What do we learn about vector interactions from GW170817?

Dexheimer, V.; Gomes, Rosana de Oliveira; Schramm, Stefan; Pais, Helena

doi:10.1088/1361-6471/ab01f0

Cited by 84 publications

(67 citation statements)

References 102 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For the canonical star with mass 1.4 M , a corresponding radius of 14 km is found. In addition, when we consider nonlinear isovector singlet to isovector triplet coupling of the vector mesons for the baryons, the radius of the 1.4 M star reduces to less than 13 km [31]. These values of the maximum mass and radii are compatible with the expectations matured after the first detection of gravitational waves from a binary neutron-star merger (GW170817) [32; 33; 34; 35; 36; 37; 38; 39; 40].…”

Section: Equation Of Statesupporting

confidence: 71%

On the deconfinement phase transition in neutron-star mergers

et al. 2020

Self Cite

View full text Add to dashboard Cite

We study in detail the nuclear aspects of a neutron-star merger in which deconfinement to quark matter takes place. For this purpose, we make use of the Chiral Mean Field (CMF) model, an effective relativistic model that includes self-consistent chiral symmetry restoration and deconfinement to quark matter and, for this reason, predicts the existence of different degrees of freedom depending on the local density/chemical potential and temperature. We then use the out-of-chemical-equilibrium finite-temperature CMF equation of state in full general-relativistic simulations to analyze which regions of different QCD phase diagrams are probed and which conditions, such as strangeness and entropy, are generated when a strong first-order phase transition appears. We also investigate the amount of electrons present in different stages of the merger and discuss how far from chemical equilibrium they can be and, finally, draw some comparisons with matter created in supernova explosions and heavy-ion collisions.PACS. PACS-key discribing text of that key -PACS-key discribing text of that key

show abstract

Section: Equation Of Statesupporting

confidence: 71%

On the deconfinement phase transition in neutron-star mergers

et al. 2020

Self Cite

View full text Add to dashboard Cite

show abstract

“…7), astronomical observations can also be used to place constraints on the relevant parameter space. In general, since GW170817 provided an upper limit onΛ, any physical effect that results in a softening of the equation of state can be consistent with the data [88,[240][241][242][243][244][245][246] As such, a strong first-order phase transition might make an equation of state model compatible with the GW170817 data, even if the hadronic part on its own is not [152,[247][248][249][250]. A number of studies have constructed models that can successfully interpret the inspiral signal from GW170817 as the coalescence of any combination of hadronic and hybrid hadronic-quark neutron stars and place corresponding constraints on the relevant model parameter space [149,247,248,[251][252][253][254][255][256][257][258][259][260].…”

Section: Microscopic Propertiesmentioning

confidence: 57%

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

2020

View full text Add to dashboard Cite

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.

show abstract

“…This first detection shows the potential of future GW detections from binary neutron star mergers to constrain the EoS, see e.g. (De et al 2018;Dexheimer et al 2019;Capano et al 2020;Malik et al 2019;Güven et al 2020). There exists in fact a one-to-one relation between a given EoS and the tidal deformability as function of the star's mass (Hinderer et al 2010) similar to the mass-radius diagram (M-R diagram) of cold non-rotating neutron stars.…”

Section: Introductionmentioning

confidence: 64%

What can be learned from a proto-neutron star’s mass and radius?

Preau

Pascal

Novak

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We make extensive numerical studies of masses and radii of proto-neutron stars during the first second after their birth in core-collapse supernova events. We use a quasi-static approach for the computation of proto-neutron star structure, built on parameterized entropy and electron fraction profiles, that are then evolved with neutrino cooling processes. We vary the equation of state of nuclear matter, the proto-neutron star mass and the parameters of the initial profiles, to take into account our ignorance of the supernova progenitor properties. Our results suggest that if masses and radii of a proto-neutron star can be determined in the first second after the birth, e.g. from gravitational wave emission, no information could be obtained on the corresponding cold neutron star and therefore on the cold nuclear equation of state. Similarly, it seems unlikely that any property of the proto-neutron star equation of state (hot and not beta-equilibrated) could be determined either, mostly due to the lack of information on the entropy, or equivalently temperature, distribution in such objects.

show abstract

What do we learn about vector interactions from GW170817?

Cited by 84 publications

References 102 publications

On the deconfinement phase transition in neutron-star mergers

On the deconfinement phase transition in neutron-star mergers

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

What can be learned from a proto-neutron star’s mass and radius?

Contact Info

Product

Resources

About