### Abstract

We derive spin-dominated waveforms (SDW) for binary systems composed of spinning black holes with unequal masses (less than 130). Such systems could be formed by an astrophysical black hole with a smaller black hole or a neutron star companion; and typically arise for supermassive black hole encounters. SDW characterize the last stages of the inspiral, when the larger spin dominates over the orbital angular momentum (while the spin of the smaller companion can be neglected). They emerge as a double expansion in the post-Newtonian parameter ε and the ratio ξ of the orbital angular momentum and dominant spin. The SDW amplitudes are presented to (ε3 ^{/}2,ξ) orders, while the phase of the gravitational waves to (ε2,ξ) orders (omitting the highest order mixed terms). To this accuracy the amplitude includes the (leading order) spin-orbit contributions, while the phase the (leading order) spin-orbit, self-spin and mass quadrupole-monopole contributions. While the SDW hold for any mass ratio smaller than 130, lower bounds for the mass ratios are derived from the best sensitivity frequency range expected for Advanced LIGO (giving 1140), the Einstein Telescope (7×10 ^{-}4), the LAGRANGE (7×10 ^{-}7) and LISA missions (7×10 ^{-}9), respectively.

Original language | English |
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Article number | 104045 |

Journal | Physical Review D - Particles, Fields, Gravitation and Cosmology |

Volume | 86 |

Issue number | 10 |

DOIs | |

Publication status | Published - Nov 19 2012 |

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### ASJC Scopus subject areas

- Nuclear and High Energy Physics

### Cite this

**Spin-dominated waveforms for unequal mass compact binaries.** / Tápai, Márton; Keresztes, Z.; Gergely, L.

Research output: Contribution to journal › Article

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TY - JOUR

T1 - Spin-dominated waveforms for unequal mass compact binaries

AU - Tápai, Márton

AU - Keresztes, Z.

AU - Gergely, L.

PY - 2012/11/19

Y1 - 2012/11/19

N2 - We derive spin-dominated waveforms (SDW) for binary systems composed of spinning black holes with unequal masses (less than 130). Such systems could be formed by an astrophysical black hole with a smaller black hole or a neutron star companion; and typically arise for supermassive black hole encounters. SDW characterize the last stages of the inspiral, when the larger spin dominates over the orbital angular momentum (while the spin of the smaller companion can be neglected). They emerge as a double expansion in the post-Newtonian parameter ε and the ratio ξ of the orbital angular momentum and dominant spin. The SDW amplitudes are presented to (ε3 /2,ξ) orders, while the phase of the gravitational waves to (ε2,ξ) orders (omitting the highest order mixed terms). To this accuracy the amplitude includes the (leading order) spin-orbit contributions, while the phase the (leading order) spin-orbit, self-spin and mass quadrupole-monopole contributions. While the SDW hold for any mass ratio smaller than 130, lower bounds for the mass ratios are derived from the best sensitivity frequency range expected for Advanced LIGO (giving 1140), the Einstein Telescope (7×10 -4), the LAGRANGE (7×10 -7) and LISA missions (7×10 -9), respectively.

AB - We derive spin-dominated waveforms (SDW) for binary systems composed of spinning black holes with unequal masses (less than 130). Such systems could be formed by an astrophysical black hole with a smaller black hole or a neutron star companion; and typically arise for supermassive black hole encounters. SDW characterize the last stages of the inspiral, when the larger spin dominates over the orbital angular momentum (while the spin of the smaller companion can be neglected). They emerge as a double expansion in the post-Newtonian parameter ε and the ratio ξ of the orbital angular momentum and dominant spin. The SDW amplitudes are presented to (ε3 /2,ξ) orders, while the phase of the gravitational waves to (ε2,ξ) orders (omitting the highest order mixed terms). To this accuracy the amplitude includes the (leading order) spin-orbit contributions, while the phase the (leading order) spin-orbit, self-spin and mass quadrupole-monopole contributions. While the SDW hold for any mass ratio smaller than 130, lower bounds for the mass ratios are derived from the best sensitivity frequency range expected for Advanced LIGO (giving 1140), the Einstein Telescope (7×10 -4), the LAGRANGE (7×10 -7) and LISA missions (7×10 -9), respectively.

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U2 - 10.1103/PhysRevD.86.104045

DO - 10.1103/PhysRevD.86.104045

M3 - Article

AN - SCOPUS:84870205350

VL - 86

JO - Physical review D: Particles and fields

JF - Physical review D: Particles and fields

SN - 1550-7998

IS - 10

M1 - 104045

ER -