几类可积系统的构造

利用 Hamilton-Jacobi 方程并分别采用球坐标、抛物坐标和椭圆坐标来讨论一个中心力场附加一个引力势为 R 的外场所组成的摄动保守系统可积时摄动引力势R的具体表达形式.     

银河系中心存在超大黑洞天文学家又有新证据

在我们生活的银河系中心位置，藏匿着一个人肉眼无法看见的“超级黑洞”：它的直径与地球相当，质量却至少是太阳的40万倍．它“吞噬”周围的所有物质，连光也无法逃逸出去．利用国际最先进的地面望远镜阵列，上海科学家领导的一个国际小组成功拍摄到了迄今为止最接近该黑洞的“射电照片”．     

Tunneling Radiation from a Static Spherically Symmetric Black Hole Surrounded by Quintessence

By extending the Parikh-Wilczek tunneling framework, we investigate the tunneling radiation of uncharged massless particles from a static spherically symmetric black hole surrounded by quintessence. The results are consistent with an underlying unitary theory.     

D-term Chaotic Braneworld in Supergravity Constrained by WMAP9 Data

We study a supergravity D-term chaotic inflationary model, in the context of the braneworld scenario, in particular we consider the Randal1-Sundrum model type 2. Using the latest release from the combination of WMAP9, eCMB, BAO, and Ho, we show that the inflation observables depend only on the number ore-folds N. We also derive all known spectrum inflationary parameters, which are widely consistent with WMAP9 data for a particular choice of values N specially for the scalar spectral index ns and the ratio r. However, the running of the scalar spectral index dns/dlnk is now excluded from the range given by the latest observational measurements.     

利用黑洞原理改进稀疏外观模型跟踪算法

为了解决跟踪漂移问题,提出了一种利用黑洞原理改进的稀疏外观模型目标跟踪算法,用来提高目标跟踪的鲁棒性。利用黑洞原理从目标模板中搜索聚类中心来降低目标模板数量。通过学习分类器用于构造目标特征;用黑洞原理获取模板字典表示目标;采用高斯分布运动模型获取目标样本,在贝叶斯框架下根据观测模型获取最优目标位置实现跟踪。不同视频序列被用于改进的稀疏外观模型跟踪算法和其他先进目标跟踪算法进行仿真实验。实验结果表明,实现了目标跟踪的目的,有效地降低了目标局部遮挡问题的影响,提高了目标跟踪精度。     

清水出彩虹

利用白光脉冲光纤激光器发出的高强度、高定向性的白光,聚焦地照射水,可以产生定向的、多级的彩色干涉环,这就是"相干彩虹".脉冲激光加热在水里产生了大小相仿的气泡,每个气泡成为散射源.强光导致了空间自相位调制效应,从而产生了相干彩虹.已经在多种液体中观测到了这种现象.     

Parikh-Wilczek Tunneling as Massive Particles from Noncommutative Schwarzschild Black Hole

In this paper, we apply the tunneling of massive particle through the quantum horizon of a Schwarzschild black hole in noncommutative spaeetime. The tunneling effects lead to modified Hawking radiation due to inclusion of back-reaction effects. Our calculations show also that noncommutativity effects cause the further modifications to the thermodynamical relations in black hole. We calculate the emission rate of the massive particles＇ tunneling from a Schwarzschild black hole which is modified on account of noncommutativity influences. The issues of information loss and possible correlations between emitted particles are discussed. Unfortunately even by considering noneommutativity view point, there is no correlation between different modes of evaporation at least at late-time. Nevertheless, as a result of spacetime noncommutativity, information may be conserved by a stable black hole remnant.     

Black Hole Entropy with Modified Dispersion Relations

There is much interest in resolving the quantum corrections to Bekenstein-Hawking entropy with a large length scale limit. The leading correction term ＆ given by the logarithm of black hole area with a model-dependent coefficient. Recently the research for quantum gravity implies the emergence of a modification of the energy-momentum dispersion relation （MDR）, which plays an important role in the modified black hole thermodynamics. In this paper, we investigate the quantum corrections to Bekenstein-Hawking entropy in four-dimensional Sehwarzschild black hole and Reissner-Nordstrom black hole respectively based on MDR.     

Dark Energy Accretion onto a Black Hole in an Expanding Universe

By using the solution describing a black hole embedded in the FLRW universe, we obtain the evolving equation of the black hole mass expressed in terms of the cosmological parameters. The evolving equation indicates that in the phantom dark energy universe the black hole mass becomes zero before the Big Rip is reached.     

Discussion of Garfinkle-Horowitz-Strominger Dilaton Black Hole Entropy

We discuss the entropy of the Garfinkle-Horowitz-Strominger dilaton black hole by using the thin film brick-wall model, and the entropy obtained is proportional to the horizon area of the black hole confirming the Bekenstein-Hawking＇s area-entropy formula. Then, by comparing with the original brick-wall method, we find that the result obtained by the thin film method is more reasonable avoiding some drawbacks, such as little mass approximation, neglecting logarithm term, and taking the term L^3 as a contribution of the vacuum surrounding the black hole, and the physical meaning of the entropy is more clearer.