One of the major uncertainties in dense matter equation state has been nuclear symmetry energy. The density dependence energy is important astrophysics, as it controls neutronization core-collapse supernovae, radii neutron stars and thicknesses their crusts, rate cooling stars, properties nuclei involved r-process nucleosynthesis. We show that fits masses to experimental masses, combined with other information from skins, heavy ion collisions, giant dipole resonances, polarizabilities, lead...

We confront observational data from gravitational wave event GW170817 with microscopic modeling of the cold neutron star equation state. develop and employ a Bayesian statistical framework that enables us to implement constraints on state laboratory measurements nuclei state-of-the-art chiral effective field theory methods. The energy density functionals constructed posterior probability distributions are then used compute consistently outer crust inner core, assuming composition consisting...

We investigate the nuclear symmetry energy and neutron star properties using a Bayesian analysis based on constraints from different chiral effective field theory calculations new density functionals that allow for large variations at high densities. Constraints densities are included observations of GW170817 NICER. In particular, we show both NICER analyses lead to very similar posterior results when folded into our equation-of-state framework. Using posteriors, provide slope parameter, as...

We investigate the structure of neutron star crusts, including crust-core boundary, based on new Skyrme mean field models constrained by bulk-matter equation state from chiral effective theory and ground-state energies doubly-magic nuclei. Nuclear pasta phases are studied using both liquid drop model as well Thomas-Fermi approximation. compare energy per nucleon for each geometry (spherical nuclei, cylindrical nuclear slabs, holes, spherical holes) to obtain ground phase a function density....

The explicit density (rho) dependence in the coupling coefficients of non-relativistic nuclear energy-density functional (EDF) encodes effects three-nucleon forces and dynamical correlations. necessity for a coefficient form small fractional power rho is empirical often chosen arbitrarily. Consequently, precision-oriented parameterisations risk overfitting loss predictive power. Observing that Fermi momentum kF~rho^1/3 key variable systems, we examine if hierarchy kF can be inferred from...

From general Fermi liquid theory arguments, we derive correlations among the symmetry energy (J), its slope parameter (L), and curvature (Ksym) at nuclear matter saturation density. We argue that certain properties of these do not depend on details forces used in calculation. as well a global parametrization density dependence show is more reliable, especially low densities, than usual Taylor series expansion around then benchmark predictions against explicit results from chiral effective...

Motivated by the unknown nature of $2.50-2.67\,M_\odot$ compact object in binary merger event GW190814, we study maximum neutron star mass based on constraints from low-energy nuclear physics, tidal deformabilities GW170817, and simultaneous mass-radius measurements PSR J0030+045 NICER. Our prior distribution is a combination modeling valid vicinity normal densities together with assumption maximally stiff equation state at high densities, choice that enables us to probe connection between...

Recent experimental and ab initio theory investigations of the 208Pb neutron skin thickness have potential to inform star equation state. In particular, strong correlation between pressure matter at normal nuclear densities leads modified predictions for radii, tidal deformabilities, moments inertia typical 1.4M⊙ stars. present work, we study relative impact these recent analyses on bulk properties stars within a Bayesian statistical analysis. Two models state prior are employed in order...

We propose two novel constraints for the theoretical corrections to Gamow-Teller transition rates. The first, derived from a two-level model, predicts forbidden regions within plane defined by isospin-mixing correction 𝛿𝐶⁢1 and ratio 𝜂 of isospin-symmetry matrix elements between upper lower admixed states. It serves as filter calculations, particularly effective small values |𝜂|. other employs experimental 𝑓⁡𝑡 values, incorporating states, exploits mirror symmetry eliminate isospin-invariant...

We investigate nuclear matter equations of state in neutron star with kaon condensation. It is generally known that the existence kaons makes equation soft so maximum mass not likely to be greater than 2.0 $M_{\odot}$, constrained by current observations. With existing Skyrme force model parameters, we calculate and check possibility condensation core stars. The results show even condensation, satisfies both allowed ranges radius.

We formulate microscopic optical potentials for nucleon-nucleus scattering from chiral two- and three-nucleon forces. The real imaginary central terms of the are obtained nucleon self-energy in infinite nuclear matter at a given density isospin asymmetry, calculated self-consistently to second order many-body perturbation theory. spin-orbit term is extracted same potential using an improved matrix expansion. density-dependent then folded with distributions $^{40,42,44,48}\mathrm{Ca}$ which...

We investigate neutron star moments of inertia from Bayesian posterior probability distributions the nuclear equation state that incorporate information microscopic many-body theory and empirical data finite nuclei. focus on PSR J0737-3039A predict for this 1.338 M_sun moment lies in range $1.04 \times 10^{45}$ g cm$^{2} < I 1.51 cm$^{2}$ at 95% credibility level, while most probable value is $\tilde = 1.36 cm$^{2}$. Assuming a measurement to 10% precision, we study implications radii tidal...

We develop for the first time a microscopic global nucleon-nucleus optical potential with quantified uncertainties suitable analyzing nuclear reaction experiments at next-generation rare-isotope beam facilities. Within improved local density approximation and without any adjustable parameters, we begin by computing proton-nucleus neutron-nucleus potentials from set of five forces chiral effective field theory 1800 target nuclei in mass range 12≤A≤242 energies between 0 MeV<E≲150 MeV. then...

The effects of nuclear isospin asymmetry on $\alpha$ decay lifetimes heavy nuclei are investigated within various phenomenological models potential for the particle. We consider widely used simple square well and Woods-Saxon potential, modify them by including an term. then suggest a model particle motivated microscopic approach Skyrme force model, which naturally introduce dependent form empirical lifetime formula Viola Seaborg is also modified to include effects. obtained half-lives in...

We construct a new Skyrme interaction Skχm⁎ by fitting the equation of state and nucleon effective masses in asymmetric nuclear matter from chiral two- three-body forces as well binding energies finite nuclei. Employing this to study electric dipole polarizabilities 48Ca, 68Ni, 120Sn, 208Pb random-phase approximation, we find that theoretical predictions are good agreement with experimentally measured values without additional fine tuning interaction, thus confirming usefulness studying...

We investigate spherical proton emitters in the region from I $(Z=53)$ to Bi $(Z=83)$ isotopes as a crucial application of relativistic energy density functional PC-PK1 beyond drip line. The continuum effect is treated carefully by using Hartree-Bogoliubov theory. calculate half-lives Wentzel-Kramers-Brillouin (WKB) method and observe that calculated values are reasonable agreement with experimental results for most considered this study. also discuss clue improve future.

We consider the so called hyperon puzzle of neutron star (NS). employ Skyrme force models for description in-medium nucleon-nucleon, nucleon-Lambda ($N\Lambda$), and Lambda-Lambda ($\Lambda\Lambda$) interactions. A phenomenological finite-range $\Lambda\Lambda$ interaction is considered as well. Equation state (EoS) NS matter obtained in framework density functional theory, Tolman-Oppenheimer-Volkoff equations are solved to obtain mass-radius relations NSs. It has been generally known that...

In this paper, we investigate the cooling of neutron stars with relativistic and nonrelativistic models dense nuclear matter. We focus on effects uncertainties originated from models, composition elements in envelope region, formation superfluidity core crust stars. Discovery [Formula: see text] PSR J1614−2230 J0343[Formula: text]0432 has triggered revival stiff equation state at high densities. meantime, observation a star Cassiopeia A for more than 10 years provided us very accurate data...

We investigate the constraints on mass and radius of neutron stars by considering tidal deformability in merge star binaries. employ models based Skyrme force density-functional theory select that are consistent with empirical data finite nuclei, measured properties nuclear matter around saturation density, observation maximum stars. From selected models, we calculate Love number ${k}_{2}$, dimensionless $\mathrm{\ensuremath{\Lambda}}$, mass-weighted $\stackrel{\ifmmode \tilde{}\else...

We examine the role of hyperons in a neutron star based on relativistic mean field approach. For nuclear matter below 1.5 times normal density we constrain model parameters by using symmetric properties and theoretical investigations for literature. then extend to higher densities including isoscalar vector mesons that contain strangeness degree freedom. confirm $\phi$ meson induces $\Lambda$ repulsive force hardens equation state. The hardening arising from compensates softening existence...

We formulate microscopic neutron-nucleus optical potentials from many-body perturbation theory based on chiral two- and three-body forces. The neutron self-energy is first calculated in homogeneous matter to second order theory, which gives the central real imaginary terms of potential. spin-orbit term separately density matrix expansion using same interaction as self-energy. Finally, full potential derived within improved local approximation utilizing mean-field models consistent with...