管内高温介质层流入口段中的热辐射作用

数值研究了高温介质密度随温度变化时,管内层流入口段耦合换热中的热辐射作用。采用离散坐标法、控制容积法耦合求解辐射传递方程、能量方程及N-S方程。考察了中等大小光学厚度下,热辐射作用对介质内速度分布、温度分布以及换热的影响。结果表明,即使在不大的光学厚度下,热辐射作用对管内高温介质层流入口段耦合换热的速度场与换热强度都有明显影响。     

大学物理网络个性化教学研究

随着计算机网络技术的发展,开发网络教学平台进行教学已成为目前高校提高教学质量的重要的途径之一.但目前现有的网络课程大多在个性化教学、因材施教方面存在诸多问题,本文建议在大学物理网络教学平台的构建中使用数据挖掘技术,为实施个性化教学提供决策支持.本文介绍了数据挖掘技术及其常用方法,并列举了数据挖掘技术在大学物理网络课程中的应用实例.     

干凝胶法制备空心玻璃微球

在ICF研究中，空心玻璃微球（HGM）因其具有耐压强度高、气体渗透率低、光学透明和相对较低的原子序数等优点，是一种重要的氘氚燃料容器。相对于液滴法，干凝胶法需要较少的传质传热量，并且溶胶一凝胶过程有利于Ca，Al，Zn，Mg等增强组分的均匀掺入，因此，干凝胶法更适于制备大直径厚壁空心玻璃微球。     

薄膜物理与制备

薄膜物理与制备技术研究对于惯性约束聚变(ICF)实验具有重要意义，2003年开展的研究工作主要包括几个方面的内容：低压等离子体化学气相沉积(LPPCVD)法微球CH涂层及掺杂(溴等)技术研究；脉冲激光沉积(PLD)法Fe／Al合金薄膜研制；磁控溅射法Au／Gd，Ti／A1，Ti／Cr支撑薄膜研制；碳氢氮(CxNyH1-x-y)薄膜制备技术研究。相应主要结果如下：(1)利用低压等离子体化学气相沉积(LPPCVD)装置深入考察了以反式-2-丁烯如下：     

Central black hole mass determination for blazars

In this paper, we use a method to determine some basic parameters for the $\gamma$-ray loud blazars. The parameters include the central black mass ($M$), the boosting factor ($\delta$), the propagation angle (${\it {\it\Phi}}$), the distance along the axis to the site of the $\gamma$-ray production ($d$). A sample including 32 $\gamma$-ray loud blazars with available variability time scales has been used to discuss the above properties. In this method, the $\gamma$-ray energy, the emission size and the property of the accretion disc determine the absorption effect. If we take the intrinsic $\gamma$-ray luminosity to be $\lambda$ times the Eddington luminosity, i.e. $L_{\gamma}^{\rm in}=\lambda{L_{\rm Edd}}$, then we have the following results: the mass of the black hole is in the range of $(0.59-67.99)\times10^{7}M_{\odot} \ (\lambda=1.0)$ or $(0.90-104.13)\times10^{7}M_{\odot} \ (\lambda=0.1)$; the boosting factor ($\delta$) in the range of In this paper, we use a method to determine some basic parameters for the $\gamma$-ray loud blazars. The parameters include the central black mass ($M$), the boosting factor ($\delta$), the propagation angle (${\it {\it\Phi}}$), the distance along the axis to the site of the $\gamma$-ray production ($d$). A sample including 32 $\gamma$-ray loud blazars with available variability time scales has been used to discuss the above properties. In this method, the $\gamma$-ray energy, the emission size and the property of the accretion disc determine the absorption effect. If we take the intrinsic $\gamma$-ray luminosity to be $\lambda$ times the Eddington luminosity, i.e. $L_{\gamma}^{\rm in}=\lambda{L_{\rm Edd}}$, then we have the following results: the mass of the black hole is in the range of $(0.59-67.99)\times10^{7}M_{\odot} \ (\lambda=1.0)$ or $(0.90-104.13)\times10^{7}M_{\odot} \ (\lambda=0.1)$; the boosting factor ($\delta$) in the range of In this paper, we use a method to determine some basic parameters for the $\gamma$-ray loud blazars. The parameters include the central black mass ($M$), the boosting factor ($\delta$), the propagation angle (${\it {\it\Phi}}$), the distance along the axis to the site of the $\gamma$-ray production ($d$). A sample including 32 $\gamma$-ray loud blazars with available variability time scales has been used to discuss the above properties. In this method, the $\gamma$-ray energy, the emission size and the property of the accretion disc determine the absorption effect. If we take the intrinsic $\gamma$-ray luminosity to be $\lambda$ times the Eddington luminosity, i.e. $L_{\gamma}^{\rm in}=\lambda{L_{\rm Edd}}$, then we have the following results: the mass of the black hole is in the range of $(0.59-67.99)\times10^{7}M_{\odot} \ (\lambda=1.0)$ or $(0.90-104.13)\times10^{7}M_{\odot} \ (\lambda=0.1)$; the boosting factor ($\delta$) in the range of In this paper, we use a method to determine some basic parameters for the $\gamma$-ray loud blazars. The parameters include the central black mass ($M$), the boosting factor ($\delta$), the propagation angle (${\it {\it\Phi}}$), the distance along the axis to the site of the $\gamma$-ray production ($d$). A sample including 32 $\gamma$-ray loud blazars with available variability time scales has been used to discuss the above properties. In this method, the $\gamma$-ray energy, the emission size and the property of the accretion disc determine the absorption effect. If we take the intrinsic $\gamma$-ray luminosity to be $\lambda$ times the Eddington luminosity, i.e. $L_{\gamma}^{\rm in}=\lambda{L_{\rm Edd}}$, then we have the following results: the mass of the black hole is in the range of $(0.59-67.99)\times10^{7}M_{\odot} \ (\lambda=1.0)$ or $(0.90-104.13)\times10^{7}M_{\odot} \ (\lambda=0.1)$; the boosting factor ($\delta$) in the range of In this paper, we use a method to determine some basic parameters for the $\gamma$-ray loud blazars. The parameters include the central black mass ($M$), the boosting factor ($\delta$), the propagation angle (${\it {\it\Phi}}$), the distance along the axis to the site of the $\gamma$-ray production ($d$). A sample including 32 $\gamma$-ray loud blazars with available variability time scales has been used to discuss the above properties. In this method, the $\gamma$-ray energy, the emission size and the property of the accretion disc determine the absorption effect. If we take the intrinsic $\gamma$-ray luminosity to be $\lambda$ times the Eddington luminosity, i.e. $L_{\gamma}^{\rm in}=\lambda{L_{\rm Edd}}$, then we have the following results: the mass of the black hole is in the range of $(0.59-67.99)\times10^{7}M_{\odot} \ (\lambda=1.0)$ or $(0.90-104.13)\times10^{7}M_{\odot} \ (\lambda=0.1)$; the boosting factor ($\delta$) in the range of $0.16-2.09(\lambda=1.0)$ or $0.24-2.86\ (\lambda=0.1)$; the angle (${\it\Phi}$) in the range of $9.53^{\circ}-73.85^{\circ}\ (\lambda=1.0)$ or $7.36^{\circ}-68.89^{\circ}\ (\lambda=0.1)$; and the distance ($d/R_{\rm g}$) in the range of $22.39-609.36\ (\lambda=1.0)$ or $17.54-541.88\ (\lambda=0.1)$.     

微波共振探针及其在等离子体诊断中的应用

介绍了能够测量稳定和时变等离子体电子密度的微波共振探针,给出了其工作原理和在测量稳定、时变和瞬态等离子体电子密度中的应用。分析了传输模式和反射模式的工作过程及对测量范围、测量精度和空间分辨率等影响因素。结果表明,选用较长的探针有利于提高电子密度的测量范围和精度;选用的微波扫频源高端频率越高,频率分辨率越高,则电子密度的测量范围越大,测量精度越高。理论分析得出系统可测量的电子密度约为1.37×10⁸~4.1×10¹¹cm^-3。     

关于微积分教学中辩证思维与形象思维的表现与培养

辩证思维和形象思维贯穿于微积分数学的全过程,它们是学好微积分的关键,也是大力发展学生教学思维水平的着眼点。     

壁面传质扰动有纵向速度的流动问题

研究壁面有周期性定向抽吸－引射且在壁面上形成纵向速度的二维渠道流动,壁面上的纵向平均速度为〈uω〉．数值结果表明,抽吸－引射的传质倾角θ对流场的性质和壁面上的切应力等有重要的影响．与速度为〈uω〉的运动壁无扰动流动相比,它的阻力偏低,这种阻力偏低与流场的扰动特性有关,即与扰动速度分量的二重相关积分I成正比．阻力在θ＞-24°的范围内有减阻效果;能量在θ＞8°时有净能量减小的效果．     

交联孔隙结构TiO_2-PEDOT:PSS纳米复合薄膜的制备及作为对电极的应用

以TiO2为多孔模板并以聚3,4-亚乙二氧基噻吩-聚苯乙烯磺酸(PEDOT:PSS)为催化材料合成了具有交联孔隙结构的TiO2-PEDOT:PSS纳米复合薄膜(TPNF),并将其作为对电极应用于染料敏化太阳电池(DSC)。首先将TiO2纳米颗粒沉积在导电的掺杂氟的SnO2透明玻璃(FTO)上形成骨架和孔隙均在纳米级别的模板,随后将PEDOT:PSS水溶液附着在模板的骨架表面,最终经热处理获得TPNF。通过优化模板结构和旋涂转速,获得了催化活性优异的TPNF,组装后DSC的填充因子和转换效率分别达到0.528和4.57%,均远高于纯PEDOT:PSS薄膜组装的器件的填充因子(0.297)和转换效率(1.98%)。改善的光电性能归功于TPNF具有优异的协同效应:导电的TiO2骨架为电子迁移提供了快速路径,同时涂覆在骨架表面的PEDOT:PSS通过扩展表面积为还原电解质提供了更多的催化活性点。