Nuclear Mass Dependence of Chaotic Dynamics in Ginocchio Model

The chaotic dynamics in nuclear collective motion is studied in the framework of a schematic shell model which has only monopole and quadrupole degrees of freedom. The model is shown to reproduce the experimentally observed global trend toward less chaotic motion in heavier nuclei. The relation between current approach and the earlier studies with bosonic models is discussed.Comment: 11 Page REVTeX file, 2 postscript figures, uuencode

Quantum Level Statistics of Gaussian Ensembles in One-Dimensional Conservative System(2) Equilibrium and nonequilibrium statistical mechanics in systems showing chaos and quantum chaos, Chaos and Nonlinear Dynamics in Quantum-Mechanical and Macroscopic Systems)

この論文は国立情報学研究所の電子図書館事業により電子化されました。ガウス不変集団に従う量子エネルギー準位統計を持つ一次元保存系を数値的に研究した。一次元保存系は可積分であることが証明されている。一方、カオス系の固有値を充分多数有限個持つようなポテンシャルを数値的には構成することができることも示されている。ポテンシャルの数値的構成法として最急降下法とdressing法を採用した。ポテンシャル形状はフラクタル的となり、そのフラクタル次元は数値的に1.7と求められた

Equations of State for Hadronic Matter and Mass-Radius Relations of Neutron Stars with Strong Magnetic Fields

Neutron star is an important object for us to verify the equation of state of hadronic matter. For a specific choice of equations of state, mass and radius of a neutron star are determined, for which there are constraints from observations. According to some previous studies, since the strong magnetic field acts as a repulsive force, there is a possibility that neutron stars with strong magnetic fields may have relatively heavier masses than other non-magnetized neutron stars. In this paper, the structure of a neutron star with a strong internal magnetic field is investigated by changing its internal functional form to see how much the neutron star can be massive and also how radius of a neutron star can be within a certain range

Equations of State for Hadronic Matter and Mass-Radius Relations of Neutron Stars with Strong Magnetic Fields

Neutron star is an important object for us to verify the equation of state of hadronic matter. For a specific choice of equations of state, mass and radius of a neutron star are determined, for which there are constraints from observations. According to some previous studies, since the strong magnetic field acts as a repulsive force, there is a possibility that neutron stars with strong magnetic fields may have relatively heavier masses than other non-magnetized neutron stars. In this paper, the structure of a neutron star with a strong internal magnetic field is investigated by changing its internal functional form to see how much the neutron star can be massive and also how radius of a neutron star can be within a certain range

Symposium Symmetries in Science XIII

This book is a collection of reviews and essays about the recent developments in the area of Symmetries and applications of Group Theory. Contributions have been written mostly at the graduate level but some are accessible to advanced undergraduates. The book is of interest to a wide audience and covers a broad range of topics with a strong degree of thematical unity. The book is part of a Series of books on Symmetries in Science and may be compared to the published Proceedings of the Colloquia on Group Theoretical Methods in Physics. Here, however, prevails a distinguished character for presenting extended reviews on present applications to Science, not restricted to Theoretical Physics

/ (ǧamaʿahū wa rattabahū) Muḥammad al-Biblāwī wa-Aḥmad ad-Dīrūṭī

In arab. Schr., arab

Electric dipole moment of 199^{199}Hg atom from PP, CPCP-odd electron-nucleon interaction

International audienceWe calculate the effect of the P, CP-odd electron-nucleon interaction on the electric dipole moment of the Hg199 atom by evaluating the nuclear spin matrix elements in terms of the nuclear shell model. It is found that the neutron spin matrix element of the Hg199 nucleus is ⟨Ψ|σnz|Ψ⟩≈-0.4 with a dominant configuration of p1/2 orbital neutron. We also derive constraints on the CP phases of Higgs-doublet models, supersymmetric models, and leptoquark models from the latest experimental limit |dHg|<7.4×10-30  e cm