Wen De-Hua

Noise in Genotype Selection Model

We study the steady state properties of a genotype selection model in presence of correlated Gaussian white noise. The effect of the noise on the genotype selection model is discussed. It is found that correlated noise can break the balance of gene selection and induce the phase transition which can makes us select one type gene haploid from a gene group.

R-mode Instability of Neutron Star with Non-Newtonian Gravity

The Chandrasekhar—Friedmann—Schutz (CFS) instabilities of r-modes for canonical neutron stars (1.4 M⊙) with rigid crusts are investigated by using an equation of state of asymmetric nuclear matter with super-soft symmetry energy, where the non-Newtonian gravity proposed in the grand unification theories is also considered. Constrained by the observations of the masses and the spin frequencies for neutron stars, the boundary of the r-mode instability window for a canonical neutron star is obtained, and the results show that the observed neutron stars are all outside the instability window, which is consistent with the theoretical expectation. In addition, an upper limit of the non-Newtonian gravity parameters is also given.

Structural and Spacial Characters of Neutron Star in Relativistic σ–ω Model

The analytical and numerical solutions of structure and curvature of two kinds of static spherically symmetric neutron stars are calculated. The results show that Ricci tensor and curvature scalar cannot denote the curly character of the space directly, however, to static spherically symmetric stars, these two quantities can present the relative curly degree of the space and the matter distribution to a certain extent.

Energy of Gravitational Field of Static Spherically Symmetric Neutron Stars

By using the Einstein–Tolman expression of the energy-momentum pseudo-tensor, the energy density of the gravitational field of the static spherically symmetric neutron stars is calculated in the Cartesian coordinate system. It is exciting that the energy density of gravitational field is positive and rational. The numerical results of the energy density of gravitational field of neutron stars are calculated. For neutron stars with , the ratio of the energy density of gravitational field to the energy density of pure matters would be up to 0.54 at the surface.

Softness of Nuclear Matter and the Production of Strange Particles in Neutron Stars

In the various models, we study the influences of the softness of nuclear matter, the vacuum fluctuation of nucleons and ? mesons on the production of strange particles in neutron stars. We find that the stiffer the nuclear matter is, the more easily the strange particles is produced in neutron stars. The vacuum fluctuation of nucleons has large effect on strange particle production while that of ? meson has little effect on it.

Constraints on Non-Radial Oscillation Modes by Symmetry Energy Slope

The effect of the nuclear symmetry energy slope on the non-radial oscillation f-modes in neutron stars is calculated and discussed. Based on a conservative range of the symmetry energy slope constrained by the experiment and theoretical analysis, a constraint on the frequency and damping time of the gravitational radiation from the f-mode in neutron star is obtained. It is also shown that a higher symmetry energy slope corresponds with a smaller frequency and a longer damping time. Meanwhile, a new set of parameters is given to present the universal properties of the scaled frequency and damping time.

Frame Dragging Effect on Properties of Rotating Neutron Stars with Strong Magnetic Field

The general relativistic frame dragging effect on the properties, such as the moments of inertia and the radii of gyration of fast rotating neutron stars with a uniform strong magnetic field, is calculated accurate to the first order in the uniform angular velocity. The results show that compared with the corresponding non-rotating static spherical symmetric neutron star with a weaker magnetic field, a fast rotating neutron star (millisecond pulsar) with a stronger magnetic field has a relative smaller moment of inertia and radius of gyration.

Properties of Rotating Neutron Stars in the Relativistic σ-ω Model

The properties such as the moment of inertia, the surface redshift and the radius of gyration of rotating neutron stars in the relativistic σ-ω model are studied with the Hartles method. The relation between the angular velocity of the fluid relative to the local inertial frame and the uniform angular velocity relative to the infinite is calculated.

Dispersion Relation of σ Meson and Pion at Finite Nuclear Density in Chiral σ Model

The propagators of pion and sigma meson at a finite nuclear density and zero temperature are studied in chiral σ model. Their dispersion relations are calculated numerically in one-loop approximation. In order to avoid the so-called tachyon pole appearing in the one-loop propagators of pion and sigma meson, we regard the mass of sigma meson as a free parameter and adjust it to fit the nuclear saturation properties. For equal to 3075 MeV, the tachyon pole does not appear at the normal nuclear density. Thus the dispersion relation can be calculated in chiral σ model in one-loop level for the first time.

Equation of State of Nuclear Matter in Chiral σ-ω Model*

The equation of state of nuclear matter is studied in the 1-loop approximation of chiral linear σ-ω model. By introducing the density-dependent coupling constants, the problem of tachyon pole in the chiral σ-ω model is resolved. The 1-loop contributions of σ and π mesons to the nucleons binding energy are included, while the empirical properties of nuclear matter such as saturation density, binding energy, and incompressibility are well reproduced.