Recognition: unknown
Relativistic tidal properties of neutron stars
read the original abstract
We study the various linear responses of neutron stars to external relativistic tidal fields. We focus on three different tidal responses, associated to three different tidal coefficients: (i) a gravito-electric-type coefficient G\mu_\ell=[length]^{2\ell+1} measuring the \ell^{th}-order mass multipolar moment GM_{a_1... a_\ell} induced in a star by an external \ell^{th}-order gravito-electric tidal field G_{a_1... a_\ell}; (ii) a gravito-magnetic-type coefficient G\sigma_\ell=[length]^{2\ell+1} measuring the \ell^{th} spin multipole moment G S_{a_1... a_\ell} induced in a star by an external \ell^{th}-order gravito-magnetic tidal field H_{a_1... a_\ell}; and (iii) a dimensionless ``shape'' Love number h_\ell measuring the distortion of the shape of the surface of a star by an external \ell^{th}-order gravito-electric tidal field. All the dimensionless tidal coefficients G\mu_\ell/R^{2\ell+1}, G\sigma_\l/R^{2\ell+1} and h_\ell (where R is the radius of the star) are found to have a strong sensitivity to the value of the star's ``compactness'' c\equiv GM/(c_0^2 R) (where we indicate by c_0 the speed of light). In particular, G\mu_\l/R^{2\l+1}\sim k_\ell is found to strongly decrease, as c increases, down to a zero value as c is formally extended to the ``black-hole (BH) limit'' c^{BH}=1/2. The shape Love number h_\ell is also found to significantly decrease as c increases, though it does not vanish in the formal limit c\to c^{BH}. The formal vanishing of \mu_\ell and \sigma_\ell as c\to c^{BH} is a consequence of the no-hair properties of black holes; this suggests, but in no way proves, that the effective action describing the gravitational interactions of black holes may not need to be augmented by nonminimal worldline couplings.
This paper has not been read by Pith yet.
Forward citations
Cited by 9 Pith papers
-
Axial tidal Love numbers of black holes in matter environments
Axial tidal Love numbers for black holes in anisotropic fluid environments are derived analytically and numerically, with non-compact support density profiles producing logarithmic terms that obstruct standard tidal m...
-
Dynamical tidal Love numbers of black holes under generic perturbations: Connecting black hole perturbation theory with effective field theory
Dynamical tidal Love numbers for Kerr black holes are obtained to linear frequency order by matching EFT worldline couplings to black-hole perturbation solutions, including spin-induced mode mixing.
-
GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run
LIGO and Virgo detected 39 compact binary coalescence events in O3a, including 13 new ones, with black hole binaries up to 150 solar masses and the first significantly asymmetric mass ratios.
-
The Good, the Bad, and the Subtle: Relativistic mode sums for neutron-star tidal response
A practical relativistic mode-sum method for neutron-star tidal response is implemented, with robust f-mode agreement to direct matching but acknowledged limitations in convergence and tidal field uniqueness.
-
Tidal Response and Thermodynamics of Black Holes
A new gauge-invariant effective action computes black hole Love numbers without Regge-Wheeler methods, and these numbers determine leading thermodynamic corrections under external perturbations.
-
High-order effective-one-body tidal interactions and gravitational scattering
High-order PM tidal corrections improve EOB predictions for neutron-star gravitational scattering and lay groundwork for PM-based tidal EOB waveforms.
-
Can wormholes have vanishing Love numbers?
For a specific R=0 wormhole, the magnetic Love number for ℓ=2 vanishes to linear order in the regularization parameter under static axial gravitational perturbations.
-
Love numbers of black holes and compact objects
A pedagogical review of Love numbers and tidal responses for black holes and compact objects in general relativity and extensions.
- The Science of the Einstein Telescope
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.