太极/天琴，，but also by the ground-based observatories,LIGO/Virgo,KAGRA or ET.Amar-Seoane 20.Audley et.al.2017,Huerta et.al.2011 In particular,for IMRACs with a total mass 2000M and initial eccentricities up to 0.999(nearly a circular orbit),the gravitational waves can be detected first by LISA one year in advance such that the ground-based observatories can get a warning.Amaso Event rate:a few hundred per yeardalr et2010 The second type of IMRAC would be a very loud source in the LISA band.The GW signal may have a large signal-to-noise ratio(SNR)and can be detectable during the end of inspiral without the need for matched filteringmaer etaL 2004. Event rate:a few to a few hundred per year Mler.r0 Analytic and numerical studies are highly expected.... 4口◆4回4三+1声，￥)QC

. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . GW from IMRACs Depending on their orbital parameters, IMRACs in clusters can be detectable not only by the planned space-based gravitational wave observatories, including LISA, 太极/天琴,..., but also by the ground-based observatories, LIGO/Virgo, KAGRA or ET. Amaro-Seoane 2018, Audley et.al. 2017, Huerta et.al. 2011 In particular, for IMRACs with a total mass ≤ 2000M⊙ and initial eccentricities up to 0.999 (nearly a circular orbit), the gravitational waves can be detected first by LISA one year in advance such that the ground-based observatories can get a warning. Amaro-Seoane 2018 Event rate: a few hundred per yearGair et.al 2010 The second type of IMRAC would be a very loud source in the LISA band. The GW signal may have a large signal-to-noise ratio (SNR) and can be detectable during the end of inspiral without the need for matched filteringMiller et.al. 2004. Event rate: a few to a few hundred per year Miller et.al. 2004, Gair 2010 Analytic and numerical studies are highly expected

Numerical study For comparable mass binary systems,the inspiral phase could be well modeled by post-Newtonian(PN)theory and numerical relativity. 口卡4三色至习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?

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) 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?