This paper uses an elegant mathematical method to calculate the orbital effects in the axisymmetric field created by the spinning mass with electric charge and a large number of magnetic monopoles. In comparison with that in the Reissner-Nordstrm (R-N) field, the correction terms caused by the spinning mass decrease the advanced effect as the revolution direction of the test particle coincides with that of the Kerr field, however, the correction terms caused by the spinning charged mass increase the advance effect as the revolution direction of the test particle coincides with that of the Kerr-Newman-Kasnya (KNK) field. Generalizing the effect in the axisymmetric field, it obtains interesting results by discussing the parameters of the celestial body, these parameters provide a feasible experimental verification of the general relativity.
The chirality-asymmetry macroscopic force mediated by light pseudoscalar particles between α-quartz and some achiral matter is studied. If this force between achiral source mass and α-quartz with some chirality is attractive, it will become repulsive when the chirality of the α-quartz crystal is changed. According to the tested limits of the coupling constant gsgp/hc < 1.5 × 10-24 at the Compton wavelength λ = 10-3 m, the force (F) between a 0.08 × 0.08 × 0.002 m3 block of α-quartz and a 0.08 × 0.08 × 0.01 m3 copper block with a separation being 0.5 × 10-3 m in between, is estimated from the published data at less than 4.64 × 10-24 N, i.e. F < 4.64 × 10-24 N.
In accordance with holographic principle, by calculating the statistical entropy of the quantum field just at the event horizon of the Garfinkle-Horowitz-Strominger dilaton black hole, the information entropy of the black hole was investigated and the Bekenstein-Hawking formula was obtained. The results show that black hole entropy is identical with the statistical entropy of the quantum field at the horizon. Using the generalized uncertainty relation, the divergence of the state density near the event horizon in usual quantum field theory was removed, and the cutoffs and the little mass approximation in the heat gas method of black hole entropy were avoided. Thus, the microstates of the massive scalar field just at the event horizon of the static dilaton black hole were studied directly and a description on holograph principle was presented. By using residue theorem, the integral difficulty in the calculation was overcome, and the information entropy and the Bekenstein-Hawking formula were obtained quantitatively. Compared with the black hole entropy from the loop quantum gravity, the consistency of methods and results of calculating black hole entropy in non-commutative quantum field theory and loop quantum gravity was investigated. By this, the gravity correction constant in the generalized uncertainty relation was suggested and the sense of holographic principle was discussed.
LIU ChengZhou Institute of Theoretical Physics, Binzhou University, Binzhou 256600, China
As one of the fitting methods, the polynomial approximation is effective to process sophisticated problem. In this paper, we employ this approach to handle the scattering of scalar field around the Schwarzschild–de Sitter black- hole. The complicated relationship between tortoise coordinate and radial coordinate is replaced by the approximate polynomial. The Schrdinger-like equation, the real boundary conditions and the polynomial approximation construct a full Sturm–Liouville type problem. Then this boundary value problem can be solved numerically for two limiting cases: the first one is the Nariai black-hole whose horizons are close to each other, the second one is the black-hole with the horizons widely separated. Compared with previous results (Brevik and Tian), the field near the event horizon and cosmological horizon can have a better description.
