Spectrum of shear modes in the neutron-star crust: Estimating the nuclear-physics uncertainties

Tews, Ingo

doi:10.1103/physrevc.95.015803

Cited by 52 publications

(49 citation statements)

References 83 publications

(187 reference statements)

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“…To obtain the neutron-star equations of state, we extend our models to β equilibrium and include a crust, as described in Refs. [22,28]. These different prescriptions show excellent agreement, see Figs.…”

Section: Neutron-star Equation Of Statesupporting

confidence: 58%

Critical examination of constraints on the equation of state of dense matter obtained from GW170817

2018

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The correlation of the tidal polarizabilities Λ1-Λ2 for GW170817 is predicted by combining densematter equations of state (EOSs) that satisfy nuclear physics constraints with the chirp mass and mass asymmetry for this event. Our models are constrained by calculations of the neutron-matter EOS using chiral effective field theory Hamiltonians with reliable error estimates up to once or twice the nuclear saturation density. In the latter case, we find that GW170817 does not improve our understanding of the EOS. We contrast two distinct extrapolations to higher density: a minimal model (MM) which assumes that the EOS is a smooth function of density described by a Taylor expansion and a more general model parametrized by the speed of sound that admits phase transitions. This allows us to identify regions in the Λ1-Λ2 plots that could favor the existence of new phases of matter in neutron stars. We predict the combined tidal polarizability of the two neutron stars in GW170817 to be 80 ≤Λ ≤ 580 (280 ≤Λ ≤ 480 for the MM), which is smaller than the range suggested by the LIGO-Virgo data analysis. Our analysis also shows that GW170817 requires a NS with M = 1.4M to have a radius 9.0 < R1.4 < 13.6 km (11.3 < R1.4 < 13.6 km for the MM). *

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Section: Neutron-star Equation Of Statesupporting

confidence: 58%

Critical examination of constraints on the equation of state of dense matter obtained from GW170817

2018

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“…Starting from the pure neutron matter calculations, we construct the neutronstar EOS up to n tr by constructing a crust as described in Ref. [46] and extending the neutron-matter results to β equilibrium above the crust-core transition. Having constructed the EOS up to n tr we compute the speed of sound,…”

Section: The Maximal Modelmentioning

confidence: 99%

Confronting gravitational-wave observations with modern nuclear physics constraints

2019

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Multi-messenger observations of neutron star (NS) mergers have the potential to revolutionize nuclear astrophysics. They will improve our understanding of nucleosynthesis, provide insights about the equation of state (EOS) of strongly-interacting matter at high densities, and enable tests of the theory of gravity and of dark matter. Here, we focus on the EOS, where both gravitational waves (GWs) from neutron-star mergers and X-ray observations from space-based detectors such as NICER will provide more stringent constraints on the structure of neutron stars. Furthermore, recent advances in nuclear theory have enabled reliable calculations of the EOS at low densities using effective field theory based Hamiltonians and advanced techniques to solve the quantum many-body problem. In this paper, we address how the first observation of GWs from GW170817 can be combined with modern calculations of the EOS to extract useful insights about the EOS of matter encountered inside neutron stars. We analyze the impact of various uncertainties, the role of phase transitions in the NS core, and discuss how future observations will improve our understanding of dense matter.PACS. 26.60.Kp Equations of state of neutron-star matter -26.60.-c Nuclear matter aspects of neutron stars arXiv:1901.09874v2 [nucl-th]

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“…Refs. [150,151,152,153,154,155,156,157] for recent calculations). In this approach, the nuclear clusters and the neutron liquid are considered as two distinct homogeneous phases.…”

Section: Nonaccreted Neutron Starsmentioning

confidence: 99%

Phases of Dense Matter in Compact Stars

Blaschke

Chamel

2018

The Physics and Astrophysics of Neutron Stars

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Formed in the aftermath of gravitational core-collapse supernova explosions, neutron stars are unique cosmic laboratories for probing the properties of matter under extreme conditions that cannot be reproduced in terrestrial laboratories. The interior of a neutron star, endowed with the highest magnetic fields known and with densities spanning about ten orders of magnitude from the surface to the centre, is predicted to exhibit various phases of dense strongly interacting matter, whose physics is reviewed in this chapter. The outer layers of a neutron star consist of a solid nuclear crust, permeated by a neutron ocean in its densest region, possibly on top of a nuclear "pasta" mantle. The properties of these layers and of the homogeneous isospin asymmetric nuclear matter beneath constituting the outer core may still be constrained by terrestrial experiments. The inner core of highly degenerate, strongly interacting matter poses a few puzzles and questions which are reviewed here together with perspectives for their resolution. Consequences of the dense-matter phases for observables such the neutron-star mass-radius relationship and the prospects to uncover their structure with modern observational programmes are touched upon.

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Spectrum of shear modes in the neutron-star crust: Estimating the nuclear-physics uncertainties

Cited by 52 publications

References 83 publications

Critical examination of constraints on the equation of state of dense matter obtained from GW170817

Critical examination of constraints on the equation of state of dense matter obtained from GW170817

Confronting gravitational-wave observations with modern nuclear physics constraints

Phases of Dense Matter in Compact Stars

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