Rotating Love: The dynamical tides of spinning Newtonian stars

Pnigouras, Pantelis; Gittins, Fabian; Nanda, Amlan; Andersson, Nils; Jones, David

doi:10.48550/arxiv.2205.07577

Cited by 2 publications

(3 citation statements)

References 149 publications

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“…In particular, recent gravitational waveform modelling developments include the dynamical tidal correction due to the excitation of NS f-modes [31,32,104,105]. Recently in [31], by considering the state of the art effective one body (EOB) model TEOBResumS, it has been shown that due to the noise dominance in the higher frequency range of GW170817, both waveform model with and without f-mode dynamics behave similarly.…”

Section: Discussionmentioning

confidence: 99%

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Impact of updated multipole Love numbers and f -Love universal relations in the context of binary neutron stars

2023

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Neutron star (NS) equation of state (EoS) insensitive relations or universal relations (UR) involving neutron star bulk properties play a crucial role in gravitational-wave astronomy. Considering a wide range of equations of state originating from (i) phenomenological relativistic mean field models, (ii) realistic EoS models based on different physical motivations, and (iii) polytropic EoSs described by spectral decomposition method, we update the EoS-insensitive relations involving NS tidal deformability (Multipole Love relation) and the UR between f-mode frequency and tidal deformability (f-Love relation). We analyze the binary neutron star (BNS) event GW170817 using the frequency domain TaylorF2 waveform model with updated universal relations and find that the additional contribution of the octupolar electric tidal parameter and quadrupolar magnetic tidal parameter or the change of multipole Love relation has no significant impact on the inferred NS properties. However, adding the f-mode dynamical phase lowers the 90% upper bound on Λ by 16-20% as well as lowers the upper bound of NSs radii by ∼500m. The combined URs (multipole Love and f-Love) developed in this work predict a higher median (also a higher 90% upper bound) for Λ by 6% and also predict higher radii for the binary components of GW170817 by 200-300m compared to the URs used previously in the literature. We further perform injection and recovery studies on simulated events with different EoSs in A+ detector configuration as well as with third generation (3G) Einstein telescope. In agreement with the literature, we find that neglecting f-mode dynamical tides can significantly bias the inferred NS properties, especially for low mass NSs. However, we also find that the impact of the URs is within statistical errors.

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Section: Discussionmentioning

confidence: 99%

“…Although we ignore the spin and eccentricity, it was suggested that spin and eccentricity further enhance the excitation of f-modes in binary [30]. However, the corrections to the f-mode dynamical tide due to spin and eccentricity are still matter of investigation and recent efforts are going on this direction [30,104,105,108].…”

Section: Discussionmentioning

confidence: 99%

Impact of updated multipole Love numbers and f -Love universal relations in the context of binary neutron stars

2023

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“…The reason is that the Keplerian orbital frequency is much smaller than the relativistic frequency c/R when the two objects are far from each other, so the orbital frequency and the frequency of the internal mode can be equal only if the frequency of the mode satisfies ω ≪ c/R. Tidal resonant excitations were first discussed in the context of ordinary polytropic stars [38], then, much later, for binaries with at least one of the companions being a neutron star [39][40][41][42][43][44][45][46][47][48][49][50][51][52][53][54]. The case in which companion is a generic compact object was discussed in [54][55][56][57].…”

Section: Introductionmentioning

confidence: 99%

Discovering Love numbers through resonance excitation during extreme mass ratio inspirals

Avitan,

Brustein,

Sherf

2024

Class. Quantum Grav.

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General Relativity predicts that black holes (BHs) do not possess an internal structure and consequently cannot be excited. This leads to a specific prediction about the waveform of gravitational waves (GWs) which they emit during a binary BH inspiral and to the vanishing of their Love numbers. However, if astrophysical BHs do possess an internal structure, their Love numbers would no longer vanish, and they could be excited during an inspiral by the transfer of orbital energy. This would affect the orbital period and lead to an observable imprint on the emitted GWs waveform. The effect is enhanced if one of the binary companions is resonantly excited. We discuss the conditions for resonant excitation of a hypothetical internal structure of BHs and calculate the phase change of the GWs waveform that is induced due to such resonant excitation during intermediate- and extreme-mass-ratio inspirals. We then relate the phase change to the electric quadrupolar Love number of the larger companion, which is resonantly excited by its smaller companion. We discuss the statistical error on measuring the Love number by LISA and show that, because of this phase change, the statistical error is small even for values of the Love number as small as 10−4 for moderate values of the spin parameter. Our results indicate that, for extreme-mass-ratio inspirals with moderate spin parameter, the Love number could be detected by LISA with an accuracy which is higher by up to two orders of magnitude than what can be achieved via tidal deformation effects. Thus, our results indicate that resonant excitation of the central BH during an extreme- or intermediate-mass-ratio inspirals is the most promising effect for putting bounds on, or detecting, non-vanishing tidal Love numbers of BHs.

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Rotating Love: The dynamical tides of spinning Newtonian stars

Cited by 2 publications

References 149 publications

Impact of updated multipole Love numbers and f -Love universal relations in the context of binary neutron stars

Impact of updated multipole Love numbers and f -Love universal relations in the context of binary neutron stars

Discovering Love numbers through resonance excitation during extreme mass ratio inspirals

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