磁场中夸克物质的非轻子弱作用过程

讨论了磁场中夸克物质的非轻子弱作用过程. 改进了在弱磁场情况下的近似计算方法, 分别给出了强弱磁场下非轻子过程的反应率的表达式, 以及一定条件下的近似表达式. 结果显示, 强磁场极大的抑制反应率的大小, 进而影响奇异夸克物质的粘滞性.     

初速度对测定黏滞系数的影响

利用斯托克斯公式对小球从不同高度h下落进入液体中的初速度v0与达到匀速运动时的平衡时间t0和运动距离s0的关系进行了详细的推导，给出了不同高度h下的平衡时间t0和运动距离s0的公式和曲线．     

奇异物质体黏滞系数的计算和奇异星振动的阻尼

利用与奇异夸克质量相关的非轻子弱过程u+s←→d+u的反应速率, 在考虑了夸克之间的相互作用并做了热力学自恰处理后, 重新推导、计算了奇异夸克物质的体黏滞系数. 由于热力学自恰的需要引入一项压力附加项, 使得奇异星的体黏滞系数比前人计算的有了很大的增加. 通过计算振动衰减时间我们发现, 虽然体黏滞系数增大了很多, 但以前对于奇异星观测的结论仍然成立.     

升球法测量液体黏滞系数

设计制作了一种升球法测量液体黏滞系数的装置。通过砝码拉动待测液体中的小球上升,使用CCD摄像头识别下落砝码从而得到砝码位置与时间的数据,再对数据进行拟合得出液体的黏滞系数。用该方法对蓖麻油进行了测量,结果表明,测得的黏滞系数与蓖麻油黏滞系数标准值的相对偏差为4%,说明该方法测量精度较高。与传统落球法相比,该方法可用于测量非透明、黏滞系数较低的液体。     

低黏度透明液体黏滞系数测量实验的研究

研究小球在低黏度透明黏性液体中以初速度为零状态下落的加速运动过程, 通过分析小球在加速下 落过程中下落速度与对应时间的关系而得到液体的黏滞系数值. 新方法改进了原变速落球法研究拟合小球下落位 移与对应时间得到黏滞系数的实验方法. 实验结果表明, 新方法提高了实验的稳定性和拟合的准确度     

利用智能手机磁力计测量液体黏滞系数

利用智能手机搭建了一套可视化的简谐振动系统,通过小球在液体中欠阻尼振动的振幅衰减,测量液体的黏滞系数.实验使用手机Phyphox软件中的磁力计传感器,将小球欠阻尼振动振幅的测量转化为磁感应强度大小的测量,并通过Origin软件对采集的数据进行非线性拟合,得到液体阻尼因数,求出液体的黏滞系数.     

基于智能手机测量液体黏滞系数的方法研究

基于阻尼振动的原理,利用智能手机测量弹簧振子的加速度,通过阻尼振动的动力学方程计算出金属球做阻尼振动时液体的阻尼系数和黏滞系数,并将黏滞系数测量值与理论值进行比较,相对误差为0.39%,进一步论证了本实验方案的可行性。与传统方案相比,基于智能手机的液体黏滞系数测量方法操作简单且趣味性强,同时降低了传统实验方法的仪器成本,对物理实验的线上教学具有一定的参考意义。     

高速相机及智能手机在液体黏滞系数测量上的应用

液体黏滞性的测量非常重要,目前最常用的落球法是通过激光发射探头测量小球匀速下落过程中的速度,进而计算黏滞系数.然而,实际操作过程中,激光器的调节往往很困难,而且容易出现小球下落过程中难以穿过激光的现象,导致实验成功率低.本文通过实验研究智能手机及高速相机在落球法测黏滞系数中的应用,对比常规方法与智能手机或高速相机的测试...     

利用降膜流动测量液体黏滞系数

利用降膜流动设计并搭建了测量液体黏滞系数的实验装置,根据不可压缩液体N-S方程,结合边界条件建模。采取测量液膜表面速度的方法计算液膜厚度。测量了蓖麻油不同流量下的黏滞系数,倾斜板在不同倾角下,黏滞系数测量相对准确的流量区间基本相同,相对误差在8%以下。分析了装置的适用条件和误差来源。并用全内反射法进行了液膜厚度对比验证。该研究丰富了测量液体黏滞系数的教学内容和方法,有助于学生掌握流体力学相关知识,提高综合设计能力。     

高温近似下奇异夸克物质的体粘滞系数

在准粒子描述下,采用自洽的热力学方法,考虑奇异夸克物质(SQM?)的介质效应,计算了高温近似下奇异夸克物质的体粘滞系数.发现介质效应对奇异夸克物质的体粘滞系数有很大影响,这使得观测数据不再排除两味色超导相奇异星的存在.     

一级微扰QCD耦合的夸克物质体粘滞系数

在高密情况下考虑了夸克间弱的耦合,直接应用微扰计算得到的热力学势计算了奇异夸克物质(SQM)的体粘滞系数,发现介质效应使SQM的粘滞性提高2个量级左右     

Strange Quark Matter and Strangelets in a Strong Magnetic Field

We study the stability properties of magnetized strange quark matter and strangelets under a strong magnetic field in the MIT bag model. The free energy per baryon of strange quark matter feels a great influence from the magnetic field. At the field strength about 10¹⁷G, the magnetized strange quark matter becomes more stable. Considering the finite size effect, the magnetic influence on strangelets becomes complicated. For a given magnetic field, there exists a critical baryon number, below which the magnetized strangelets have lower energy than the non-magnetized strangelets. For the field strength of 5× 10¹⁷G, the critical baryon number is A_c ～ 100. Generally, the critical baryon number increases with the decreasing external magnetic field. When the field strength is smaller than 10¹⁷G, the critical baryon number goes up to A_c～ 10⁵. The stable radius, electric charge, and quark flavor fractions of magnetized strangelets are shown.     

Bulk viscosity of hot dense Quark matter in the PNJL model

Starting from the Kubo formula and the QCD low energy theorem, we study the the bulk viscosity of hot dense quark matter in the PNJL model from the equation of state. We show that the bulk viscosity has a sharp peak near the chiral phase transition, and that the ratio of bulk viscosity over entropy rises dramatically in the vicinity of the phase transition. These results agree with those from the lattice and other model calculations. In addition, we show that the increase of chemical potential raises the bulk viscosity.     

Equation of State of the Strong Interaction Matter in an External Magnetic Field

We investigate the equation of state of the strong interaction matter in a background magnetic field via the two flavor Nambu-Jona-Lasinio model. Starting from the mean-field thermodynamical potential density Ω, we calculate the pressure density p, the entropy density s, the energy density ε, and the interaction measure (ε-3p)=T⁴ of the strong interaction matter at finite temperature and finite magnetic field. The results manifest that the chiral phase transition is just a crossover but not a low order phase transition. Moreover there may exist magnetic catalysis effect, and its mechanism is just the effective dimension reduction induced by the magnetic field.     

用布里渊散射测量水的体粘滞系数

提出了一种直接测量水的体粘滞系数的实验方法－布里渊散射方法,通过分析剪切粘滞系数和体粘滞系数与布里渊散射线宽的关系,得到了布里渊散射线宽和频移与水的体粘滞系数关系的公式,建立了实验测量水的体粘滞系数的基础,给出了不同温度下水的体粘滞系数的实验测量结果,估算了这种方法的测量误差,实验和理论分析都表明这是一种直接测量水的体粘滞系数的快速而精确的方法。     

Bianchi Type Ⅲ String Cosmological Model with Bulk Viscosity

The Bianchi type Ⅲ cosmological model for a cloud string with bulk viscosity are presented. To obtain a determinate model, an equation of state ρ=kλ and a relation between metric potentials B = C^n are assumed. The physical and geometric aspects of the model are also discussed. The model describes a shearing non-rotating continuously expanding universe with a big-bang start, and the relation between the coefficient of bulk viscosity and the energy density is ζ∝ρ^1/2.     

Singularities and Entropy in Bulk Viscosity Dark Energy Model

In this paper bulk viscosity is introduced to describe the effects of cosmic non-perfect fluid on the cosmos evolution and to build the unified dark energy (DE) with (dark) matter models. Also we derive a general relation between the bulk viscosity form and Hubble parameter that can provide a procedure for the viscosity DE model building. Especially, a redshift dependent viscosity parameterζ∝λ₀ +λ₁(1+z)ⁿ proposed in the previous work [X.H. Meng and X. Dou, Commun. Theor. Phys. 52 (2009) 377] is investigated extensively in this present work. Further more we use the recently released supernova dataset
(the Constitution dataset) to constrain the model parameters. In order to differentiate the proposed concrete dark energy models from the well known $\Lambda$CDM model, statefinder diagnostic method is applied to this bulk viscosity model, as a complementary to the Om parameter diagnostic and the deceleration parameter analysis performed by us before. The DE model evolution behavior and tendency are shown in the plane of the statefinder diagnostic parameter pair {r,s} as axes where the fixed point represents theΛCDM model. The possible singularity property in this bulk viscosity
cosmology is also discussed to which we can conclude that in the different parameter regions chosen properly, this concrete viscosity DE model can have various late evolution behaviors and the late time singularity could be avoided. We also calculate the cosmic entropy in the bulk viscosity dark energy frame, and find that the total entropy in the viscosity DE model increases monotonously with respect to the scale factor evolution, thus this monotonous
increasing property can indicate an arrow of time in the universe evolution, though the quantum version of the arrow of time is still very puzzling.