English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT

Released

Journal Article

Gravitomagnetic tidal effects in gravitational waves from neutron star binaries

MPS-Authors
/persons/resource/persons192129

Vines,  J.
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

External Resource
No external resources are shared
Fulltext (public)

1805.07266.pdf
(Preprint), 392KB

PhysRevD.101.064003.pdf
(Publisher version), 346KB

Supplementary Material (public)
There is no public supplementary material available
Citation

Banihashemi, B., & Vines, J. (2020). Gravitomagnetic tidal effects in gravitational waves from neutron star binaries. Physical Review D, 101: 064003. doi:10.1103/PhysRevD.101.064003.


Cite as: http://hdl.handle.net/21.11116/0000-0001-838D-C
Abstract
Gravitational waves emitted by coalescing binary systems containing neutron stars (or other compact objects) carry signatures of the stars' internal equation of state, notably, through the influence of tidal deformations during the binary's inspiral stage. While the leading-order tidal effects for post-Newtonian binaries of compact bodies in general relativity are due to the bodies' mass-quadrupole moments induced by gravitoelectric tidal fields, we consider here the leading effects due to current-quadrupole moments induced by gravitomagnetic tidal fields. We employ an effective action approach to determine the near-zone gravitational field and the conservative orbital dynamics, initially allowing for arbitrary (not just tidally induced) current-quadrupoles; our approach significantly reduces the complexity of the calculation compared to previous derivations of the conservative dynamics for arbitrary multipoles. We finally compute the leading contributions from gravitomagnetic tides to the phase and (for the first time) the mode amplitudes of the gravitational waves from a quasi-circular binary inspiral, given in terms of the bodies' quadrupolar gravitomagnetic tidal Love numbers (tidal linear response coefficients in an adiabatic approximation). In the phase, gravitomagnetic tides are suppressed by one post-Newtonian order relative to gravitoelectric ones, but this is not always the case for the mode amplitudes. In the $(\ell,|m|)=(2,1)$ and $(3,2)$ modes for example, they appear at the same leading orders.