Concluding Remarks: Connecting Relativistic Heavy Ion Collisions and Neutron Star Mergers by the Equation of State of Dense Hadron- and Quark Matter as signalled by Gravitational Waves

Hanauske, Matthias; Steinheimer, Jan; Bovard, Luke; Mukherjee, A.; Schramm, Stefan; Takami, Kentaro; Papenfort, Jens; Wechselberger, N.; Rezzolla, Luciano; Stöcker, H.

doi:10.1088/1742-6596/878/1/012031

Cited by 44 publications

(51 citation statements)

References 26 publications

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“…Here the specific total entropy is predicted to reach S/A ≈ 3, in accord with previous RMFcalculations [61] which also used the 1-D RRHT-scenario. The T − µ B values, T ≈ 70 MeV, µ B ≈ 1.2 GeV, with net baryon densities n B /n 0 ≈ 3, reached here in heavy ion collisions, coincide with the T − µ B values reached in binary neutron star collisions, as recent general relativistic fully 3+1-dimensional hydrodynamical calculations have confirmed [15,17] for the gravitational wave event GW170817. At these temperatures and densities, T ≈ 70 MeV and n B /n 0 ≈ 3, the RRHT model predicts that there are abut 20% of the dense matter are already transformed to quarks.…”

Section: Application To Heavy-ion Collisionssupporting

confidence: 82%

“…Astrophysical observations of compact stars, along with data from the recent gravitational-wave detection by LIGO provide an additional tool to probe the equation of state of dense nuclear and possible quark matter [12][13][14][15][16][17][18] in the region of moderate temperatures and high baryon densities, close to those as created in HIC.…”

Section: Introductionmentioning

confidence: 99%

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Equation of state for hot QCD and compact stars from a mean-field approach

et al. 2020

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The thermodynamic properties of high temperature and high density QCD-matter are explored within the Chiral SU(3)-flavor parity-doublet Polyakov-loop quark-hadron mean-field model, CMF. The quark sector of the CMF model is tuned to describe the µB = 0 thermodynamics data of lattice QCD. The resulting lines of constant physical variables as well as the baryon number susceptibilities are studied in some detail in the temperature/chemical potential plane. The CMF model predicts three consecutive transitions, the nuclear first-order liquid-vapor phase transition, chiral symmetry restoration, and the cross-over transition to a quark-dominated phase. All three phenomena are cross-over, for most of the T − µB-plane. The deviations from the free ideal hadron gas baseline at µB = 0 and T ≈ 100 − 200 MeV can be attributed to remnants of the liquid-vapor first order phase transition in nuclear matter. The chiral crossing transition determines the baryon fluctuations at much higher µB ≈ 1.5 GeV, and at even higher baryon densities µB ≈ 2.4 GeV, the behavior of fluctuations is controlled by the deconfinement cross-over. The CMF model also describe well the static properties of high µB neutron stars as well as the new neutron star merger observations. The effective EoS presented here describes simultaneously lattice QCD results at µB = 0, as well as observed physical phenomena (nuclear matter and neutron star matter) at T ∼ = 0 and high densities, µB > 1 GeV.

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Section: Application To Heavy-ion Collisionssupporting

confidence: 82%

Section: Introductionmentioning

confidence: 99%

Equation of state for hot QCD and compact stars from a mean-field approach

et al. 2020

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“…In these events, a post-merger object is formed which either evolves into a stable neutron star or collapses to a black hole, once it cannot be supported by the differential rotation. As seen in numerical simulations [2][3][4][5][6][7][8][9][10][11][12][13][14][15] event of a merger leads to significant oscillations of the postmerger remnant, which can generate observable gravitational waves.…”

Section: Introductionmentioning

confidence: 90%

Bulk viscosity of baryonic matter with trapped neutrinos

2019

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We study bulk viscosity arising from weak current Urca processes in dense baryonic matter at and beyond nuclear saturation density. We consider the temperature regime where neutrinos are trapped and therefore have non-zero chemical potential. We model the nuclear matter in a relativistic density functional approach, taking in to account the trapped neutrino component. We find that the resonant maximum of the bulk viscosity would occur at or below the neutrino trapping temperature, so in the neutrino trapped regime the bulk viscosity decreases with temperature as T −2 , this decrease being interrupted by a drop to zero at a special temperature where the proton fraction becomes density-independent and the material scale-invariant. The bulk viscosity is larger for matter with lower lepton fraction, i.e., larger isospin asymmetry. We find that bulk viscosity in the neutrinotrapped regime is smaller by several orders than in the neutrino-transparent regime, which implies that bulk viscosity in neutrino-trapped matter is probably not strong enough to affect the evolution of neutron star mergers.

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“…Without doubt, GWs from a binary compact star merger will soon be announced by the LIGO-VIRGO collaboration including an electromagnetic counterpart. 1 By analysing the power spectral density profile of the post-merger emission, the GW signal can set tight constraints on the high density regime of the equation of state (EOS) of elementary matter. The modification of the EOS due to a potential influence of a hadron-quark phase transition (HQPT) and the impact of strange quark matter on the EOS, which is currently solely probed in relativistic heavy ion collisions, might be imprinted in the post-merger phase of the emitted GW of a merging compact star binary.…”

Section: Introductionmentioning

confidence: 99%

“…The modification of the EOS due to a potential influence of a hadron-quark phase transition (HQPT) and the impact of strange quark matter on the EOS, which is currently solely probed in relativistic heavy ion collisions, might be imprinted in the post-merger phase of the emitted GW of a merging compact star binary. Hybrid star mergers represent optimal astrophysical laboratories to investigate the QCD phase structure and in addition with the observations from heavy ion collisions will possibly provide a conclusive picture on the QCD phase structure at high density and temperature [1]. Figure 1.…”

Section: Introductionmentioning

confidence: 99%

Gravitational waves from binary compact star mergers in the context of strange matter

et al. 2018

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Abstract. In this article we will focus on the appearance of the hadron-quark phase transition and the formation of strange matter in the interior region of the hypermassive neutron star and its conjunction with the spectral properties of the emitted gravitational waves (GWs). A strong hadron-quark phase transition might give rise to a mass-radius relation with a twin star shape and we will show in this article that a twin star collapse followed by a twin star oscillation is feasible. If such a twin star collapse would happen during the postmerger phase it will be imprinted in the GW-signal.

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Concluding Remarks: Connecting Relativistic Heavy Ion Collisions and Neutron Star Mergers by the Equation of State of Dense Hadron- and Quark Matter as signalled by Gravitational Waves

Cited by 44 publications

References 26 publications

Equation of state for hot QCD and compact stars from a mean-field approach

Equation of state for hot QCD and compact stars from a mean-field approach

Bulk viscosity of baryonic matter with trapped neutrinos

Gravitational waves from binary compact star mergers in the context of strange matter

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