Composition of Nuclear Matter with Light Clusters and Bose–Einstein Condensation of 
                $$\alpha $$
                
                    
                                    
                        α
                    
                
             Particles

Xin-rong, WU; Wang, Si-Bo; Sedrakian, Armen; Röpke, G.

doi:10.1007/s10909-017-1795-x

Cited by 18 publications

(16 citation statements)

References 57 publications

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“…The measured deuteron distributions are well described by simple statistical models, therefore there is no direct experimental evidence of condensation of deuterons in heavy-ion collisions. It has been also speculated that deuteron condensates can be formed in the dilute nuclear matter found in supernova and hot proto-neutron-star matter at sub-saturation densities; see for example [176,[274][275][276][277][278][279][280][281][282].…”

Section: Bcs-bec Transitionmentioning

confidence: 99%

Superfluidity in nuclear systems and neutron stars

2019

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Nuclear matter and finite nuclei exhibit the property of superfluidity by forming Cooper pairs. We review the microscopic theories and methods that are being employed to understand the basic properties of superfluid nuclear systems, with emphasis on the spatially extended matter encountered in neutron stars, supernova envelopes, and nuclear collisions. Our survey of quantum many-body methods includes techniques that employ Green functions, correlated basis functions, and Monte Carlo sampling of quantum states. With respect to empirical realizations of nucleonic and hadronic superfluids, this review is focused on progress that has been made toward quantitative understanding of their properties at the level of microscopic theories of pairing, with emphasis on the condensates that exist under conditions prevailing in neutron-star interiors. These include singlet S-wave pairing of neutrons in the inner crust, and, in the quantum fluid interior, singlet-S proton pairing and triplet coupled P -F -wave neutron pairing. Additionally, calculations of weak-interaction rates in neutron-star superfluids within the Green function formalism are examined in detail. We close with a discussion of quantum vortex states in nuclear systems and their dynamics in neutron-star superfluid interiors. PACS. 97.60.Jd Neutron stars -21.65.+f Nuclear matter -47.37.+q Hydrodynamic aspects of superfluidity; quantum fluids -67.85.+d Ultracold gases, trapped gases -74.25.Dw Superconductivity phase diagrams Contents arXiv:1802.00017v4 [nucl-th] 26 Sep 2019 emerge in the interaction part of the Hamiltonian when evaluating Eq. (5) in terms of Bogolyubov operators vanish. Such terms would account for fluctuations in the system, but are beyond the scope of the present mean-field treatment. 4 Note that the variation δ(E − µN )/δn p,↑ , with up and vp held constant, yields the quantity Ep, confirming its interpretation. Armen Sedrakian, John W. Clark: Superfluidity in nuclear systems and neutron stars 5

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Section: Bcs-bec Transitionmentioning

confidence: 99%

Superfluidity in nuclear systems and neutron stars

2019

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“…As it is seen, this reduction is larger for protons at densities belonging to the region of the outer NS crust. Although our model only considers light clusters it is worth noting that the addtional pressence of a fraction of heavier species, nuclei, is to be considered in future works as it could lead to a supression of the light bound clusters as found in [53].…”

Section: Resultsmentioning

confidence: 99%

Tetraneutron condensation in neutron rich matter

2019

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In this work we investigate the possible condensation of tetraneutron resonant states in the lower density neutron rich gas regions inside Neutron Stars (NSs). Using a relativistic density functional approach we characterize the system containing different hadronic species including, besides tetraneutrons, nucleons and a set of light clusters ( 3 He, α particles, deuterium and tritium). σ, ω and ρ mesonic fields provide the interaction in the nuclear system. We study how the tetraneutron presence could significantly impact the nucleon pairing fractions and the distribution of baryonic charge among species. For this we assume that they can be thermodynamically produced in an equilibrated medium and scan a range of coupling strengths to the mesonic fields from prescriptions based on isospin symmetry arguments. We find that tetraneutrons may appear over a range of densities belonging to the outer NS crust carrying a sizable amount of baryonic charge thus depleting the nucleon pairing fractions.

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“…It is also interesting to note that the effective mass calculated with the same parameter set leads to an approximate dispersion relation of the alpha particle, E p = E + P 2 /2M * , with the density-dependent interaction energy E given above. Applying the dispersion relation to the Bose distribution for a dilute alpha gas in neutron matter, we can estimate the transition temperature for possible Bose-Einstein condensation [27] to be…”

Section: Discussionmentioning

confidence: 99%

Quasiparticle properties of a single alpha particle in cold neutron matter

Nakano,

Iida,

Horiuchi

2020

Preprint

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Light clusters such as alpha particles and deuterons are predicted to occur in hot nuclear matter as encountered in intermediate-energy heavy-ion collisions and protoneutron stars. To examine the in-medium properties of such light clusters, we consider a much simplified system in which like an impurity, a single alpha particle is embedded in a zero-temperature, dilute gas of non-interacting neutrons. By adopting a non-selfconsistent ladder approximation for the effective interaction between the impurity and the gas, which is often used for analyses of Fermi polarons in a gas of ultracold atoms, we calculate the quasiparticle properties of the impurity, i.e., the energy shift, effective mass, quasiparticle residue, and damping rate.

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Composition of Nuclear Matter with Light Clusters and Bose–Einstein Condensation of $$\alpha $$ α Particles

Cited by 18 publications

References 57 publications

Superfluidity in nuclear systems and neutron stars

Superfluidity in nuclear systems and neutron stars

Tetraneutron condensation in neutron rich matter

Quasiparticle properties of a single alpha particle in cold neutron matter

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