Three body first post-Newtonian effects on the secular dynamics of a compact binary near a spinning supermassive black hole

Fang, Yun; Huang, Qing-Guo

doi:10.1103/physrevd.102.104002

Cited by 16 publications

(13 citation statements)

References 62 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We address these complications by following the method of near-identity transformations [38], which allows to consistently implement the averaging procedure to any order of accuracy. While several authors already studied quadrupolar couplings at 1PN order [9,31,32,34,[39][40][41][42], we are aware of only three which took into account these deviations from the adiabatic approximation [31][32][33][34]. However, we believe that we give in this work the first complete expressions of quadrupolar 1PN terms.…”

mentioning

confidence: 90%

Effective two-body approach to the hierarchical three-body problem

2021

View full text Add to dashboard Cite

Many binary systems of interest for gravitational-wave astronomy are orbited by a third distant body, which can considerably alter their relativistic dynamics. Precision computations are needed to understand the interplay between relativistic corrections and three-body interactions. We use an effective field theory approach to derive the effective action describing the long time-scale dynamics of hierarchical three-body systems up to 1PN quadrupole order. At this level of approximation, computations are complicated by the backreaction of small oscillations on orbital time-scales as well as deviations from the adiabatic approximation. We address these difficulties by eliminating the fast modes through the method of near-identity transformations. This allows us to compute for the first time the complete expression of the 1PN quadrupole cross-terms in generic configurations of three-body systems. We numerically integrate the resulting equations of motion and show that 1PN quadrupole terms can affect the long term dynamics of relativistic three-body systems.

show abstract

mentioning

confidence: 90%

Effective two-body approach to the hierarchical three-body problem

2021

View full text Add to dashboard Cite

show abstract

“…We generate the waveform for the XMRIs using a code based on Barack & Cutler (2004) and Fang & Huang (2020) expanding the rate of change of the orbital frequency and eccentricity to 2.5 post-Newtonian (PN) order while considering the effect of the spin of the SMBH through the pericentre precession and the Lense-Thirring precession to effectively 1.5 PN order. Restricting our analysis to lower PN orders reduces the computational costs and allows us to include a higher number of modes which is crucial due to the high eccentricity of the orbit and the sensitivity of space-based detectors (Amaro-Seoane et al 2017;Luo et al 2016).…”

Section: Measuring the Spin And Mass Of Sgra *mentioning

confidence: 99%

SgrA$^{*}$ spin and mass estimates through the detection of an extremely large mass-ratio inspiral

Vazquez-Aceves¹,

Lin²,

Torres-Orjuela³

2022

Preprint

View full text Add to dashboard Cite

Estimating the spin of SgrA * is one of the current challenges we face in understanding the center of our Galaxy. In the present work, we show that detecting the gravitational waves (GWs) emitted by a brown dwarf inspiraling around SgrA * will allow us to measure the mass and the spin of SgrA * with unprecedented accuracy. Such systems are known as extremely large mass-ratio inspirals (XMRIs) and are expected to be abundant and loud sources in our galactic center. We consider XMRIs with a fixed orbital inclination and two scenarios for SgrA * 's spin (𝑠): A highly spinning scenario where 𝑠=0.9 and a low spinning scenario where 𝑠=0.1. For both cases, we obtain the number of circular and eccentric XMRIs expected to be detected by space-borne GW detectors like LISA and TianQin. We later perform a Fisher matrix analysis to show that by detecting a single XMRI the mass of SgrA * can be determined with an accuracy ranging from 0.06 to 3 solar masses while the spin can be measured with an accuracy between 1.5×10 −7 and 4×10 −4 .

show abstract

“…• t PN ∼ t KL : The quadrupolar force has an equivalent strength to PN effects. Several interesting behaviors can emerge from the non-trivial interplay between quadrupolar and PN terms [27,[34][35][36][37][38][39][40][41] • t PN t KL : PN terms dominate the evolution. This suppresses greatly the magnitude of KL oscillations, so that the outer orbit cannot induce sizeable changes in the eccentricity of the inner orbit [24][25][26].…”

Section: Resonant Hierarchical Systemsmentioning

confidence: 99%

Precession resonances in hierarchical triple systems

Kuntz

2021

Preprint

View full text Add to dashboard Cite

We describe a new kind of resonance occuring in relativistic three-body hierarchical systems: the precession resonance, occuring when the relativistic precession timescale of a binary equals the period of a distant perturber. We find that, contrary to what most previous studies assume, it can lead to an exponential increase of eccentricity of the binary even when relativistic precession dominates the quadrupolar perturbation. The resonance may happen in the observation band of LISA or change the eccentricity distribution of triples. We discuss the physics of the resonance, showing that it mainly depends on three parameters.

show abstract

Three body first post-Newtonian effects on the secular dynamics of a compact binary near a spinning supermassive black hole

Cited by 16 publications

References 62 publications

Effective two-body approach to the hierarchical three-body problem

Effective two-body approach to the hierarchical three-body problem

SgrA$^{*}$ spin and mass estimates through the detection of an extremely large mass-ratio inspiral

Precession resonances in hierarchical triple systems

Contact Info

Product

Resources

About