Hyperons in the nuclear pasta phase

Menezes, D. P.; Providência, Constança

doi:10.1103/physrevc.96.045803

Cited by 17 publications

(10 citation statements)

References 31 publications

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“…Ref. [27] finds that hyperon fraction stays below 10 −7 for temperatures up to 14 MeV in the inhomogeneous "pasta" phases of supernova matter independent of the value of Y Q , which is consistent with present results. Figures 2 and 3 show the mass fractions mass fraction X j at two fixed temperatures T = 30 MeV and T = 10 MeV and varying density.…”

Section: Resultssupporting

confidence: 92%

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: Resultssupporting

confidence: 92%

Light clusters in dilute heavy-baryon admixed nuclear matter

Sedrakian

2020

Eur. Phys. J. A

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“…In a more complete model, where light clusters and hyperons are allowed to coexist, the bump would probably disappear, and above a temperature of roughly 20 MeV, hyperons would exist at any density. In Menezes & Providência (2017), hyperon fractions have been calculated in the presence of heavy clusters. Under these conditions these fractions were always below 10 −5 .…”

Section: Hyperon Content and Thermodynamic Propertiesmentioning

confidence: 99%

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

Fortin

Oertel

Providência

2018

Publ. Astron. Soc. Aust.

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For core-collapse and neutron star merger simulations, it is important to have at hand adequate equations of state which describe the underlying dense and hot matter as realistically as possible. Here, we present two newly constructed equation of state (EoS) including the entire baryon octet. The two EoS are compatible with the main constraints coming from nuclear physics, both experimental and theoretical. Besides, one of the EoS also describes cold β-equilibrated neutron stars with a maximum mass of 2M , in agreement with recent observations. The predictions obtained with the new EoS are compared with the results obtained with DD2Y. The latter is the only presently existing EoS model containing the baryon octet which also satisfies the above constraints within the existing uncertainties. The main difference between our new EoS models and DD2Y is the harder symmetry energy of the latter. We show that the density dependence of the symmetry energy has a direct influence on the amount of strangeness inside hot and dense matter and, consequently, on thermodynamic quantities, e.g. the temperature for a given entropy per baryon. We expect that these differences affect the evolution of a protoneutron star or binary neutron star mergers. We also propose several parametrizations calibrated to Λ hypernuclei based on the DD2 and SFHo models that satisfy the two solar mass constraint.

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“…The effects of the CPI are widely investigated in many branches of physics with fairly accurate experimental corroboration [1]. Successful efforts have been made to probe more complicated contexts like entanglement [2], spacetime curvature [3][4][5], Unruh effect [6][7][8] and to check thermal and nonthermal scaling in black hole spacetime [9]. Information of background spacetime and relativistic motion of interacting systems can be extracted from modification of CPI due to them [3][4][5][6][7][8][9][10].…”

Section: Introductionmentioning

confidence: 99%

Remarks on distinguishability of Schwarzschild spacetime and thermal Minkowski spacetime using Resonance Casimir–Polder interaction

Singha

2019

Mod. Phys. Lett. A

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The response of a single-atom detector, when placed at a point outside the horizon in Schwarzschild spacetime is the same as the response of a static single-atom detector in thermal Minkowski spacetime. So one cannot distinguish Schwarzschild spacetime from thermal Minkowski spacetime by using a single-atom detector. Here we show that beyond a characteristic length scale which is proportional to the inverse of the surface gravity κ, the Resonance Casimir-Polder interaction (RCPI) between two entangled atoms is characterized by a 1/L 2 power-law decay for the Schwarzschild spacetime when the atoms are located close to the horizon. However, the RCPI between two entangled atoms is always characterized by a 1/L power-law decay for the thermal Minkowski spacetime. These two spacetimes can be distinguished therefore using RCPI.

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Hyperons in the nuclear pasta phase

Cited by 17 publications

References 31 publications

Light clusters in dilute heavy-baryon admixed nuclear matter

Light clusters in dilute heavy-baryon admixed nuclear matter

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

Remarks on distinguishability of Schwarzschild spacetime and thermal Minkowski spacetime using Resonance Casimir–Polder interaction

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