含氧燃料黏度的理论推算模型

本文结合Vogel-Fulchner-Tammann(VFT)模型、Eyring绝对速率理论和SRK立方型状态方程提出了一种适用于计算含氧燃料黏度的理论推算模型,并对9种含氧燃料在温度在243~373 K、压力在0.1~22 MPa范围内的黏度进行了计算。计算结果表明,黏度模型对含氧燃料黏度的计算值与实验值之间的相对偏差绝对平均值在3.3%以内,最大相对偏差绝对值为4.5%。     

制冷剂及其混合物黏度的计算

本文在收集了制冷剂R11、R12、1%13、R22、R23、R32、R13B1、R113、R114、R123、R124、R125、R134a、R141b、R142b、R143a、R152a、R227ea、R236ea、R236fa、R245ca、R245fa、R1234yf、R1234ze及其二元和三元混合物黏度数据的基础上,结合自由体积理论和混合法则建立了一种可以计算制冷剂及其混合物黏度的推算模型。对于纯质制冷剂的黏度,模型预测值与实验值之间的相对偏差绝对平均值小于1.5%,最大相对偏差绝对值小于3.1%。对于制冷剂二元和三元混合物的黏度,模型预测值与实验值之间的相对偏差绝对平均值小于3.6%,最大相对偏差绝对值小于7.5%。     

基于绝对速率理论的高压液体黏度模型

本文通过考虑压力对流体空穴形成能的影响,并引入参考状态项,对Macías-Salinas绝对速率理论黏度模型进行了改进,建立了一种适用于流体高压液相黏度的推算模型。新模型避免了因计算流体汽化焓与饱和状态下的压缩因子所引入的计算偏差,同时使模型形式得到了简化。利用该模型计算了15种流体在温度为90～440 K、压力为0.01～251.3MPa范围内的液相黏度,计算结果与文献值的相对偏差绝对平均值在2%以内,最大相对偏差绝对值小于9.4%,验证了模型的准确性。     

基于自由体积理论的离子液体黏度模型

离子液体具有熔点低、不挥发、热稳定性好等优点,被视为新型绿色溶剂而得到广泛研究。本文在大量搜集已发表文献中离子液体黏度实验数据的基础上,对自由体积理论进行了修正,建立了离子液体黏度模型。应用该模型对29种离子液体黏度进行了计算,温度为273.15~373.15 K。对比计算值与实验数据,相对偏差绝对平均值在1.22%以内,最大偏差在3.91%以内。结果表明该模型可较好的预测离子液体黏度,为离子液体的进一步研究及相关的工程应用提供了基础数据。     

天然气组元及其混合物的黏度计算

本文利用自由体积理论(FVT)并结合相关混合规则建立了一种可以预测天然气组元及其混合物黏度的计算模型。在对实验数据进行收集整理的基础上,通过对实验数据的回归计算确定了9种天然气基础组元的FVT模型参数,模型计算结果与实验数据之间的平均绝对相对偏差(AARD)小于2.8%。针对天然气组元的二元及多元混合物,本文利用FVT结合适当的混合规则对其黏度进行了预测,模型计算值与实验数据之间的AARD小于7.41%。     

一种适用于烷烃高压液相黏度的推算模型

本文基于绝对速率理论和SRK状态方程,建立了一种可以精确计算烷烃高压液相黏度的推算模型。选取10种正构烷烃(C_1-C_(10))的液相黏度作为研究对象,温度范围为90~448 K,压力范围为0.01~254.4 MPa,利用本文所提出的黏度模型对其进行了计算。计算结果表明:本文的黏度推算模型对这10种烷烃黏度的计算值与实验值之间的平均绝对偏差小于3%,验证了模型的精确性。     

基于对比态原理的常压气体黏度关联式

本文依据对比态原理.通过关联常压下气态物质的无量纲黏度ηr与对比温度Tr以及临界压缩因子Zc,分别建立了适用于单原子气体、双原子气体、碳氢化合物气体以及卤代烃类气态物质的常压下黏度关联式.选用40种物质常压黏度数据对上述关联式分别进行了验证.与文献数据相比,气体黏度计算的相对偏差绝对平均值分别为:0.47%、0.45%...     

烃类混合物的McAllister三体模型通用化

McAllister三体模型的关联性限制了其拓展应用,本文在搜集文献中14类系列型烃类混合物黏度实验数据的基础上,拟合得到了其模型参数。分析发现,McAllister三体模型的两个待定参数(v_(12)与v_(21))与等效沸点(T_(bij))及实验温度(T)间存在一定的规律,由此获得了模型参数的定量推算关系,进而建立了一种具有预测同系列烃类混合物黏度的通用化McAllister三体模型。将新模型的计算结果与实验值进行比较表明,对于所有二元体系的总体平均相对偏差为0.79%,最大相对偏差为7.22%。     

基于逾渗理论的非晶合金屈服行为研究

从非晶合金的微观结构出发,基于处理强无序和具有随机几何结构系统常用的理论方法——逾渗理论来描述非晶合金剪切屈服时的塑性流变.为了更好地理解非晶合金剪切带萌生时的临界问题,结合已有的"自由体积(free volume)模型"和"剪切转变区(shear transformation zone)模型",建立了非晶合金剪切转变的逾渗模型.以Cu_(25)Zr_(75)二元非晶合金为例,计算了在剪切转变区内易发生塑性流动的原子团簇剪切失稳的逾渗阈值,并粗略估算了这些原子团簇的大小.研究发现,剪切失稳的逾渗阈值与临界约化自由体积浓度(x_c～2.4%)有着相似的特性,不同之处在于其值与自由体积的分散度有着密切联系.研究结果作为非晶合金的韧脆转变问题提供了新思路.     

CO_2/正己烷体系质扩散系数和黏度的分子动力学模拟研究

在CO_2驱油提高采收率技术(CO_2-EOR)中,质扩散系数和黏度参数决定了液相混合体系的扩散行为和流动特性。本文基于分子动力学模拟方法,对CO_2/正己烷体系的质扩散系数和黏度进行了研究。CO_2采用改进的EPM2模型,正己烷采用L-OPLS模型,模拟得到的纯质密度分布和自扩散系数与文献数据吻合良好。模拟计算了CO_2/正己烷体系在温度为303.15 K、383.15 K、压力为1～5 MPa范围条件下的质扩散系数和黏度。结果表明:在相同温度下,随压力增大,扩散系数模拟值与实验值相对偏差增大,偏差基本在20%以内。黏度模拟值与实验值相对偏差不超过15%.采用本文所用力场模型与数据处理方法可以用来预测CO_2/正己烷体系的质扩散系数和黏度。     

关于"太阳在银河系中所受引力与到银心距离r的关系"的讨论

讨论了银道面内的引力场强分布和太阳在银河系中所受引力与到银心距离r的关系，指出引力场强g并不是与r的平方成反比，这是由于银河系的大小和形状不能忽略造成的．强调了万有引力定律的适用条件．     

On the calculation of the bremsstrahlung in the region of the plasma frequency

On the basis of the classical theory of radiation produced in incomplete Coulomb interaction, a formula is derived for the coefficient of the bremsstrahlung of fully ionized plasma. In the region of rectilinear approximation a comparison is made with the results of the quantum formula derived from the Born approximation. Furthermore, the influence of dispersion upon the emission coefficient is taken into account; some relations for the region of dispersion are given.     

On the predictability of the positions of the convergence zones in the ocean

The disagreement between the experimental and calculated positions of the first convergence zone are known from many publications. The most probable cause for such a disagreement, namely, the incorrect specification of the input data for the calculations, is considered. The lack of simultaneity between the hydrological surveys of the region and the acoustic experiments is emphasized. The experimental data obtained by the author in five ocean regions are presented. These data characterize the diurnal variability of the distance from the source to the nearest boundary of the convergence zone. The relations proposed by different researchers for calculating the sound speed from the temperature, salinity, and hydrostatic pressure are analyzed. It is shown that these relations lead to a substantial difference in the estimated depth dependence of the hydrostatic gradient of the sound speed. The position of the first convergence zone is calculated for the propagation conditions determined by vertical temperature and salinity profiles with the subsequent recalculation of these profiles into sound speed profiles by using eight different formulas known from the literature. It is shown that different formulas lead to different values of the distance to the first zone; this difference is substantially greater than that between the calculations and experiment. The necessity of improving the recalculation relations in view of the experimental data on sound propagation in natural oceanic waveguides, including the data on the actual positions of the convergence zones, is emphasized.     

Dependence of the Intensity of the Spectral Lines and the Composition of the Sample and the Plasma Parameters of the Unipolar Arc

The investigation was made of the dependence of the intensity of Tl, Ga, Mo, Mg, Mn, Sn, Bi, Ni, Zn, Pt and Au spectral lines and the plasma parameters (temperature T, electron concentration n_e, degree of 6 ionnization α) from concentration of lithium additive.     

Extracting the wavefunction of the LSP at the LHC

We consider associated production of squarks and gluinos with the lightest supersymmetric particle (LSP), or states nearly degenerate in mass with it. Though sub-dominant to pair production of color SU(3)-charged superpartners, these processes are directly sensitive to the wavefunction composition of the lightest neutralinos. Exploiting event-shape variables - including some introduced here for the first time - we are able to identify the composition of the LSP by selecting events involving a single high-pT jet recoiling against missing transverse energy. We illustrate the proposed technique on a set of benchmark cases and propose methods for applying these results in more realistic experimental environments.     

Set the controls for the heart of the Sun

In this paper we describe experiments conducted with high-power lasers that are attempting to replicate, for a very short time and in miniature, conditions found in the Sun. Experiments to date have reached conditions in the outer part of the Sun. To reach the Sun's centre requires compression of material to very much greater than solid density and heating to over ten million degrees. To achieve this, a new class of experiments and a new generation of high-power lasers are required.     

On the Question of the Source of the Apokamp

Technical Physics - The object of this work is the apokamp—a new type of plasma jet, which is formed from a bright offshoot emerging at the bending point of a channel of a high-voltage...