校车安排问题

探讨如何安排校车运行使得教师和工作人员尽量满意的问题.首先建立动态规划模型和选址规划模型,求出合理站点位置及其总距离.然后用归一法定义满意度与距离的函数关系,考虑各区域人数,建立选址规划模型.得到合理站点位置和总满意度.之后建立双目标非线性规划模型,利用量纲分析法给出权重,以此求出合理乘车位置和满意度.最后对问题进行推...     

A New Approach to Black hole Spin in X-Ray Binaries

A new approach of detecting the black hole spin in x-ray binaries is proposed based on the model of the coexistence of the Blandford-Znajek （BZ） and magnetic coupling （MC） processes, in which the BZ process is used to power the jet emissions from x-ray binaries, and high frequency quasi-periodic oscillations （QPOs） are explained by a rotating hotspot in the inner region of the accretion disc surrounding a fast-spinning black hole. It is shown that the black hole spins of several x-ray binaries （XTE J1550-564, GRO d1665-40 and GRS 1915＋105） can be constrained in a rather narrow range, provided that QPOs and jets coexist in these sources.     

Effects of Magnetic Coupling on Profile of Emission Lines and Images of an Accretion Disc Around a Black Hole

The profiles of emission lines and images of an accretion disc around a black hole (13tt) are simulated by considering the effects of the magnetic coupling (MC) of a central BH with the disc. The MC effects are discussed for both slow- and fast-spinning BHs, and the following results are obtained. Firstly, the width of the emission lines and the brightness of the disc are reduced and augmented for slow- and fast-spinning BHs, respectively. Secondly,the image of the disc becomes dimmer and brighter near the inner edge of the disc for slow- and fast-spinning BHs, respectively. It turns out that all these results arise from the MC effects on the position of the dominant emission region of the accretion disc.     

Screw Instability in Black Hole Magnetosphere and kHz QPOs in X-Ray Binaries

Screw instability of the magnetic field connecting a rotating black hole (BH) with its surrounding disc is discussed in coexistence with the Blandford-Znajek (BZ) process and the magnetic coupling (MC) process. A scenario for kilohertz quasi-periodic oscillations (kHz QPOs) in x-ray binaries is proposed by introducing inductance components in the equivalent circuit for BH magnetosphere. It turns out that the period related to the screw instability is consistent with the observations of kHz QPO x-ray binaries.     

Electromagnetic Quantities in Black Hole Magnetosphere

Some electromagnetic quantities in the black hole (BH) magnetosphere are discussed by considering the coexistence of the Blandford-Znajek process and the magnetic coupling process. These quantities are (i) flux of electromagnetic energy and angular momentum transferred between the BH and the disc, (ii) poloidal currents flowing on the     

第四届全国周培源大学生力学竞赛材料力学试题

题一（２５分） 如图所示,狭长矩形截面直杆单侧作用有轴向均布剪切载荷,其单位长度上的大小为ｑ． １．（５分）任意截面上的轴力Ｎ（ｘ）＝ 与弯矩Ｍ（ｘ）＝ ２．（５分）如果平面假设与胡克定律成立,任意横截面上正应力 ３．（５分）ｑ、Ｎ与Ｍ之间的平衡微分关系为 ４．（１０分）任意横截面上剪应力（２０分） 今有两个相同的Ｌ型元件,用螺栓连接,以传递拉力Ｐ．几何尺寸如图所示．Ｌ型元件是刚体．螺栓是线性弹性体,其拉压弹性模量为Ｅ,许用正应力为 设两Ｌ型元件间无初始间隙,也无预紧力,并设在变形过程中两个螺母与Ｌ型元…     

Fibonacci序列的统计属性和电子输运系数

对按膨胀规律A→AB和B→A生成的Fibonacci序列,采用一维随机行走模型数值计算了序列的自相关函数以及自行定义的准标准偏差.利用Hurst分析法研究了序列的再标度范围函数及其Hurst指数,并将结果与一维随机二元序列进行了对比.发现这些统计量有奇特的准周期振荡行为以及小于05的Hurst指数,直接论证了Fibonacci序列具有关联、标度不变及自相似等性质.从Anderson紧束缚模型出发,采用传输矩阵方法研究了Fibonacci序列的电子输运特性,讨论了输运系数对能量及其序列长度的依赖关系.研究 关键词： Fibonacci序列 统计属性 电子输运系数     

高压相BeO晶体的电子结构和光学性质

应用基于密度泛函理论的第一性原理研究方法,考虑广义梯度近似(GGA)下的交换关联势,模拟计算了高压下纤维锌矿(WZ)、闪锌矿(ZB)和岩盐(RS)结构氧化铍(BeO)晶体的电子结构和光学性质等.计算结果表明,随着压力的增加,同种结构下原子间的键长和电荷转移有所减小,并且价带和导带分别向低能和高能方向移动,禁带展宽.与常压下的BeO相比,随着压力的增加,三种结构的BeO晶体的光学性质有一定的变化,介电函数、吸收系数、折射率以及电子能量损失谱曲线出现更多的精细结构,峰的数量增多;各高压相结构的吸收谱和能量损失谱宽度逐次展宽;吸收系数曲线的吸收峰及其位于低能区域的吸收边以及电子能量损失谱峰的位置均发生一定程度的蓝移.     

Cycle of Black Hole Spin due to Disc Accretion Alternating with Magnetic Transfer

The cycle of black hole (BH) spin proposed by Li and Paczynski (henceforth CYCLP) is compared with a more naturad model (henceforth CYC03), in which energy and angular momentum are transferred from a rotating BH to a region of some widths by the closed magnetic field fines. It turns out that the efficiency of converting theaccreted mass into the radiation energy in the CYC03 is less than that estimated in the CYCLP, while the BH mass and entropy in the CYC03 are greater than those in the CYCLP. It is shown that the features of the CYC03 are insensitive to the power-law index indicating the variation of the magnetic field in the disc.