Finite-temperature effects in dynamical spacetime binary neutron star merger simulations: validation of the parametric approach

Raithel, Carolyn A.; Espino, Pedro; Paschalidis, Vasileios

doi:10.1093/mnras/stac2450

Cited by 9 publications

(2 citation statements)

References 67 publications

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“…For use in our numerical merger simulations, we extend these zero-temperature, β-equilibrium EoSs to finite-temperatures and arbitrary compositions using the framework of [64], which was recently validated in the context of merger simulations in [83].…”

Section: Discussionmentioning

confidence: 99%

Tidal Deformability Doppelgangers: I. Differentiability of gravitational waveforms for neutron stars with a low-density phase transition

Raithel¹,

Most²

2022

Preprint

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Gravitational wave detections of binary neutron star inspirals will be crucial for constraining the dense matter equation of state (EoS). Such constraints rely on the robust association of the inferred tidal deformability to the underlying EoS. Here, we demonstrate the existence of a new family of EoSs that differ by 30 in their tidal deformability curves across the entire neutron star mass range, despite differences of up to ∼ 0.45 km in radius. These "tidal deformability doppelgängers" are indiscernible with current gravitational wave detectors; however, next generation detectors and advances in nuclear theory may be able to constrain or rule out this family of EoSs.

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Section: Discussionmentioning

confidence: 99%

Tidal Deformability Doppelgangers: I. Differentiability of gravitational waveforms for neutron stars with a low-density phase transition

Raithel¹,

Most²

2022

Preprint

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“…The combination of different M and different q can alter the results quantitatively in several ways. Smaller values of both imply particularly small mass for the less-massive star, giving it both a lower mean density and a less centrally concentrated internal density profile (see Lattimer & Prakash 2007;Bauswein et al 2012;Shibata et al 2021;Raithel et al 2022). Relatively large tidal mass loss would likely follow.…”

Section: Parameter Dependencementioning

confidence: 99%

Bound Debris Expulsion from Neutron Star Merger Remnants

Zenati,

Krolik,

Werneck

et al. 2023

ApJ

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Many studies have found that neutron star mergers leave a fraction of the stars’ mass in bound orbits surrounding the resulting massive neutron star or black hole. This mass is a site of r-process nucleosynthesis and can generate a wind that contributes to a kilonova. However, comparatively little is known about the dynamics determining its mass or initial structure. Here we begin to investigate these questions, starting with the origin of the disk mass. Using tracer particle as well as discretized fluid data from numerical simulations, we identify where in the neutron stars the debris came from, the paths it takes in order to escape from the neutron stars’ interiors, and the times and locations at which its orbital properties diverge from those of neighboring fluid elements that end up remaining in the merged neutron star.

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Effects of onset of phase transition on binary neutron star mergers

Haque,

Mallick,

Thakur

2023

Monthly Notices of the Royal Astronomical Society

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Quantum Chromodynamics predicts phase transition from hadronic matter to quark matter at high density, which is highly probable in astrophysical systems like binary neutron star mergers. To explore the critical density where such phase transition can occur, we performed numerical relativity simulations of binary neutron star mergers with various masses (equal and unequal binaries). We aim to understand the effect of the onset of phase transition on the merger dynamics and gravitational wave spectra. We generated a set of equations of states by agnostically changing the onset of phase transition, having the hadronic matter part and quark matter part fixed. This particular arrangement of the equation of states explores the scenario of mergers where mixed phases of matter are achieved before or during the merger. Under these circumstances, if the matter properties with hadronic and quark degrees differ significantly, it is reflected in the stability of the final merger product for the intermediate mass binary. We performed a case study on mixed species merger, where one of the binary companions is hybrid star. If quark matter appears at low densities, we observe significant change in post-merger gravitational wave analysis in terms of higher peak frequencies and post-merger frequencies in power spectral density. We report indications expressed as spikes in phase difference plots at merger time for mixed mergers. We found that the expression of phase transition in post-merger gravitational wave signals is more significant for unequal mass binary than for equal mass binary having the same total baryonic mass.

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Finite-temperature effects in dynamical spacetime binary neutron star merger simulations: validation of the parametric approach

Cited by 9 publications

References 67 publications

Tidal Deformability Doppelgangers: I. Differentiability of gravitational waveforms for neutron stars with a low-density phase transition

Tidal Deformability Doppelgangers: I. Differentiability of gravitational waveforms for neutron stars with a low-density phase transition

Bound Debris Expulsion from Neutron Star Merger Remnants

Effects of onset of phase transition on binary neutron star mergers

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