The Merger of Two Compact Stars: A Tool for Dense Matter Nuclear Physics

Drago, A.; Pagliara, Giuseppe; Попов, С. Б.; Traversi, Silvia; Wiktorowicz, Grzegorz

doi:10.3390/universe4030050

Cited by 15 publications

(14 citation statements)

References 100 publications

(177 reference statements)

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“…Using a similar interpretation, a relation between the radius, the maximum neutron star mass, and the threshold mass for prompt collapse of the merger remnant [293] suggests R 1.6 10.6km [220]. The arguments leading to the above constraints rely on equations of state without strong phase transitions and the possibility of hybrid quark-hadron stars [294][295][296], however, detection of further systems can provide stronger constraints or put the above expectations to the test [297].…”

Section: Multimessenger Constraintsmentioning

confidence: 93%

Neutron-star tidal deformability and equation-of-state constraints

2020

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Despite their long history and astrophysical importance, some of the key properties of neutron stars are still uncertain. The extreme conditions encountered in their interiors, involving matter of uncertain composition at extreme density and isospin asymmetry, uniquely determine the stars' macroscopic properties within General Relativity. Astrophysical constraints on those macroscopic properties, such as neutron star masses and radii, have long been used to understand the microscopic properties of the matter that forms them. In this article we discuss another astrophysically observable macroscopic property of neutron stars that can be used to study their interiors: their tidal deformation. Neutron stars, much like any other extended object with structure, are tidally deformed when under the influence of an external tidal field. In the context of coalescences of neutron stars observed through their gravitational wave emission, this deformation, quantified through a parameter termed the tidal deformability, can be measured. We discuss the role of the tidal deformability in observations of coalescing neutron stars with gravitational waves and how it can be used to probe the internal structure of Nature's most compact matter objects. Perhaps inevitably, a large portion of the discussion will be dictated by GW170817, the most informative confirmed detection of a binary neutron star coalescence with gravitational waves as of the time of writing.

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Section: Multimessenger Constraintsmentioning

confidence: 93%

Neutron-star tidal deformability and equation-of-state constraints

2020

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“…Finally, the so-called two family scenario [600,565,601,561,602] involves also quark stars, but I will describe it in the next Sect. 7.3, for convenience.…”

Section: Quark Starsmentioning

confidence: 99%

Gravitational waves from neutron star mergers and their relation to the nuclear equation of state

Baiotti

2019

Preprint

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In this article, I introduce ideas and techniques to extract information about the equation of state of matter at very high densities from gravitational waves emitted before, during and after the merger of binary neutron stars. I also review current work and results on the actual use of the first gravitational-wave observation of a neutron-star merger to set constraints on properties of such equation of state. In passing, I also touch on the possibility that what we observe in gravitational waves are not neutron stars, but something more exotic. In order to make this article more accessible, I also review the dynamics and gravitational-wave emission of neutron-star mergers in general, with focus on numerical simulations and on which representations of the equation of state are used for studies on binary systems.

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“…Therefore, a sufficiently large signal-to-noise ratio detection can be used to distinguish such corrections to the waveform to extract the EoS informations. Since the detection of GWs from a double black hole system, excitement about a double neutron stars system took place, and recent research has been performed on tidal deformation in neutron stars [26,100,[108][109][110][111][112][113][114][115][116][117][118][119][120] and also on constraining the nuclear matter EoS [26,100,[121][122][123][124][125][126][127].…”

Section: Introductionmentioning

confidence: 99%

Constraining Strangeness in Dense Matter with GW170817

Gomes

Char

Schramm

2019

ApJ

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Particles with strangeness content are predicted to populate dense matter, modifying the equation of state of matter inside neutron stars as well as their structure and evolution. In this work, we show how the modeling of strangeness content in dense matter affects the properties of isolated neutrons stars and the tidal deformation in binary systems. For describing nucleonic and hyperonic stars we use the many-body forces model (MBF) at zero temperature, including the φ mesons for the description of repulsive hyperon-hyperon interactions. Hybrid stars are modeled using the MIT Bag Model with vector interaction (vMIT) in both Gibbs and Maxwell constructions, for different values of bag constant and vector interaction couplings. A parametrization with a Maxwell construction, which gives rise to third family of compact stars (twin stars), is also investigated. We calculate the tidal contribution that adds to the post-Newtonian point-particle corrections, the associated love number for sequences of stars of different composition (nucleonic, hyperonic, hybrid and twin stars), and determine signatures of the phase transition on the gravitational waves in the accumulated phase correction during the inspirals among different scenarios for binary systems. On the light of the recent results from GW170817 and the implications for the radius of ∼ 1.4 M⊙ stars, our results show that hybrid stars can only exist if a phase transition takes place at low densities close to saturation.

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The Merger of Two Compact Stars: A Tool for Dense Matter Nuclear Physics

Cited by 15 publications

References 100 publications

Neutron-star tidal deformability and equation-of-state constraints

Neutron-star tidal deformability and equation-of-state constraints

Gravitational waves from neutron star mergers and their relation to the nuclear equation of state

Constraining Strangeness in Dense Matter with GW170817

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