改进的GM（1,1）幂模型及其参数优化

为了提高灰色GM（1,1）幂模型的拟合精度,对灰色GM（1,1）幂模型的背景值进行了改进,建立了一类改进GM（1,1）幂模型.利用粒子群优化算法给出了改进GM（1,1）幂模型的参数优化.实例分析结果表明基于粒子群算法的改进的GM（1,1）幂模型具有更高的预测和拟合精度.     

一类准指数序列的模型优化

在传统GM(1,1)模型基础上,结合最小二乘法原理提出:对本身已具有准指数规律的原始序列直接进行建模,并在此基础上对新模型背景值进行适当优化.克服传统GM(1,1)模型建模过程中的盲目性,并提高了拟合与预测精度.     

空间目标的可见光散射与红外辐射

利用Lowtran7大气传输模型计算0.4～0.8μm可见光波段的太阳辐射、大气自身的热辐射以及天地背景辐射.依据粗糙面光散射理论与双向反射分布函数计算空中目标表面对太阳辐射和云层对阳光反射的散射.利用传热学和背景辐射理论,根据能量守恒定律建立空间目标表面温度的热平衡方程.以气球为例,计算不同表面涂层材料的气球,在不同地理位置、不同高度和不同时间条件下,其温度及辐射功率的变化.分析空间目标红外辐射特性的一般规律和特征.     

新时代背景下大学物理基础课程教学的讨论

本文讨论的是＂以怎样的理念实施大学物理基础课程教学,才能使学生的学习训练获得最大收益＂.文章首先回顾近30年来教学思想随时代发展的变化,然后提出新时代背景下大学物理基础课程教学＂以学生为中心,使广大学生在知识、能力、素质上获得全面提高＂的新理念.     

国际地下实验室发展综述

地下实验室是开展粒子物理学、天体物理学及宇宙学等领域一些重大基础性前沿课题的重要研究场所和良好的低本底环境,建设和发展地下实验室对于一个国家的基础科学研究具有重要科学意义.目前,国际上许多国家都已经建立起地下实验室,而中国一直没有很好的地下实验室,特别是极深地下实验室.2009年,清华大学与二滩水电开发有限责任公司开展战略合作,利用锦屏山隧道建立中国首个世界最深的地下实验室--中国锦屏地下实验室(China Jinping Underground Laboratory,CJPL),并于2010年12月12日正式启用.中国锦屏地下实验室的建成,标志着中国已经具备开展物理学重大基础前沿科学研究的自主地下实验平台,对于推动我国相关领域的重大基础前沿课题的自主研究意义重大.文章对国际上一些重要地下实验室的情况进行了介绍,并对中国锦屏地下实验室的基本情况进行了介绍.     

Variable low-mass filtering using an electrodynamic ion funnel

An adjustable low-mass filter has been developed for an electrospray ionization (ESI) source to block ions associated with unwanted background species from entering the mass spectrometer. The low-mass filter is made by using an adjustable potential energy barrier from the conductance-limiting plate of an electrodynamic ion funnel, which prohibits species with higher ion mobilities from exiting the ESI source. We show that this arrangement provides a linear voltage adjustment for low-mass filtering from m/z 0 to 500. Mass filtering above m/z 500 is also performed; however, higher-mass species are attenuated. The mass filter was tested with a liquid chromatography/mass spectrometry (LC/MS) analysis of a bovine serum albumin (BSA) tryptic digest and resulted in the ability to block low-mass, background species, which accounted for 40-70% of the total ion current immediately behind the ESI source during peak elution and detection.     

A Brief Note on a New Cosmic “Coincidence” and New Physics

The latest results from the Wilkinson Microwave Anisotropy Probe (WMAP) with regard to the Cosmic Microwave Background (CMB) throw up some intriguing results, and the question has been asked “Does this point to new physics?” We point out that indeed all this indicates new physics on the Planck scale.     

Some new results of IR systems'' sensitivity equations

Typical IR systems' sensitivity equations have been established for decades, these include the NETD equation for IR imaging systems, and the acquisition and tracking range equations for IR searching and tracking systems, but they only fit the specific or simplified conditions. For example, the NETD equation can only be used for systems tested under the standard condition. In the field application, we must deal with the noise equivalent radiance difference NELD, not the NETD, and give out its explicit equation for concrete calculation. For the range equation, when the small target, often called a point source, is not strong enouph, i. e., when the target contrast is seriously decreased, we must consider the unneglectable background effect. In this paper, we summarrize some more general and valuable IR systems' sensitivity equations, which can be used for the practical engineering analysis and projection effectively.     

Cosmology with cluster surveys

Surveys of clusters of galaxies provide us with a powerful probe of the density and nature of the dark energy. The red-shift distribution of detected clusters is highly sensitive to the dark energy equation of state parameterw. Upcoming Sunyaev-Zel’dovich (SZ) surveys would provide us large yields of clusters to very high red-shifts. Self-calibration of cluster scaling relations, possible for such a huge sample, would be able to constrain systematic biases on mass estimators. Combining cluster red-shift abundance with limited mass follow-up and cluster mass power spectrum can then give constraints onw, as well as onσ ₈ and Ω_M to a few per cents.     

Statistical isotropy of the cosmic microwave background

The breakdown of statistical homogeneity and isotropy of cosmic perturbations is a generic feature of ultra-large scale structure of the cosmos, in particular, of non-trivial cosmic topology. The statistical isotropy (SI) of the cosmic microwave background temperature fluctuations (CMB anisotropy) is sensitive to this breakdown on the largest scales comparable to, and even beyond the cosmic horizon. We propose a set of measures,K _l (l = 1, 2,3,...) which for non-zero values indicate and quantify statistical isotropy violations in a CMB map. We numerically compute the predictedK _l spectra for CMB anisotropy in flat torus universe models. Characteristic signatures of different models in theK _l spectrum are noted.