二维诱生引力的量子宇宙学波函数

本文用超空间方法对其有宇宙学常数的二维诱生引力进行量子化。我们用等效约束方法精确求解了宇宙波函数Ｗｈｅｅｌｅｒ－Ｄｅｗｉｔｔ方程，并且讨论了波函数的行为。     

引力“常数”和宇宙“常数”为变量的FRW平坦模型解

本文考虑了推广的Ｅｉｎｓｔｅｉｎ引力理论，即引力常数Ｇ和宇宙常数∧都是变量，而Ｅｉｎｓｔｅｉｎ引力场方程保持形式不变，在此框架上，讨论了平坦ＦＲＷ模型的解。     

洛伦兹对称破缺与宇宙加速膨胀

1998年的超新星观测表明当今宇宙正在加速膨胀.暗能量是指宇宙加速膨胀的宇宙介质.正的宇宙学常数L是暗能量的重要候选者,但导致宇宙加速膨胀的原因并非L莫属.洛伦兹不变性是物理学最严格的对称性之一,然而所有的量子引力理论都预言了洛伦兹对称性的破缺.基于大尺度洛伦兹破缺(LargeScale Lorentz Violation, LSLV)的宇宙学模型,讨论了有效引力理论修正的Friedmann方程,由此可以得到,大尺度上的洛伦兹破缺和宇宙学常数项的综合效应会产生后期观测到的宇宙加速膨胀.     

线性引力的宇宙波函数

本文研究了1+1维线性引力的量子宇宙学,关于宇宙边界条件的Hartle—Hawking提案也被推广到1+1维理论.我们发现:对于正的宇宙常数,标度因子的演化与四维欧氏空时相一致.波函数具有振荡行为;对于负的宇宙常数,会出现指数膨胀和收缩的宇宙,波函数是指数型的.     

Eguchi-Hanson型度量的数量曲率方程的解

研究了引力场的Eguchi-Hanson型度量的数量曲率方程的解.这些解可用来构造带宇宙常数的引力瞬子.     

核素在引力常数减小过程中的放射性衰变

推动地球板块运动、地震及火山活动的动力机制,地球圈层及岩石结构的形成,以及地球资源和能源等,是当代地球物理急待解决的问题.依据引力常数变化对核素的作用,以及核物理基本原理,建立起了一个核素结构随引力常数变化的动态核力模型,此核力模型与宇宙天体的演化过程密切相关且同步.此模型对上述多方面存在问题的解决,作了合理的解释.通过引力常数减小而产生的地球结构能释放的论证,求证出核素放射性衰变是地球结构能的释放方式;论证及量化计算了地幔岩石化学结合能是对于地球结构能释放或核衰变能的吸收;证明了引力常数减小对宇宙宏观与原子核微观作用的内在一致性或宏观与微观的统一性;得出了原子核结构的稳定和非稳定性具有相对性的结论.       

引力"常数"和宇宙"常数"为变量的FRW平坦模型解

本文在引力“常数”G和宇宙“常数”Λ为变量，同时保持Einstein引力场方程形式不变的框架下，讨论了Friedman—Robertson—Walker(FRW)平坦模型的解．我们假设了一个状态方程P=(γ一1)ρ和宇宙常数与哈勃参数的关系Λ=3ηH^2，得到了场方程的一个精确解。它描述的是一个减速系数为常数的连续膨胀的宇宙，在极端情况下η=0，这个解可以自动变为大家熟知的G是常数和Λ=0时的FRW平坦模型的解。     

引力常数变化的地、月系统证据分析及天体膨胀和光谱的非宇宙学红移

依据基本的天体运动学定律,利用地、月轨道变化的生物钟数据及相关资料,经分析、推理,建立起了一个引力常数变化的模型.用此模型对地球、太阳系结构演化,以及光谱的非宇宙学红移进行了分析.并计算了地球、太阳系结构演化过程中的相关物理量;计算了木星相应年代的相关物理量.运用本模型,证明了引力常数减小既产生宇宙的膨胀运动,也产生了光谱的非宇宙学红移和宇宙学红移,光谱的实际红移是这2种红移综合作用的结果.解释了类星体现象.计算结果与实际观测所作对比表明,此模型与实际观测是基本相符的,确定了此模型的合理性.本文通过引力常数减小对天体运动所产生的重要作用,从一个新的角度论证了宇宙的结构和演化,以及宇宙结构的收敛性.     

标量张量暴胀宇宙学

推广的引力理论 ( generalized gravity theory)早就被用来建立拓广暴胀模型 ( extend inflationarymodel) .不过 ,引力的基本理论仍然是 Einstein的广义相对论 ,推广的引力理论只是用来改变引力常数 G的值 ,以调节宇宙膨胀的速度而解决优良出口问题 .我们的标量张量暴胀宇宙学则是以标量张量引力理论为基础 ,并且以引力标量场ψ作为暴胀场 ( inflaton)来建立暴胀宇宙模型 .我们所用的作用量为 :A =∫d4x - g[-ψR - ωψ ψ .ψ - 2ψλ(ψ) - Γ ( u .ψ) 21 -ψ + 1 6πLm],其中 Lm为物质的拉氏密度 ,ψ .ψ≡ψ,σψ,σ,u .ψ≡ uμ…     

宇宙演化、粒子演化的物理根源

 Dirac宇宙论与作者的2类自由流阻尼标度理论,虽出发点不同,但宇宙演化、粒子演化的物理根源是宇宙的引力常数随宇宙时间的推移而减小的结论却是一致的.人们对此存在长期争议.根据现有的一些实验事实和理论分析,希望对此问题有所澄清.     

X-ray clusters of galaxies as tracers of structure in the Universe

Clusters of galaxies are visible tracers of the network of matter in the Universe, marking the high-density regions where filaments of dark matter join together. When observed at X-ray wavelengths these clusters shine like cosmic lighthouses, as a consequence of the hot gas trapped within their gravitational potential wells. The X-ray emission is linked directly to the total mass of a cluster, and so can be used to investigate the mass distribution for a sizeable fraction of the Universe. The picture that has emerged from recent studies is remarkably consistent with the predictions for a low-density Universe dominated by cold dark matter.     

Detection of weak gravitational lensing distortions of distant galaxies by cosmic dark matter at large scales

Most of the matter in the Universe is not luminous, and can be observed only through its gravitational influence on the appearance of luminous matter. Weak gravitational lensing is a technique that uses the distortions of the images of distant galaxies as a tracer of dark matter: such distortions are induced as the light passes through large-scale distributions of dark matter in the foreground. The patterns of the induced distortions reflect the density of mass along the line of sight and its distribution, and the resulting 'cosmic shear' can be used to distinguish between alternative cosmologies. But previous attempts to measure this effect have been inconclusive. Here we report the detection of cosmic shear on angular scales of up to half a degree using 145,000 galaxies and along three separate lines of sight. We find that the dark matter is distributed in a manner consistent with either an open universe, or a flat universe that is dominated by a cosmological constant. Our results are inconsistent with the standard cold-dark-matter model.     

A measurement of the cosmological mass density from clustering in the 2dF Galaxy Redshift Survey

The large-scale structure in the distribution of galaxies is thought to arise from the gravitational instability of small fluctuations in the initial density field of the Universe. A key test of this hypothesis is that forming superclusters of galaxies should generate a systematic infall of other galaxies. This would be evident in the pattern of recessional velocities, causing an anisotropy in the inferred spatial clustering of galaxies. Here we report a precise measurement of this clustering, using the redshifts of more than 141,000 galaxies from the two-degree-field (2dF) galaxy redshift survey. We determine the parameter beta = Omega0.6/b = 0.43 +/- 0.07, where Omega is the total mass-density parameter of the Universe and b is a measure of the 'bias' of the luminous galaxies in the survey. (Bias is the difference between the clustering of visible galaxies and of the total mass, most of which is dark.) Combined with the anisotropy of the cosmic microwave background, our results favour a low-density Universe with Omega approximately 0.3.     

地心引力常数变化原因的分析和讨论

对地心引力常数的变化原因作了定性分析和讨论．根据地心引力常数、万有引力常数和地球质量三者的变化特点,认为地心引力常数的变化不只是万有引力常数变化或地球质量变化一种原因引起的,而是由于万有引力常数和地球质量两者联合变化引起的结果．     

A correlation between the cosmic microwave background and large-scale structure in the Universe

Observations of distant supernovae and the fluctuations in the cosmic microwave background (CMB) indicate that the expansion of the Universe may be accelerating under the action of a 'cosmological constant' or some other form of 'dark energy'. This dark energy now appears to dominate the Universe and not only alters its expansion rate, but also affects the evolution of fluctuations in the density of matter, slowing down the gravitational collapse of material (into, for example, clusters of galaxies) in recent times. Additional fluctuations in the temperature of CMB photons are induced as they pass through large-scale structures and these fluctuations are necessarily correlated with the distribution of relatively nearby matter. Here we report the detection of correlations between recent CMB data and two probes of large-scale structure: the X-ray background and the distribution of radio galaxies. These correlations are consistent with those predicted by dark energy, indicating that we are seeing the imprint of dark energy on the growth of structure in the Universe.     

An increased estimate of the merger rate of double neutron stars from observations of a highly relativistic system

The merger of close binary systems containing two neutron stars should produce a burst of gravitational waves, as predicted by the theory of general relativity. A reliable estimate of the double-neutron-star merger rate in the Galaxy is crucial in order to predict whether current gravity wave detectors will be successful in detecting such bursts. Present estimates of this rate are rather low, because we know of only a few double-neutron-star binaries with merger times less than the age of the Universe. Here we report the discovery of a 22-ms pulsar, PSR J0737-3039, which is a member of a highly relativistic double-neutron-star binary with an orbital period of 2.4 hours. This system will merge in about 85 Myr, a time much shorter than for any other known neutron-star binary. Together with the relatively low radio luminosity of PSR J0737-3039, this timescale implies an order-of-magnitude increase in the predicted merger rate for double-neutron-star systems in our Galaxy (and in the rest of the Universe).     

Dark matter maps reveal cosmic scaffolding

Ordinary baryonic particles (such as protons and neutrons) account for only one-sixth of the total matter in the Universe. The remainder is a mysterious 'dark matter' component, which does not interact via electromagnetism and thus neither emits nor reflects light. As dark matter cannot be seen directly using traditional observations, very little is currently known about its properties. It does interact via gravity, and is most effectively probed through gravitational lensing: the deflection of light from distant galaxies by the gravitational attraction of foreground mass concentrations. This is a purely geometrical effect that is free of astrophysical assumptions and sensitive to all matter--whether baryonic or dark. Here we show high-fidelity maps of the large-scale distribution of dark matter, resolved in both angle and depth. We find a loose network of filaments, growing over time, which intersect in massive structures at the locations of clusters of galaxies. Our results are consistent with predictions of gravitationally induced structure formation, in which the initial, smooth distribution of dark matter collapses into filaments then into clusters, forming a gravitational scaffold into which gas can accumulate, and stars can be built.     

平方反比律有心力场中的一种特殊恒矢量

本文指出平方反比律有心力场中，除机械能Ｅ是恒量，角动量Ｌ是恒矢量外，还存在一种特殊的恒矢量，利用这个恒矢量，可以使处理一些有心力场中的问题十分简洁有力。     

Simulations of the formation, evolution and clustering of galaxies and quasars

The cold dark matter model has become the leading theoretical picture for the formation of structure in the Universe. This model, together with the theory of cosmic inflation, makes a clear prediction for the initial conditions for structure formation and predicts that structures grow hierarchically through gravitational instability. Testing this model requires that the precise measurements delivered by galaxy surveys can be compared to robust and equally precise theoretical calculations. Here we present a simulation of the growth of dark matter structure using 2,160(3) particles, following them from redshift z = 127 to the present in a cube-shaped region 2.230 billion lightyears on a side. In postprocessing, we also follow the formation and evolution of the galaxies and quasars. We show that baryon-induced features in the initial conditions of the Universe are reflected in distorted form in the low-redshift galaxy distribution, an effect that can be used to constrain the nature of dark energy with future generations of observational surveys of galaxies.     

受约于天文观测的粒子物理暴涨模型

合理解释宇宙大尺度结构的早期宇宙暴涨理论,成功地阐明所观测到的甚早期宇宙物质密度不均匀性和宇宙微波背景的涨落,是一个能解决标准热－大－爆炸理论中紧迫难题及原初物质密度涨落起源的优选理论［１］ ．对一个合理的暴涨模型,在暴涨阶段,其势至少必须在暴涨子演化方向非常平坦．构建一个合理暴涨模型或暴涨势,必须考虑所有已知的天文观测结果．对目前一个仍未充分研究的含４ 次方自相互作用项的一般树图杂化暴涨模型势,我们做了如何通过已观测到的天文物理数据和即将由ＭＡＰ和ＰＬＡＮＣＫ 卫星实验提供的更高精度的数据［１４］,以及宇宙自洽性要求,约束模型中的待定参数．发现一般树图的Ｈｙｂｒｉｄ 暴涨模型的４ 次方自相互作用项耦合常数需要精细微调．