One of the fundamental questions is that “what the matter is composed of?” In 1897, atoms are known as the basic building blocks of matter. In the year 1911, Ernest Rutherford demonstrated that when alpha particles ...One of the fundamental questions is that “what the matter is composed of?” In 1897, atoms are known as the basic building blocks of matter. In the year 1911, Ernest Rutherford demonstrated that when alpha particles are scattered on a thin gold foil that the atom is composed of mostly empty space with a dense core at its center which is called the nucleus. Thereafter, protons and neutrons were discovered. In 1956, McAllister and Hofstadter published experimental results of elastic scattering of the electrons from a hydrogen target which revealed that the proton has an internal structure. In 1964, Gell-Mann (and independently) Zweig proposed that nucleons are composed of point-like particles which are called quarks. These quarks are postulated to have spin-1/2, fractional electric charge. Combinations of different flavors of quarks yield protons and neutrons which belong to the type of particles called baryons (built up from three quarks) and mesons as (quark and an antiquark). These two groups of particles are categorized as hadrons. The quarks showed further decay properties which suggested that they have a substructure.展开更多
We study the equation of state (EOS) of symmetric nuclear and neutron matter within the framework of the Brueckner-Hartree-Fock (BHF) approach which is extended by including a density-dependent contact interaction to ...We study the equation of state (EOS) of symmetric nuclear and neutron matter within the framework of the Brueckner-Hartree-Fock (BHF) approach which is extended by including a density-dependent contact interaction to achieve the empirical saturation property of symmetric nuclear matter. This method is shown to affect significantly the nuclear matter EOS and the density dependence of nuclear symmetry energy at high densities above the normal nuclear matter density, and it is necessary for reproducing the empirical saturation property of symmetric nuclear matter in a nonrelativistic microscopic framework. Realistic nucleon-nucleon interactions which reproduce the nucleon-nucleon phase shifts are used in the present calculations.展开更多
The investigation of strongly interacting systems ranges from matter inside atomic nuclei to matter under extreme conditions in astrophysics. These systems require the introduction of nuclear forces and a systematic m...The investigation of strongly interacting systems ranges from matter inside atomic nuclei to matter under extreme conditions in astrophysics. These systems require the introduction of nuclear forces and a systematic many-body approach to solve the strong interaction particles. Understanding the behavior of infinite nuclear matter provides a path to predict the properties of neutron stars and gives insights to astrophysical phenomena. Three-nucleon forces have to be considered when studying nuclear systems, because their impact is necessary to reproduce properties of nuclei and to correctly obtain the neutron drip line. Moreover, they are needed to predict the empirical saturation properties of infinite nuclear matter. The self-consistent Green’s Function approach paves the way for an improved Ab initio analysis of nuclear matter, thereby providing the basis for the equation of state of neutron stars and supernova explosions.展开更多
文摘One of the fundamental questions is that “what the matter is composed of?” In 1897, atoms are known as the basic building blocks of matter. In the year 1911, Ernest Rutherford demonstrated that when alpha particles are scattered on a thin gold foil that the atom is composed of mostly empty space with a dense core at its center which is called the nucleus. Thereafter, protons and neutrons were discovered. In 1956, McAllister and Hofstadter published experimental results of elastic scattering of the electrons from a hydrogen target which revealed that the proton has an internal structure. In 1964, Gell-Mann (and independently) Zweig proposed that nucleons are composed of point-like particles which are called quarks. These quarks are postulated to have spin-1/2, fractional electric charge. Combinations of different flavors of quarks yield protons and neutrons which belong to the type of particles called baryons (built up from three quarks) and mesons as (quark and an antiquark). These two groups of particles are categorized as hadrons. The quarks showed further decay properties which suggested that they have a substructure.
文摘We study the equation of state (EOS) of symmetric nuclear and neutron matter within the framework of the Brueckner-Hartree-Fock (BHF) approach which is extended by including a density-dependent contact interaction to achieve the empirical saturation property of symmetric nuclear matter. This method is shown to affect significantly the nuclear matter EOS and the density dependence of nuclear symmetry energy at high densities above the normal nuclear matter density, and it is necessary for reproducing the empirical saturation property of symmetric nuclear matter in a nonrelativistic microscopic framework. Realistic nucleon-nucleon interactions which reproduce the nucleon-nucleon phase shifts are used in the present calculations.
文摘The investigation of strongly interacting systems ranges from matter inside atomic nuclei to matter under extreme conditions in astrophysics. These systems require the introduction of nuclear forces and a systematic many-body approach to solve the strong interaction particles. Understanding the behavior of infinite nuclear matter provides a path to predict the properties of neutron stars and gives insights to astrophysical phenomena. Three-nucleon forces have to be considered when studying nuclear systems, because their impact is necessary to reproduce properties of nuclei and to correctly obtain the neutron drip line. Moreover, they are needed to predict the empirical saturation properties of infinite nuclear matter. The self-consistent Green’s Function approach paves the way for an improved Ab initio analysis of nuclear matter, thereby providing the basis for the equation of state of neutron stars and supernova explosions.
