Brans-Dicke理论中的非Accetta真空虫洞解

给出与Ａｃｃｅｔｔａ等人所得到的完全不同的Ｂｒａｕｓ－Ｄｉｃｋｅ（B－Ｄ）理论真空虫洞解，且表明这类虫洞与所得到的其他虫洞不同，其喉的尺度是随着Ｅｕｃｌｉｄｅａｎ宇宙时间的增大而线性增大。     

EDTA－钼配合物溶剂依存性的拉曼光谱

ＥＤＴＡ－钼配合物溶剂依存性的拉曼光谱吴立新，杜菲，魏君华，宋瑞芳（吉林大学理论化学研究所，分子光谱与分子结构开放实验室长春１３００２３）ＲａｍａｎＳｐｅｃｔｒｏｓｃｏｐｉｃＳｔｕｄｙｏｆＳｏｌｖｅｎｔＤｅｐｅｎｄｅｎｃｅｏｆＥＤＴＡ－Ｍｏｌｙｂｄｅ...     

存在缓冲气体的Na—Cs混合蒸汽中的三体碰撞

Ｎａ－Ｃｓ混合蒸汽中的碰撞能量合并已在［２］中研究过。当在池中充入缓冲气体后，碰撞过程出现新的特点，缓冲气体增大了Ｎａ（３Ｐ）和Ｃｓ（６Ｓ）间的能量转移，这可从测量由Ｎａ（３Ｐ）／Ｃｓ（６Ｐ）和Ｃｓ（６Ｐ）／Ｃｓ（５Ｄ）碰撞而被布居的高能级所发射的荧光得到证实。得到三体碰撞速率系数ｋ３＝５．９×１０－２７ｃｍ６ｓ－１。     

Effects of He－Ne laser irradiation on acupuncture points on Enzymic activity of SDH，3β－HSDH and 17β－HSDH of uteri and ovaria in rabbits

Ｅｆｆｅｃｔｓ ｏｆ Ｈｅ－Ｎｅ ｌａｓｅｒ ｉｒｒａｄｉａｔｉｏｎ ｏｎ ａｃｕｐｕｎｃｔｕｒｅ ｐｏｉｎｔｓ ｏｎ Ｅｎｚｙｍｉｃ ａｃｔｉｖｉｔｙ ｏｆ ＳＤＨ，３β－ＨＳＤＨ ａｎｄ １７β－ＨＳＤＨ ｏｆ ｕｔｅｒｉ ａｎｄ ｏｖａｒｉａ ...     

用于与HRD－1双光栅单色仪及1109光子计数器联用的拉曼光谱计算机数据采集与处理系统

用于与ＨＲＤ－１双光栅单色仪及１１０９光子计数器联用的拉曼光谱计算机数据采集与处理系统杨经国，刘新民，薛康（四川大学物理系成都６１００６４）ＲａｍａｎＳｐｅｃｔｒｌＣｏｍｐｕｔｅｒＤａｔａＰｒｏｃｅｓｓｉｎｇＳｙｓｔｅｍＣｏｕｐｌｅｄＷｉｔｈＨＲＤ－...     

核内核子－核子非弹散射截面（Ⅰ）

在与平均场、核内核子－核子弹性散射截面以及输运方程相统一的理论框架内推导了核内核子－核子非弹散射截面的解析表达式．其数值结果能很好地重现自由非弹截面的实验值，所计算的有效非弹截面与Ｄｉｒａｃ－Ｂｒｕｅｃｋｎｅｒ的计算结果相一致．     

BiPbSbSrCaCuO非晶态及热处理对其影响

本工作用正电子湮没谱术（ＰＡＳ），Ｘ射线衍射谱（ＸＲＤ），示差热分析（ＤＴＡ），扫描电镜显微术（ＳＥＭ）和交流磁化率（Ｘａｃ）研究了Ｂｉ－Ｐｂ－Ｓｂ－Ｃａ－Ｃｕ－Ｏ非晶态和后续热处理的影响。结果表明：所研究的非晶态晶化温度Ｔｃ－４５０－４７０℃，当热处理温度Ｔａ＜Ｔｃ，非晶太经低温结构弛豫和高温弛豫。当Ｔａ＞Ｔｃ，在晶态多相体系中随温度升高发生低ｎ相向高ｎ相的转变，８５０℃退火可使超导转变温度...     

KDEHP-HDEHP微乳体系中水结构的FTIR研究

运用傅里叶变换红外光谱对水／ＫＤＥＨＰ－ＨＤＥＨＰ／ｎ－ＨＥＰＴＡＮＥ微乳体系中的水结构进行了研究。我们对微乳体系中水分子ＯＨ伸缩振动吸收峰进行傅里叶退卷积处理,发现体系中存在四种不同结构的水。依据傅里叶退卷积的结果,对水分子在３０００～３７５０ｃｍ－１范围内的红外光谱进行曲线拟合得到四个子峰,分别位于３６１０ｃｍ－１左右,３５１０ｃｍ－１左右,３４００ｃｍ－１左右和３２７０ｃｍ－１左右,这四个子峰分别被指认为分散于表面活性剂疏水链之间的自由水,与表面活性剂阴离子相互作用的水,类似于纯水的本体水和与表面活性剂阳离子作用的水。     

3-D Phase Object Reconstruction Using Beam-Deflection Iterative Tomography

３－ＤＰｈａｓｅＯｂｊｅｃｔＲｅｃｏｎｓｔｒｕｃｔｉｏｎＵｓｉｎｇＢｅａｍ－ＤｅｆｌｅｃｔｉｏｎＩｔｅｒａｔｉｖｅＴｏｍｏｇｒａｐｈｙ￥ＧＡＯＹｉｑｉｎｇ（ＮａｎｃｈａｎｇＩｎｓｔｉｔｕｔｅｏｆＡｅｒｏｎａｕｔｉｃａｌＴｅｃｈｎｏｌｏｇｙ，Ｎａｎｃｈ...     

热丝CVD生长金刚石薄膜喇曼散射研究

本文报道热丝化学气相沉积法（ＨＦＣＶＤ）生长金钢石薄膜的喇曼散射结果。选取多种峰型，对金钢石薄膜喇曼谱（１１０－１８００ｃｍ－１）采用最小二乘法进行非线性拟合，得到最佳拟合模型，其计算得到的拟合曲线怀实验谱图符合得较好。该模型揭示，石墨Ｄ峰（１３５５ｃｍ－１）是金刚石薄膜喇曼谱中不可缺少的一个组份，并且结合石墨Ｄ峰和金刚石喇曼的空间相关线型，可以解释金刚石喇曼区特殊峰形的物理机制，拟合参量的进一步     

Wormhole solution in Bergmann-Wagoner scalar-tensor gravitational theory

We give a Euclidean wormhole solution in the vacuum Bergmann-Wagoner scalar-tensor gravitational theory. We show that this wormhole, unlike others, has complex charge and is a baby universe (half a wormhole).     

Euclidean Wormholes with Phantom Field and Phantom Field Accompanied by Perfect Fluid

We study the classical Euclidean wormhole solutions for the gravitational systems with minimally coupled pure Phantom field and minimally coupled Phantom field accompanied by perfect fluid. It is shown that such solutions do exist and then the general forms of the Phantom field potential are obtained for which there are classical Euclidean wormhole solutions.     

Wormholes in vacuum Brans-Dicke theory

We present a Euclidean wormhole solution in vacuum Brans-Dicke theory, which is different from that obtained by Accetta et al. This wormhole appears to have the feature that its throat dimension increases linearly with Euclidean cosmic time, although this increase may not be measurable. It also requires a negative Brans-Dicke parameter.     

Morris–Thorne wormhole with Karmarkar condition

In this paper, we construct a wormhole shape function by using Karmarkar condition. We observe that our proposed shape function connects two asymptotically flat regions, which shows the existence of Morris–Thorne traversable wormhole. Moreover, we also represent the embedding diagram in three-dimensional Euclidean space which can be extended from throat to infinity. Further, the Null and Weak energy conditions are discussed in detail. With this shape function, the anisotropic factor exhibits a repulsive nature at the throat. We support all the analysis of this work through graphical representation. It is concluded that our proposed model fulfills all the necessary conditions and shows the existence of exotic matter in the formulism of wormhole geometry in the context of General Relativity.     

Why concave rather than convex inflaton potential?

The Planck data on cosmic microwave background indicates that the Starobinsky-type model with concave inflation potential is favored over the convex-type chaotic inflation. Is there any reason for that? Here we argue that if our universe began with a Euclidean wormhole, then the Starobinsky-type inflation is probabilistically favored. It is known that for a more generic choice of parameters than that originally assumed by Hartle and Hawking, the Hartle–Hawking wave function is dominated by Euclidean wormholes, which can be interpreted as the creation of two classical universes from nothing. We show that only one end of the wormhole can be classicalized for a convex potential, while both ends can be classicalized for a concave potential. The latter is therefore more probable.     

Classical Euclidean Wormhole Solution and Wave Function for a Nonlinear Scalar Field

In this paper we consider the classical Euclidean wormhole solution of the Born—Infeld scalar field. The corresponding classical Euclidean wormhole solution can be obtained analytically for both very small and large . At the extreme limit of small the wormhole solution has the same format as one obtained by Giddings and Strominger (Nuclear Physics B 306, 890, 1988). At the extreme limit of large the wormhole solution is a new one. The wormhole wave functions can also be obtained for both very small and large . These wormhole wave functions are regarded as solutions of quantum-mechanical Wheeler—Dewitt equation with certain boundary conditions.     

What if? Exploring the multiverse through Euclidean wormholes

We present Euclidean wormhole solutions describing possible bridges within the multiverse. The study is carried out in the framework of third quantisation. The matter content is modelled through a scalar field which supports the existence of a whole collection of universes. The instanton solutions describe Euclidean solutions that connect baby universes with asymptotically de Sitter universes. We compute the tunnelling probability of these processes. Considering the current bounds on the energy scale of inflation and assuming that all the baby universes are nucleated with the same probability, we draw some conclusions about which universes are more likely to tunnel and therefore undergo a standard inflationary era.     

Nondifferentiable Dynamic: Two Examples

Some nondifferentiable quantities (for example, the metric signature) can be the independent physical degrees of freedom. It is supposed that in quantum gravity these degrees of freedom can fluctuate. Two examples of such quantum fluctuation are considered: a quantum interchange of the sign of two components of the 5D metric and a quantum fluctuation between Euclidean and Lorentzian metrics. The first case leads to a spin-like structure on the throat of a composite wormhole and to a possible inner structure of the string. The second case leads to a quantum birth of the non-singular Euclidean Universe with frozen 5^th dimension. The probability for such quantum fluctuations is connected with an algorithmical complexity of the Einstein equations.     

Wormholes in higher dimensions with Gauss-Bonnet terms

A class of wormhole solutions permitted in a theory with Gauss-Bonnet terms in the gravitational action in higher dimensions have been studied. The case of de-Sitter type instantons, with a compact inner space, are of particular interest here. Some of the configurations, when continued analytically to the Lorentzian metric lead to the standard inflationary universe. Some multiple-sphere configurations of the type studied by Myers have also been noted. The Euclidean action for the solutions has been calculated and the relevance of the solutions in the quantum creation of the universe has been considered.