Dinuclear systems in complete fusion reactions

Abstract

Formation and evolution of dinuclear systems in reactions of complete fusion are considered. Based on the dinuclear system concept, the process of compound nucleus formation is studied. Arguments confirming the validity of this concept are given. The main problems of describing the complete fusion in adi abatic approximation are listed. Calculations of evaporation residue cross sections in complete fusion reac tions leading to formation of superheavy nuclei are shown. Isotopic trends of the cross sections of heavy nuclei formation in complete fusion reactions are considered.

Close Binary Galaxies: Application to Source of Energy and Expansion in Universe

“…These energies behave differently as a function of mass asymmetry: U 1 + U 2 decreases and V increases with changing η from η = 0 to η = ±1. One should stress that the driving potentials U(η) for the di-galaxy systems look like the driving potentials for the microscopic dinuclear systems [14,15]. For the close binary star systems, the same conclusion was drawn in Refs.…”

“…Coulomb and centrifugal forces are superimposed. However, extending the methods and results from the femto-scale of microscopic nuclear physics to macroscopic binary stellar systems, we obtained that the driving potentials for the di-star systems resembles in many aspects the driving potentials for the microscopic dinuclear systems [4,5,14,15]. In the present paper, we explore the landscape of total potential energy of the close binary galaxy as a function of mass asymmetry coordinate, searching specifically for the evolution paths in the mass asymmetry coordinate and mass transfer source of the transformation of gravitational energy to other types of energy in the universe.…”

From dinuclear systems to close binary stars: Application to source of energy in the universe

“…Nuclear reactions are dominated by shortranged strong interactions, to which minor contributions of long-range (repulsive) Coulomb and centrifugal forces are superimposed. However, extending the methods and results from the femto-scale of microscopic nuclear physics to macroscopic binary stellar systems, we obtained that the driving potentials U(η) for the di-star systems looks like the driving potentials for the microscopic dinuclear systems [9][10][11].…”

“…The limits for the formation and evolution of the di-star systems were derived and analyzed. We used theoretical methods which are being applied successfully to corresponding processes in nuclear systems where mass asymmetry plays an important role as the collective coordinate governing fusion of two heavy nuclei [10,11]. Nuclear dynamics, of course, is quite different from the gravitational interactions in di-stars.…”

Production of proton-rich nuclei around Z = 84-90 in fusion-evaporation reactions

“…The structure properties of the proton-rich nuclei (PRN) associated with the fission barrier, density profiles of neutrons and protons, proton-drip line, level spectra etc would be helpful to extend the superheavy region. A number of models have been developed for understanding the formation mechanism of superheavy nuclei and heavy PRN in the fusion-evaporation reactions [7][8][9][10][11][12][13][14][15][16][17][18][19][20]. The formation of superheavy nuclei in the massive fusion reactions is hindered due to the quasifission process.…”