Nonlinear-in-spin effects in effective-one-body waveform models of spin-aligned, inspiralling, neutron star binaries

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Abstract

Spinning neutron stars acquire a quadrupole moment due to their own rotation. This quadratic-in-spin, self-spin effect depends on the equation of state (EOS) and affects the orbital motion and rate of inspiral of neutron star binaries. Building upon circularized post-Newtonian results, we incorporate the EOS-dependent self-spin (or monopole-quadrupole) terms in the spin-aligned effective-one-body (EOB) waveform model TEOBResumS at next-to-next-to-leading (NNLO) order, together with other (bilinear, cubic and quartic) nonlinear-in-spin effects (at leading order, LO). We point out that the structure of the Hamiltonian of TEOBResumS is such that it already incorporates, in the binary black hole case, the recently computed [Levi and Steinhoff, arXiv:1607.04252] quartic-in-spin LO term. Using the gauge-invariant characterization of the phasing provided by the function ${Q}_{\ensuremath{\omega}}={\ensuremath{\omega}}^{2}/\stackrel{\ifmmode \dot{}\else \textperiodcentered \fi{}}{\ensuremath{\omega}}$ of $\ensuremath{\omega}=2\ensuremath{\pi}f$, where $f$ is the gravitational wave frequency, we study the EOS dependence of the self-spin effects and show that: (i) the next-to-leading order (NLO) and NNLO monopole-quadrupole corrections yield increasingly phase-accelerating effects compared to the corresponding LO contribution; (ii) the standard TaylorF2 post-Newtonian (PN) treatment of NLO (3PN) EOS-dependent self-spin effects makes their action stronger than the corresponding EOB description; (iii) the addition to the standard 3PN TaylorF2 post-Newtonian phasing description of self-spin tail effects at LO allows one to reconcile the self-spin part of the TaylorF2 PN phasing with the corresponding TEOBResumS one up to dimensionless frequencies $M\ensuremath{\omega}\ensuremath{\simeq}0.04--0.06$. Such a tail-augmented TaylorF2 approximant then yields an analytically simplified, EOB-faithful, representation of the EOS-dependent self-spin phasing that can be useful to improve current PN-based (or phenomenological) waveform models for inspiralling neutron star binaries. Finally, by generating the inspiral dynamics using the post-adiabatic approximation, incorporated in a new implementation of TEOBResumS, one finds that the computational time needed to obtain a typical waveform (including all multipoles up to $\ensuremath{\ell}=8$) from 10 Hz is of the order of 0.4 sec.

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