Catching spiral – S0 transition in groups. Insights from SPH simulations with chemo-photometric implementation

We are investigating the co-evolution of galaxies within groups combining multi-wavelength photometric and 2D kinematical observations. Here we focus on S0s showing star formation in ring/arm-like structures. We use smooth particle hydrodynamical simulations (SPH) with chemo-photometric implementation which provide dynamical and morphological information together with the spectral energy distribution (SED) at each evolutionary stage. As test cases, we simulate the evolution of two such S0s: NGC 1533 and NGC 3626.     

Galaxy evolution in groups. USGC U268 and USGC U376 in the Leo cloud

With the aim of investigating galaxy evolution in nearby galaxy groups, we analyzed the spectral energy distribution of 24 galaxies, members of two groups in the Leo cloud, USGC U268 and USGC U376. We estimated the ages and stellar masses of the galaxies by fitting their total apparent magnitudes from far-ultraviolet to near-infrared with population synthesis models. The comparison of the results for a subsample of galaxies with smooth particle hydrodynamic (SPH) simulations with chemo-photometric implementation, shows that in most cases the estimated stellar masses obtained with the two different approaches are in good agreement. The kinematical and dynamical analysis indicates that USGC U268 is in a pre-virial collapse phase while USGC U376 is likely in a more evolved phase towards virialization.     

民用飞机个人通风送风温度对人体舒适性的影响

通过对某真实客机座舱进行建模，使用计算流体力学（CFD）的方法计算出不同个人通风送风温度下座舱内的温度场和流场分布。然后提取乘客头部区域温度与试验结果进行对比，验证模拟的可信度。最后结合基于人体平均皮肤温度的热舒适评价方法，对不同个人通风送风温度情况下的乘客舒适性进行研究。结果表明：不同个人通风送风温度对乘客头部区域温度影响较小，随着个人通风送风温度从7℃上升到14℃，乘客头部区域温度变化不超过0.8℃。不同个人通风送风温度对乘客平均皮肤温度以及热舒适性的影响较小，随着个人通风送风温度从7℃上升到14℃，目标乘客平均皮肤温度上升0.33℃。     

Reverberation time lags in the high luminosity quasar PG 1247+267

Virial estimates of the black hole mass in the center of AGNs, derived from single-epoch observations of luminosity and emission line widths, are now available for several thousands of objects at all redshifts and luminosities, so that studies of the cosmological evolution of the AGN mass function are becoming possible. These estimates are based on the empirical luminosity-size relation measured through reverberation mapping at low redshifts and luminosities. For this reason the spectrophotometric monitoring of 4 luminous quasars was started in 2003, with the 1.8 m telescope of the Asiago Observatory. To measure the reverberation time lag we adopt a method, recently introduced by Zu et al. (2011), which takes advantage of the available statistical information on variability autocorrelation and makes simple assumptions on the continuum-emission line transfer function. We present the estimate of the broad line region size for the quasar PG 1247+267, which is the most luminous object with reverberation measures to date. Virial products computed for C iv and C iii] emission lines provide consistent results. A possible flattening of the size-luminosity relation for C iv at high luminosity is suggested.     

Integrated Framework for Understanding Relationship Between Human Error and Aviation Safety

Introducing a framework for understanding the relationship between human error and aviation safety from multiple perspectives and using multiple models. The first part of the framework is the perspective of individual operator using the information processing model. The second part is the group perspective with the Crew Resource Management （CRM） model. The third and final is the organization perspective using Reason＇s Swiss cheese model. Each of the perspectives and models has been in existence for a long time, but the integrated framework presented allows a systematic understanding of the complex relationship between human error and aviation safety, along with the numerous factors that cause or influence error. The framework also allows the identification of mitigation measures to systematically reduce human error and improve aviation safety.     

非英语专业本科生学习风格探究及启示

研究学习风格和英语学习成绩之间存在的关系。利用PLSPQ对河南省洛阳市三所高校的479名非英语专业二年级学生进行调查问卷,以学生的四级成绩为依据,分析其学习风格总体状况及其偏好以及在学习风格上所呈现出的差异。结果表明,非英语专业本科生触觉型学习风格的倾向性最为明显,听觉型学习风格倾向最弱,就学习风格而言,英语学习成绩优异者与成绩较差者存在较为明显的差异。结论是学习风格与学习成绩之间并没有显著的关系。     

垂直于流向的截面中2D-PIV测量误差分析

常规二维粒子图像测速技术(2D-PIV)作为重要的流场测试手段,被越来越多地应用到各种类型的流场测量中。然而采用该技术对垂直于流向的截面进行测量时会产生明显误差,该误差是由2D-PIV 原理中几何透视成像关系引起。本文分析了测量截面内有法向速度分量时透视误差产生原因及影响因素,建立了2D-PIV 测量平面内的误差模型。通过实验测试验证了误差模型的正确性,确定了影响测量误差的关键参数为测量平面的法向速度和视场的离轴角。计算结果显示,最大透视误差可达法向速度的9.3%。根据误差模型进行分析,透视误差对流向涡类流场测量的影响主要为3个方面:改变流场速度量值大小、改变旋涡形状、改变旋涡的位置。最后,提出了一些减小误差的措施,为2D-PIV应用于垂直流向截面的测量提供了改进方法。     

独立子树等效时变可用度分析

在复杂系统可用度分析中,采用深度和广度遍历算法将复杂动态故障树分解为独立子树,推导和证明了独立子树等效时变可用度参数模型,建立了各独立子树同构的马尔可夫状态转移链.通过求解降维微分方程获得故障子树的时变可用度参数,采用由下至上的递归处理算法快速实现复杂系统的可用性定量分析,既解决了复杂系统可用度计算的"组合爆炸"问题,又通过考虑时变参数保证了可用度解算的精度.实例分析表明,采用独立子树等效时变可用度分析方法在有效的分解下,其误差可以很小.      

视觉检测中椭圆中心成像畸变误差模型研究

针对在三维视觉检测应用中,空间椭圆的中心经摄像机针孔成像后存在畸变误差的问题进行了研究.基于透视投影变换和空间解析几何理论,建立了在摄像机的像平面上该畸变误差的数学模型,从而为圆孔(椭圆孔)或圆柱(椭圆柱)类工件中心位置的视觉检测、结构光三维视觉检测应用以及视觉检测中的CCD摄像机内部参数标定等问题的解决提供了一个有效的理论依据,具有一定的理论意义和工程应用价值.      

Time series analysis of active galactic nuclei: The case of Arp 102B, 3C 390.3, NGC 5548 and NGC 4051

We used the Z-transformed Discrete Correlation Function (ZDCF) and the Stochastic Process Estimation for AGN Reverberation (SPEAR) methods for the time series analysis of the continuum and the Hα$\alpha$ and Hβ$\beta$ line fluxes of a sample of well known type 1 active galactic nuclei (AGNs): Arp 102B, 3C 390.3, NGC 5548, and NGC 4051, where the first two objects are showing double-peaked emission line profiles. The aim of this work is to compare the time lag measurements from these two methods, and check if there is a connection with other emission line properties. We found that the obtained time lags from Hβ are larger than those derived from the Hα analysis for Arp 102B, 3C 390.3 and NGC 5548. This may indicate that the Hβ   line originates at larger radii in these objects. Moreover, we found that the ZDCF and SPEAR time lags are highly correlated (r∼0.87$r\sim 0.87$), and that the error ranges of both ZDCF and SPEAR time lags are correlated with the FWHM of used emission lines (r∼0.7$r\sim 0.7$). This increases the uncertainty of the black hole mass estimates using the virial theorem for AGNs with broader lines.