Dynamical tides in neutron stars: the impact of the crust

Passamonti, Andrea; Andersson, Nils; Pnigouras, Pantelis

doi:10.1093/mnras/stab870

Cited by 27 publications

(25 citation statements)

References 33 publications

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“…With our model we can study the ordinary and superfluid fundamental modes (f-modes) and pressure modes (p-modes). In addition, as in Passamonti, Andersson and Pnigouras (2021), the presence of an elastic crust sustains shear modes (s-modes), while any sharp transition between different stellar regions produces an interface mode (i-modes). We cannot study here the gravity modes (g-modes), which are restored by buoyancy, because in superfluid stars these appear only when there is at least a third constituent, as for instance muons (see Gusakov and Kantor 2013, Kantor and Gusakov 2014and Passamonti, Andersson and Ho 2016.…”

Section: Resultsmentioning

confidence: 93%

“…It is useful to note that in Andersson and Pnigouras (2020) and Passamonti, Andersson and Pnigouras (2021) we decomposed the Love number as…”

Section: Resultsmentioning

confidence: 99%

“…We determine the mode properties by solving the linearised equations as an eigenvalue problem using multiple shooting and relaxation methods, updating the numerical code developed by Passamonti, Andersson and Pnigouras (2021) taking care of the junction conditions at the internal boundaries. The relaxation approach is used to increase the numerical ac-…”

Section: Resultsmentioning

confidence: 99%

“…The multiple shooting method provides a first guess solution for the relaxation code. More details on the numerical codes and relevant tests are provided by Passamonti, Andersson and Pnigouras (2021).…”

Section: Resultsmentioning

confidence: 99%

“…We can apply the strategy and formalism developed for single fluid stars (Passamonti, Andersson and Pnigouras 2021), the only difference being the normalisation A 2 n which is now given by Eq. ( 82).…”

Section: Mode Excitationmentioning

confidence: 99%

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Dynamical tides in superfluid neutron stars

Passamonti,

Andersson,

Pnigouras

2022

Preprint

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We study the tidal response of a superfluid neutron star in a binary system, focussing on Newtonian models with superfluid neutrons present throughout the star's core and the inner crust. Within the two-fluid formalism, we consider the main aspects that arise from the presence of different regions inside the star, with particular focus on the various interfaces. Having established the relevant theory, we determine the tidal excitation of the most relevant oscillation modes during binary inspiral. Our results suggest that superfluid physics has a negligible impact on the static tidal deformation. The overwhelming contribution to the Love number is given by, as for normal matter stars, the ordinary fundamental mode (f-mode). Strong entrainment, here described by a phenomenological expression which mimics the large effective neutron mass expected at the bottom of the crust, is shown to have significant impact on the superfluid modes, but our results for the dynamical tide are nevertheless similar to the static limit: the fundamental modes are the ones most significantly excited by the tidal interaction, with the ordinary f-mode dominating the superfluid one. We also discuss the strain built up in the star's crust during binary inspiral, showing that the superfluid f-mode may (depending on entrainment) reach the limit where the crust breaks, although it does so after the ordinary f-mode. Overall, our results suggest that the presence of superfluidity may be difficult to establish from binary neutron star gravitational-wave signals.

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Section: Resultsmentioning

confidence: 93%

“…It is useful to note that in Andersson and Pnigouras (2020) and Passamonti, Andersson and Pnigouras (2021) we decomposed the Love number as…”

Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Section: Mode Excitationmentioning

confidence: 99%

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Dynamical tides in superfluid neutron stars

Passamonti,

Andersson,

Pnigouras

2022

Preprint

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Inferring the dense nuclear matter equation of state with neutron star tides

Pnigouras

Andersson

2020

Proc. IAU

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During the late stages of a neutron star binary inspiral finite-size effects come into play, with the tidal deformability of the supranuclear density matter leaving an imprint on the gravitational-wave signal. As demonstrated in the case of GW170817—the first direct detection of gravitational waves from a neutron star binary—this can lead to strong constraints on the neutron star equation of state. As detectors become more sensitive, effects which may have a smaller influence on the neutron star tidal deformability need to be taken into consideration. Dynamical effects, such as oscillation mode resonances triggered by the orbital motion, have been shown to contribute to the tidal deformability, especially close to the neutron star coalesence. We calculate the contribution of the various stellar oscillation modes to the tidal deformability and demonstrate the (anticipated) dominance of the fundamental mode, showing what the impact of the matter composition is on the tidal deformability.

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Measuring spin in coalescing binaries of neutron stars that show double precursors

Kuan¹,

Suvorov²,

Kokkotas³

2023

A&A

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Gamma-ray bursts resulting from binary neutron-star mergers are sometimes preceded by precursor flares. These harbingers can be ignited by quasi-normal modes, excited by orbital resonances, shattering the stellar crust of one of the inspiralling stars up to ≳10 s before coalescence. In the rare case when a system displays two precursors, successive overtones of either interface modes or g modes can be responsible for the overstrainings. Since the free-mode frequencies of these overtones have an almost constant ratio, and the inertial-frame frequencies for rotating stars are shifted relative to static ones, the spin frequency of the flaring component can be constrained as a function of the equation of state, the binary mass ratio, the mode quantum numbers, and the spin-orbit misalignment angle. As a demonstration of the method, we find that the precursors of GRB090510 hint at a spin frequency range of 2 ≲ ν⋆/Hz ≲ 20 for the shattering star if we allow for an arbitrary misalignment angle, assuming ℓ = 2 g modes account for the events.

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Dynamical tides in neutron stars: the impact of the crust

Cited by 27 publications

References 33 publications

Dynamical tides in superfluid neutron stars

Dynamical tides in superfluid neutron stars

Inferring the dense nuclear matter equation of state with neutron star tides

Measuring spin in coalescing binaries of neutron stars that show double precursors

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