Classical and quantum wormholes with tachyon field

The wormhole equations are presented in the presence of tachyon field. Specializing at some values of ω(the ratio of pressure to energy density), we find a family of classical and quantum wormhole solutions.     

First quantum correction to entropy of Vaidya－Bonner black holes due to arbitrary spin fields

Using the improved brick-wall model, we have calculated the first quantum correction to the entropy of non-static black holes, Vaidya－Bonner black holes, due to the gravitational, electro-magnetic and neutrino fields. The result shows that both bosonic entropy and fermionic entropy are exactly proportional to the area of the event horizon. Thus, the entropy-area law still holds in such a non-static case.     

一般Kerr-Newman黑洞的Dirac粒子的Hawking蒸发

本文把极端Kerr-Newman黑洞的Dirac粒子的Hawking蒸发问题推广到一般Kerr-Newman黑洞,并在黑洞的视界附近通过适当的变换找到了静止质量不为零的Dirac方程的有物理意义的解,导出了Hawking热谱公式,从而解决了Dirac粒子在一般Kerr-Newman黑洞背景下的Hawking蒸发问题。 关键词：     

虫洞和时空的维数

本文在１０维的Ｅｉｎｓｔｅｉｎ—Ｍａｘｗｅｌｌ理论中，讨论了虫洞对时空维数的作用，发现时空拓朴结构为自发紧致的Ｓ４Ｓ４Ｓ２的几率最大，从而说明可观测宇宙为什么是４维的．     

具有O(8N+1)对称耦合标量场的量子宇宙学

本文利用Hartle和Hawking的方法讨论了具有O(8N+1)对称耦合标量场的量子宇宙学,导出了相应的Wheeler-De Witt方程,计算了宇宙波函数,所得到的宇宙波函数的物质部分解具有谐振子本征态的形式,而空间部分解是Gauss因子与一个多项式乘积,由宇宙波函数分析发现考虑了量子效应后,宇宙在α=O处出现的几率密度为零,并指出宇宙基态最可几半径为Planck长度;由宇宙波函数分析还发现在宇宙极早期有多个标量物质场的几率密度小于只有单个标量物质场的几率密度。     

同步球对称静态Yang-Mills 自对偶解和连续面分布的 ’tHooft-Polyakov磁单极

在本文中。我们得到了Yang-Mills规范场的全部同步球对称静态自对偶解。由此解我们进一步导出了磁荷连续面分布的结论。 关键词：     

具有旋量场的量子虫洞

本文利用Hawking-Page的边界条件讨论了具有费米场的量子虫洞,导出了相应的Wheeler-DeWitt方程,计算了虫洞波函数,由虫洞波函数的分析,发现虫洞在a=0处出现几率密度为零,虫洞基态最可几半径为Planck尺度.     

Planck时期宇宙的拓扑结构

本文利用Hartle-Hawking的宇宙波函数方法,讨论了Planck时期的宇宙时空拓扑结构,由所得波函数的分析,发现宇宙在Planck时期形成球拓扑与环拓扑的可能性都存在,从而表明形成单连通宇宙与多连通宇宙可能性都存在。     

Generalized Uncertainty Principle and the Quantum Entropy of Rotating Black Hole

The entropy of rotating Kerr-Newman-Kasuya black hole due to massive charged fields （bosons and fermions） is calculated by using the new equation of state density motivated by the generalized uncertainty relation. The result shows the entropy does not depend on the mass and the charge but the parameter A, the area A and the spin of the fields. Moreover, an improved approximation is provided to calculate the scalar entropy.     

Quintessence Cosmology with a Coupled Real Scalar Field

In the light of the recent observations of type Ia supernovae (SNe Ia) suggesting an accelerating Universe,we show the possibility of a coupled real scalar field to be quintessence for the source of the accelerating Universe.We derive the main equations which govern the evolution of the Universe and rewrite them with the observable quantities.Finally we point out very briefly how future observations may determine the equation of state of quintessence.