From nuclear reactions to compact stars: a unified approach
arXiv:1404.4360 · doi:10.1140/epjp/i2014-14062-x
Abstract
An equation of state (EoS) for symmetric nuclear matter is constructed using the density dependent M3Y effective interaction and extended for isospin asymmetric nuclear matter. Theoretically obtained values of symmetric nuclear matter incompressibility, isobaric incompressibility, symmetry energy and its slope agree well with experimentally extracted values. Folded microscopic potentials using this effective interaction, whose density dependence is determined from nuclear matter calculations, provide excellent descriptions for proton, alpha and cluster radioactivities, elastic and inelastic scattering. The nuclear deformation parameters extracted from inelastic scattering of protons agree well with other available results. The high density behavior of symmetric and asymmetric nuclear matter satisfies the constraints from the observed flow data of heavy-ion collisions. The neutron star properties studied using -equilibrated neutron star matter obtained from this effective interaction for pure hadronic model agree with the recent observations of the massive compact stars such as PSR J1614-2230, but if a phase transition to quark matter is considered such agreement is no longer possible.
17 pages including 12 figures and 6 tables. To be published in Eur. Phys. J. Plus (2014) 129. arXiv admin note: substantial text overlap with arXiv:1309.6793, arXiv:1111.4617, arXiv:0707.4620, arXiv:0905.1599, arXiv:0907.5350, arXiv:nucl-th/0407001; and text overlap with arXiv:0709.0900 by other authors
References in corpus (27)
- Shapiro delay measurement of a two solar mass neutron star
- A Massive Pulsar in a Compact Relativistic Binary
- Neutron-Rich Nuclei in Heaven and Earth
- Nuclear symmetry energy probed by neutron skin thickness of nuclei
- Cold Quark Matter
- Rapid Cooling of the Neutron Star in Cassiopeia A Triggered by Neutron Superfluidity in Dense Matter
- Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
- Isotopic dependence of the giant monopole resonance in the even-A ^{112-124}Sn isotopes and the asymmetry term in nuclear incompressibility
- Higher-order effects on the incompressibility of isospin asymmetric nuclear matter
- Neutron skin thickness in droplet model with surface width dependence: indications of softness of the nuclear symmetry energy
- Incompressibility of neutron-rich matter
- Alpha decay half-lives of new superheavy elements
- Predictions of Alpha Decay Half lives of Heavy and Superheavy Elements
- Cooling rates of neutron stars and the young neutron star in the Cassiopeia A supernova remnant
- Cooling of the quasi-persistent neutron star X-ray transients KS 1731-260 and MXB 1659-29
- Search for long lived heaviest nuclei beyond the valley of stability
- The Giant Monopole Resonance in the Sn Isotopes: Why is Tin so "Fluffy"?
- Isospin Diffusion in Heavy-Ion Collisions and the Neutron Skin Thickness of Lead
- The High-Density Symmetry Energy and Direct Urca
- Nuclear Half-Lives for Alpha Radioactivity of Elements with 100 Z 130
- Alpha decay chains from element 113
- Coefficients and terms of the liquid drop model and mass formula
- Nuclear equation of state at high baryonic density and compact star constraints
- Isospin dependent properties of asymmetric nuclear matter
- The breathing-mode giant monopole resonance and the surface compressibility in the relativistic mean-field theory
- Cluster radioactivity in very heavy nuclei: a new perspective
- Isospin asymmetric nuclear matter and properties of axisymmetric neutron stars