Hyperons in hot dense matter: what do the constraints tell us for equation of state?

Fortin, M.; Oertel, Micaela; Providência, Constança

doi:10.1017/pasa.2018.32

Cited by 59 publications

(60 citation statements)

References 73 publications

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“…A previous study of hyperon abundances at finite temperatures in Ref. [28] finds that the hyperon fraction exceeds 10 −4 at density n B /n 0 = 10 −2 for temperatures T ≥ 40 MeV. According to Fig.…”

Section: Resultsmentioning

confidence: 70%

Light clusters in dilute heavy-baryon admixed nuclear matter

Sedrakian

2020

Eur. Phys. J. A

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We study the composition of nuclear matter at sub-saturation densities, non-zero temperatures, and isospin asymmetry, under the conditions characteristic of binary neutron star mergers, stellar collapse, and low-energy heavy-ion collisions. The composition includes light clusters with mass number $$A\le 4$$ A ≤ 4 , a heavy nucleus ($$^{56}{Fe}$$ 56 Fe ), the $$\varDelta $$ Δ -resonances, the isotriplet of pions, as well as the $$\Lambda $$ Λ hyperon. The nucleonic mean-fields are computed from a zero-range density functional, whereas the pion-nucleon interactions are treated to leading order in chiral perturbation theory. We show that with increasing temperature and/or density the composition of matter shifts from light-cluster to heavy baryon dominated one, the transition taking place nearly independent of the magnitude of the isospin. Our findings highlight the importance of simultaneous treatment of light clusters and heavy baryons in the astrophysical and heavy-ion physics contexts.

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Section: Resultsmentioning

confidence: 70%

Light clusters in dilute heavy-baryon admixed nuclear matter

Sedrakian

2020

Eur. Phys. J. A

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“…The relative stability of x sΞ to the modification of the nucleonic EoS, for each considered scenario, reflects the relatively small dispersion among the considered EoS, over the subsaturation density domain explored by a hyperon bound in a nucleus. Note that a similar situation corresponds, according to [8][9][10], also to x sΛ and the explication is the same.…”

Section: B Hyperonic Eos With Calibrated Meson Couplingsmentioning

confidence: 91%

Relativistic hypernuclear compact stars with calibrated equations of state

et al. 2020

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Within the covariant density functional theory of hypernuclear matter we build a series of equations of state for hypernuclear compact stars, by calibrating the coupling constants of the Ξ-hyperon to the experimental binding energy of the single-Ξ hypernuclei 15 Ξ − C and 12 Ξ − Be. Coupling constants of the Λ-hyperon to nucleons have been calibrated on a vast collection of experimental data on single Λ-hypernuclei and we employ those values. Uncertainties on the couplings of the Σ-hyperon to nuclear matter, due to lack of experimental data, are accounted for by allowing for a wide variation of the well depth of Σ at rest in symmetric saturated nuclear matter. To account for uncertainties in the nucleonic sector at densities much larger than n 0 , a rich collection of parametrizations is employed, some of them in agreement with existing constraints from nuclear physics and astrophysics. Neutron star properties are investigated with all these calibrated equations of state. The effects of the presence of hyperons on the radius, on the tidal deformability, on the moment of inertia, and on the nucleonic direct Urca process are discussed. The sensitivity of the hyperonic direct Urca processes to uncertainties in the nucleonic and hyperonic sectors is also addressed. It is shown that the relative variations of the radius, tidal deformability and moment of inertia from the values that characterize purely nucleonic stars are linearly correlated with the strangeness fraction. The maximum radius deviation, obtained for most massive neutron stars, is ≈ 10%. The reduction of the maximum mass, triggered by nucleation of strangeness, is estimated at ≈ 15 − 20%, out of which 5% comes from insufficient information on the Σ-hyperon interactions. A total of 44 calibrated hyperonic equations of state are published as Supplemental Material.

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“…Those calculations do not lead to significant deviations in the Λf peak correlation. Also the calculations with models that include hyperonic matter [67,68,69] do not show characteristic differences compared to purely nucleonic EoSs. We thus argue that only a sufficiently strong phase transition with a strong density jump can yield such a clear, unambiguous signature of a phase transition in the GW signal of NS mergers.…”

Section: Gravitational-wave Emissionmentioning

confidence: 99%

Equation-of-state constraints and the QCD phase transition in the era of gravitational-wave astronomy

Bauswein

Bastian

Blaschke

et al. 2019

AIP Conference Proceedings

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We describe a multi-messenger interpretation of GW170817, which yields a robust lower limit on NS radii. This excludes NSs with radii smaller than about 10.7 km and thus rules out very soft nuclear matter. We stress the potential of this type of constraints when future detections become available. For instance, a very similar argumentation may yield an upper bound on the maximum mass of nonrotating NSs. We also discuss simulations of NS mergers, which undergo a first-order phase transition to quark matter. We point out a different dynamical behavior. Considering the gravitational-wave signal, we identify an unambiguous signature of the QCD phase transition in NS mergers. We show that the occurrence of quark matter through a strong first-order phase transition during merging leads to a characteristic shift of the dominant postmerger frequency. The frequency shift is indicative for a phase transition if it is compared to the postmerger frequency which is expected for purely hadronic EoS models. A very strong deviation of several 100 Hz is observed for hybrid EoSs in an otherwise tight relation between the tidal deformability and the postmerger frequency. In future events the tidal deformability will be inferred with sufficient precision from the premerger phase, while the dominant postmerger frequency can be obtained when current detectors reach a higher sensitivity in the high-frequency range within the next years. Finally, we address the potential impact of a first-order phase transition on the electromagnetic counterpart of NS mergers. Our simulations suggest that there would be no significant qualitative differences between a system undergoing a phase transition to quark matter and purely hadronic mergers. The quantitative differences are within the spread which is found between different hadronic EoS models. This implies on the one hand that GW170817 is compatible with a possible transition arXiv:1904.01306v1 [astro-ph.HE] 2 Apr 2019 to quark matter. On the other hand these considerations show that it may not be easy to identify quantitative differences between purely hadronic mergers and events in which quark matter occurs considering solely their electromagnetic counterpart or their nucleosynthesis products.

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Hyperons in hot dense matter: what do the constraints tell us for equation of state?

Cited by 59 publications

References 73 publications

Light clusters in dilute heavy-baryon admixed nuclear matter

Light clusters in dilute heavy-baryon admixed nuclear matter

Relativistic hypernuclear compact stars with calibrated equations of state

Equation-of-state constraints and the QCD phase transition in the era of gravitational-wave astronomy

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