Isospin-rich nuclei in neutron star matter

Sil, Tapas; De, J. N.; Samaddar, S. K.; Viñas, X.; Centelles, M.; Agrawal, B. K.; Patra, S. K.

doi:10.1103/physrevc.66.045803

Cited by 26 publications

(27 citation statements)

References 26 publications

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“…Equations (24)- (27) are solved self-consistently in a WS cell of specified size R c following the method described in (Sil et al 2002) and the energy is calculated from Eq. (19).…”

Section: Self-consistent Thomas-fermi Description Of the Inner Crust mentioning

confidence: 99%

Unified equation of state for neutron stars on a microscopic basis

Sharma

Centelles

Viñas

et al. 2015

A&A

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We derive a new equation of state (EoS) for neutron stars (NS) from the outer crust to the core based on modern microscopic calculations using the Argonne v 18 potential plus three-body forces computed with the Urbana model. To deal with the inhomogeneous structures of matter in the NS crust, we use a recent nuclear energy density functional that is directly based on the same microscopic calculations, and which is able to reproduce the ground-state properties of nuclei along the periodic table. The EoS of the outer crust requires the masses of neutron-rich nuclei, which are obtained through Hartree-Fock-Bogoliubov calculations with the new functional when they are unknown experimentally. To compute the inner crust, Thomas-Fermi calculations in Wigner-Seitz cells are performed with the same functional. Existence of nuclear pasta is predicted in a range of average baryon densities between 0.067 fm −3 and 0.0825 fm −3 , where the transition to the core takes place. The NS core is computed from the new nuclear EoS assuming non-exotic constituents (core of npeμ matter). In each region of the star, we discuss the comparison of the new EoS with previous EoSs for the complete NS structure, widely used in astrophysical calculations. The new microscopically derived EoS fulfills at the same time a NS maximum mass of 2 M with a radius of 10 km, and a 1.5 M NS with a radius of 11.6 km.

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“…Equations (24)- (27) are solved self-consistently in a WS cell of specified size R c following the method described in (Sil et al 2002) and the energy is calculated from Eq. (19).…”

Section: Self-consistent Thomas-fermi Description Of the Inner Crust mentioning

confidence: 99%

Unified equation of state for neutron stars on a microscopic basis

Sharma

Centelles

Viñas

et al. 2015

A&A

Self Cite

160

195

View full text Add to dashboard Cite

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“…The total energy of an ensemble of neutrons, protons and electrons in a WS cell of volume V c is given by [3,7,14] …”

Section: Thomas-fermi Approximation To the Neutron Star Inner Crustmentioning

confidence: 99%

Pasta-phase Transitions in the Inner Crust of Neutron Stars

Viñas¹,

Gonzalez-Boquera²,

Sharma³

et al. 2017

Acta Phys. Pol. B Proc. Suppl.

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We perform calculations of nuclear pasta phases in the inner crust of neutron stars with the Thomas-Fermi method and the Compressible Liquid Drop Model using the Barcelona-Catania-Paris-Madrid (BCPM) energy density functional and several Skyrme forces. We compare the crust-core transition density estimated from the crust side with the predictions obtained from the core by using the thermodynamical and dynamical methods. Finally, the correlation between the crust-core transition density and the slope of the symmetry energy at saturation is briefly analyzed.

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“…Reactions induced by neutronrich nuclei provide invaluable information on the isospin dependence of the nuclear equation of state [6,7]. Extremely neutron-rich nuclei offer the unprecedented opportunity to extrapolate our knowledge to the properties of bulk isospin-rich matter, such as neutron stars [8,9]. The efficient production of very neutron-rich nuclides is a key issue in current and future rare isotope beam facilities around the world [10,11,12] and, in parallel, the search for new synthetic approaches is of exceptional importance.…”

mentioning

confidence: 99%

Enhanced Production of Neutron-Rich Rare Isotopes in Peripheral Collisions at Fermi Energies

et al. 2003

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A large enhancement in the production of neutron-rich projectile residues is observed in the reactions of a 25 MeV/nucleon 86 Kr beam with the neutron rich 124 Sn and 64 Ni targets relative to the predictions of the EPAX parametrization of high-energy fragmentation, as well as relative to the reaction with the less neutron-rich 112 Sn target. The data demonstrate the significant effect of the target neutron-to-proton ratio (N/Z) in peripheral collisions at Fermi energies. A hybrid model based on a deep-inelastic transfer code (DIT) followed by a statistical de-excitation code accounts for part of the observed large cross sections. The DIT simulation indicates that the production of neutron-rich nuclides in these reactions is associated with peripheral nucleon exchange in which the neutron skins of the neutron-rich 124 Sn and 64 Ni target nuclei may play an important role. From a practical viewpoint, such reactions between massive neutron-rich nuclei offer a novel synthetic avenue to access extremely neutron-rich rare isotopes towards the neutron-drip line.PACS numbers: 25.70.Hi,25.70.Lm Exploration of the nuclear landscape towards the neutron-drip line [1] is currently of great interest in order to elucidate the evolution of nuclear structure with increasing neutron-to-proton ratio (N/Z) [2,3] and understand important nucleosynthesis pathways [4], most notably the r-process [5]. Reactions induced by neutronrich nuclei provide invaluable information on the isospin dependence of the nuclear equation of state [6,7]. Extremely neutron-rich nuclei offer the unprecedented opportunity to extrapolate our knowledge to the properties of bulk isospin-rich matter, such as neutron stars [8,9]. The efficient production of very neutron-rich nuclides is a key issue in current and future rare isotope beam facilities around the world [10,11,12] and, in parallel, the search for new synthetic approaches is of exceptional importance.Neutron-rich nuclides have traditionally been produced in spallation reactions, fission, and projectile fragmentation [13]. In high-energy fragmentation reactions, the production of the most neutron-rich isotopes is based on a "clean-cut" removal of protons from the projectile. The world's data on fragmentation cross sections are well represented by the empirical parametrization EPAX [14]. EPAX is currently the common basis for predictions to plan rare beam experiments and facilities. In addition to the widely used projectile fragmentation approach, neutron-rich nuclides can be produced in multinucleon transfer reactions [15] and deep-inelastic reactions near the Coulomb barrier (e.g. [16,17,18]). In such reactions, the target N/Z significantly affects the production cross sections, but the low velocities of the fragments and the ensuing wide angular and ionic charge state distributions render practical applications rather limited. The Fermi energy regime (20-40 MeV/nucleon) [19] offers the unique opportunity to combine the advantages of both low-and high-energy reactions. At this energy, the synergy...

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Isospin-rich nuclei in neutron star matter

Cited by 26 publications

References 26 publications

Unified equation of state for neutron stars on a microscopic basis

Unified equation of state for neutron stars on a microscopic basis

Pasta-phase Transitions in the Inner Crust of Neutron Stars

Enhanced Production of Neutron-Rich Rare Isotopes in Peripheral Collisions at Fermi Energies

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