TY - JOUR

T1 - Eccentricity-tide coupling

T2 - Impact on binary neutron stars and extreme mass ratio inspirals

AU - Bernaldez, John Paul

AU - Datta, Sayak

PY - 2023/12/4

Y1 - 2023/12/4

N2 - We study the effect of tidal interaction between two compact bodies in an eccentric orbit. We assume the tidal fields to be static. Therefore, we ignore the dynamic tides and resonant excitations. Using the results, we find the analytical expression for the phase shift of the emitted gravitational wave. In the process, we find that in the leading order, the initial eccentricity e0 and the dimensionless tidal deformability Λ couple as ∼e0nΛ, where n is a positive number. We only focus on the dominant contribution, i.e., e02Λ. We also compute the accumulated dephasing for binary neutron star systems. We find that for optimistic values of eccentricities e0∼0.05 and Λ∼600, the accumulated dephasing is O(10-4) radian, requiring a signal-to-noise ratio ∼7000 to be observable. Therefore, these effects can be measured in binary neutron star systems with large eccentricities if the signal-to-noise ratios of the systems are also very large. Hence, in third-generation detectors, it may have an observable impact if the systems have large eccentricities. We also explore the impact of this effect on extreme mass-ratio inspirals (EMRIs). We find that even for supermassive bodies with small values of Λ∼10-3, this effect has large dephasing in EMRIs∼O(10) radian. Therefore, this effect will help in probing the nature of the supermassive bodies in an EMRI.

AB - We study the effect of tidal interaction between two compact bodies in an eccentric orbit. We assume the tidal fields to be static. Therefore, we ignore the dynamic tides and resonant excitations. Using the results, we find the analytical expression for the phase shift of the emitted gravitational wave. In the process, we find that in the leading order, the initial eccentricity e0 and the dimensionless tidal deformability Λ couple as ∼e0nΛ, where n is a positive number. We only focus on the dominant contribution, i.e., e02Λ. We also compute the accumulated dephasing for binary neutron star systems. We find that for optimistic values of eccentricities e0∼0.05 and Λ∼600, the accumulated dephasing is O(10-4) radian, requiring a signal-to-noise ratio ∼7000 to be observable. Therefore, these effects can be measured in binary neutron star systems with large eccentricities if the signal-to-noise ratios of the systems are also very large. Hence, in third-generation detectors, it may have an observable impact if the systems have large eccentricities. We also explore the impact of this effect on extreme mass-ratio inspirals (EMRIs). We find that even for supermassive bodies with small values of Λ∼10-3, this effect has large dephasing in EMRIs∼O(10) radian. Therefore, this effect will help in probing the nature of the supermassive bodies in an EMRI.

UR - http://www.scopus.com/inward/record.url?scp=85179831979&partnerID=8YFLogxK

U2 - 10.48550/arXiv.2303.01398

DO - 10.48550/arXiv.2303.01398

M3 - Article

AN - SCOPUS:85179831979

VL - 108

JO - Physical Review D

JF - Physical Review D

SN - 2470-0010

IS - 12

M1 - 124014

ER -