Time-domain effective-one-body gravitational waveforms for coalescing compact binaries with nonprecessing spins, tides, and self-spin effects

被引：221

作者：

Nagar, Alessandro ^{[1
,2
,3
,4
]}

Bernuzzi, Sebastiano ^{[5
,6
,7
]}

Del Pozzo, Walter ^{[8
,9
]}

Riemenschneider, Gunnar ^{[3
,10
]}

Akcay, Sarp ^{[5
]}

Carullo, Gregorio ^{[8
,9
]}

Fleig, Philipp ^{[11
]}

Babak, Stanislav ^{[12
,13
]}

Tsang, Ka Wa ^{[13
]}

Colleoni, Marta ^{[14
]}

Messina, Francesco ^{[15
,16
]}

Pratten, Geraint ^{[14
]}

Radice, David ^{[17
,18
]}

Rettegno, Piero ^{[3
,10
]}

Agathos, Michalis ^{[19
]}

Fauchon-Jones, Edward ^{[20
]}

Hannam, Mark ^{[20
]}

Husa, Sascha ^{[14
]}

Dietrich, Tim ^{[13
,21
]}

Cerda-Duran, Pablo ^{[22
]}

Font, Jose A. ^{[22
,23
]}

Pannarale, Francesco ^{[20
,24
,25
]}

Schmidt, Patricia ^{[26
]}

Damour, Thibault ^{[4
]}

机构：

[1] Ctr Fermi Museo Stor Fis, I-00184 Rome, Italy

[2] Ctr Studi & Ric Enrico, I-00184 Rome, Italy

[3] INFN, Sez Torino, Via P Giuria 1, I-10125 Turin, Italy

[4] Inst Hautes Etud Sci, F-91440 Bures Sur Yvette, France

[5] Friedrich Schiller Univ Jena, Inst Theoret Phys, D-07743 Jena, Germany

[6] Ist Nazl Fis Nucl, Sez Milano Bicocca, Grp Collegato Parma, I-43124 Parma, Italy

[7] Univ Parma, Dept Math Phys & Comp Sci, I-43124 Parma, Italy

[8] Univ Pisa, Dipartimento Fis Enrico Fermi, I-56127 Pisa, Italy

[9] INFN, Sez Pisa, I-56127 Pisa, Italy

[10] Univ Torino, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy

[11] Max Planck Inst Dynam & Self Org, D-37077 Gottingen, Germany

[12] Univ Paris 07, CNRS, APC, F-75205 Paris 13, France

[13] Moscow Inst Phys & Technol, Dolgoprudnyi, Moscow Region, Russia

[14] Univ Illes Balears, IAC3 IEEC, Palma De Mallorca 07122, Spain

[15] Univ Milano Bicocca, Dipartimento Fis, Piazza Sci 3, I-20126 Milan, Italy

[16] INFN, Sez Milano Bicocca, Piazza Sci 3, I-20126 Milan, Italy

[17] Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08544 USA

[18] Inst Adv Study, 1 Einstein Dr, Princeton, NJ 08540 USA

[19] Univ Cambridge, Ctr Math Sci, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England

[20] Cardiff Univ, Sch Phys & Astron, Grav Explorat Inst, Cardiff CF24 3AA, S Glam, Wales

[21] Albert Einstein Inst, Max Planck Inst Gravitat Phys, Muhlenberg 1, D-14476 Potsdam, Germany

[22] Univ Valencia, Dept Astron & Astrofs, Doctor Moliner 50, E-46100 Valencia, Spain

[23] Univ Valencia, Astron Observ, C Catedrat Jose Beltran 2, Valencia 46980, Spain

[24] Univ Roma Sapienza, Dipartimento Fis, Piazzale A Moro 5, I-00185 Rome, Italy

[25] Sez INFN Roma1, Piazzale A Moro 5, I-00185 Rome, Italy

[26] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6525 GL Nijmegen, Netherlands

来源：

PHYSICAL REVIEW D | 2018年 / 98卷 / 10期

基金：

英国科学技术设施理事会; 欧盟地平线“2020”;

关键词：

NEUTRON-STARS;

D O I：

10.1103/PhysRevD.98.104052

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present TEOBResumS, a new effective-one-body (EOB) waveform model for nonprecessing (spin-aligned) and tidally interacting compact binaries. Spin-orbit and spin-spin effects are blended together by making use of the concept of centrifugal EOB radius. The point-mass sector through merger and ringdown is informed by numerical relativity (NR) simulations of binary black holes (BBHs) computed with the SpEC and BAM codes. An improved, NR-based phenomenological description of the postmerger waveform is developed. The tidal sector of TEOBResumS describes the dynamics of neutron star binaries up to merger and incorporates a resummed attractive potential motivated by recent advances in the post-Newtonian and gravitational self-force description of relativistic tidal interactions. Equation-of-state-dependent self-spin interactions (monopole-quadrupole effects) are incorporated in the model using leading order post-Newtonian results in a new expression of the centrifugal radius. TEOBResumS is compared to 135 SPEC and 19 BAM BBH waveforms. The maximum unfaithfulness to SPEC data (F) over bar -at design Advanced LIGO sensitivity and evaluated with total mass M with a variance of 10M(circle dot) <= M <= 200M(circle dot)-is always below 2.5 x 10(-3) except for a single outlier that grazes the 7.1 x 10(-3) level. When compared to BAM data, (F) over bar is smaller than 0.01 except for a single outlier in one of the corners of the NR-covered parameter space that reaches the 0.052 level. TEOBResumS is also compatible, up to merger, to high-end NR waveforms from binary neutron stars with spin effects and reduced initial eccentricity computed with the BAM and THC codes. The data quality of binary neutron star waveforms is assessed via rigorous convergence tests from multiple resolution runs and takes into account systematic effects estimated by using the two independent high-order NR codes. The model is designed to generate accurate templates for the analysis of LIGO-Virgo data through merger and ringdown. We demonstrate its use by analyzing the publicly available data for GW150914.

引用

页数：40

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