ENDF/B-VII.1 Nuclear Data for Science and Technology: Cross Sections, Covariances, Fission Product Yields and Decay Data

https://digital.library.unt.edu/ark:/67531/metadc888955/m2/1/high_res_d/900147.pdf

ENDF/B-VII.0: Next Generation Evaluated Nuclear Data Library for Nuclear Science and Technology

The authors review the present status of self-consistent mean-field (SCMF) models for describing nuclear structure and low-energy dynamics. These models are presented as effective energy-density functionals. The three most widely used variants of SCMF's based on a Skyrme energy functional, a Gogny force, and a relativistic mean-field Lagrangian are considered side by side. The crucial role of the treatment of pairing correlations is pointed out in each case. The authors discuss other related nuclear structure models and present several extensions beyond the mean-field model which are currently used. Phenomenological adjustment of the model parameters is discussed in detail. The performance quality of the SCMF model is demonstrated for a broad range of typical applications.

Self-consistent mean-field models for nuclear structure

The fourth version of the Japanese Evaluated Nuclear Data Library has been produced in cooperation with the Japanese Nuclear Data Committee. In the new library, much emphasis is placed on the impro...

https://www.tandfonline.com/doi/pdf/10.1080/18811248.2011.9711675

JENDL-4.0: A New Library for Nuclear Science and Engineering

The structure of neutron stars is considered from theoretical and observational perspectives We demonstrate an important aspect of neutron star structure: the neutron star radius is primarily determined by the behavior of the pressure of matter in the vicinity of nuclear matter equilibrium density In the event that extreme softening does not occur at these densities, the radius is virtually independent of the mass and is determined by the magnitude of the pressure For equations of state with extreme softening or those that are self-bound, the radius is more sensitive to the mass Our results show that in the absence of extreme softening, a measurement of the radius of a neutron star more accurate than about 1 km will usefully constrain the equation of state We also show that the pressure near nuclear matter density is primarily a function of the density dependence of the nuclear symmetry energy, while the nuclear incompressibility and skewness parameters play secondary roles In addition, we show that the moment of inertia and the binding energy of neutron stars, for a large class of equations of state, are nearly universal functions of the star's compactness These features can be understood by considering two analytic, yet realistic, solutions of Einstein's equations, by, respectively, Buchdahl and Tolman We deduce useful approximations for the fraction of the moment of inertia residing in the crust, which is a function of the stellar compactness and, in addition, the pressure at the core-crust interface

https://iopscience.iop.org/article/10.1086/319702/pdf

Neutron Star Structure and the Equation of State

http://cds.cern.ch/record/541349/files/9308022.pdf

Nuclear ground state masses and deformations

Using up-to-date values of nuclear radii and of the nuclear surface tension, the 1977 proximity treatment of nucleus-nucleus interaction is confronted with 113 measured fusion barriers. The $\ensuremath{\approx}4%$ overestimate of theory with respect to experiment, seen in a similiar comparison in 1981, is no longer present. The calculated proximity barriers, when applied to fusion reactions used to produce heavy elements with atomic number $Z=102$--118, suggest that the unexpectedly large cross section observed in the reaction ${}^{86}\mathrm{Kr}{+}^{208}{\stackrel{\ensuremath{\rightarrow}}{\mathrm{Pb}}}^{293}118+1n$ may be due to the sinking of the Coulomb barrier below the level of the bombarding energy. Tests of this hypothesis are suggested. Some consequences of the appearance of such ``unshielded'' reactions for very heavy systems are discussed. An Appendix supplies very accurate analytic formulas for the universal nuclear proximity force and potential functions $\ensuremath{\varphi}$ and $\ensuremath{\Phi}.$ This does away with the need to consult the tables published in 1977.

Nucleus-nucleus proximity potential and superheavy nuclei

https://escholarship.org/content/qt98j4p1j0/qt98j4p1j0.pdf?t=p0wtg3

Nuclear mass formula with a finite-range droplet model and a folded-Yukawa single-particle potential

Using the self-consistent Thomas-Fermi model from our earlier work, backed by the liquid-drop-model scaling rule for fission barriers, we have constructed a simple algebraic equation for Thomas-Fermi fission barriers. The equation is accurate for proton numbers greater than about 70 and for neutron numbers up to at least 20 units on either side of beta stability. This has made it possible to make a comprehensive comparison of the Thomas-Fermi theory with 120 measured fission barriers.

/pdf/thomas-fermi-fission-barriers-52ngifxafm.pdf

Thomas-Fermi fission barriers

We present a discussion of the equation of state of cold nuclear matter predicted by our recently completed Thomas-Fermi model. The equation is in the form of a three-term polynomial in the cube root of the density, with coefficients that are functions of the relative neutron excess \ensuremath{\delta}. The coefficients are tabulated in the range from $\ensuremath{\delta}=0$ (standard nuclear matter) to $\ensuremath{\delta}=1$ (neutron matter), making it very easy to calculate, for a given $\ensuremath{\delta}$, the pressure, compressibility, saturation binding, and any other property of the Thomas-Fermi equation of state. We discuss the empirical information concerning abnormal densities and large neutron excess that is contained in the measured values of the surface energy, surface diffuseness, and the neutron skin.

W.D. Myers

Papers

Nuclear ground state masses and deformations

Nucleus-nucleus proximity potential and superheavy nuclei

Nuclear mass formula with a finite-range droplet model and a folded-Yukawa single-particle potential

Thomas-Fermi fission barriers

Nuclear equation of state