多排螺旋CT冠状动脉成像研究进展

随着多排螺旋CT设备的不断进步,使用多排螺旋CT行冠状动脉CT血管造影(CCTA)诊断冠状动脉粥样硬化性心脏病(CAD)已广泛应用于临床实践工作中。由于影像技术的进步使CCTA检查的准确度大大提高,这项检查已经成为一种筛查诊断CAD的可靠的无创的检查方法。同时CCTA检查在预测CAD的疾病进程和心血管事件方面具有重要作用。尽管CCTA检查的作用已被学术界广泛肯定,但它有一个重要的缺陷就是检查的有效辐射剂量较大,这将增大辐射诱导性恶性肿瘤的发病风险。为了最大限度地降低CCTA检查的辐射风险,多种在满足影像诊断的前提下降低CCTA检查有效辐射剂量的方法已经出现。本文将回顾多排螺旋CT的技术进展和目前减少CCTA检查辐射剂量的主要方法,对CCTA检查在CAD中的诊断、预后价值评估和CCTA检查的未来发展方向等几个方面进行讨论。      

小肠梗阻MSCT研究现状

小肠梗阻具有很高的发病率,早期准确诊断和全面病情评估是临床选择治疗方式的前提。多层螺旋CT (MSCT)在评价是否存在小肠梗阻、梗阻部位、严重程度及梗阻病因方面均具有很高的准确度,对继发性肠缺血也能提供有价值的影像学信息。本文对MSCT在小肠梗阻评价中的应用现状进行综述。      

自适应统计迭代重建技术在髋关节64排CT低管电流检查中的应用

目的：探讨自适应统计迭代重建（ASIR）技术在髋关节64排CT低管电流检查中的应用。方法：106例髋关节64排螺旋CT扫描患者,随机选取53例患者采用常规管电流220 m As扫描,并采用滤过反投影（FBP）方式重建。另外53例患者采用低管电流50 m As扫描,并采用30%ASIR技术。对两组髋关节图像的辐射剂量和图像质量进行评价,并比较不同重建图像在同一层面的图像噪声值和信噪比。结果：常规管电流组与低管电流组的CT剂量指数（CTDIvol）分别为（15.55±0.20）m Gy、（3.56±0.15）m Gy,低管电流组平均CTDIvol较常规管电流组降低77.1%;常规管电流组与低管电流组的剂量长度乘积（DLP）分别为（297.82±2.9）m Gy·cm、（67.59±3.3）m Gy·cm,低管电流组平均DLP较常规管电流组降低77.3%,低管电流组与常规管电流组相比,辐射剂量大大降低（P〈0.05）。常规管电流组图像质量评分为优、良、差的患者分别为49、4和0例;低管电流组图像质量评分为优、良、差的患者分别为42、11及0例。两组图像的差异无统计学意义（P〉0.05）。图像噪声值分别为31.44、44.29,差异有统计学意义（P〈0.05）。图像信噪比分别为11.03、10.06,差异有统计学意义（P〈0.05）。结论：ASIR技术应用于64排螺旋CT髋关节低管电流扫描,大幅降低辐射剂量的同时,图像质量也能满足临床诊断的需要。     

中国撤县（市）设区对城市经济增长的影响分析

撤县（市）设区是通过打破行政区经济,减少行政区边界,实现以地级市为基础的经济一体化的重要手段,采用政策评估的常用工具——倍差法,对中国1990-2007年的撤县（市）设区的样本进行了分析,发现撤县（市）设区对城市经济增长具有约5年的短期促进作用,主要表现在人均GDP增长率、人均固定资产投资增长率、人均消费增长率等方面,对人均道路面积和人均公共汽车数量的增长率则是先抑后扬,对相邻城市的经济增长则具有约2年的短期促进作用;并以佛山撤县（市）设区为案例,分析了短期促进作用的来源和长期激励消失的原因,认为基础设施投资是政府在撤县（市）设区后的主要行为,以此带动产业转移和房地产消费,进而促进了经济增长;但由于撤县（市）设区削弱了地方政府的发展权限,向上级政府集中了资源的控制权,使得地方长期经济发展的激励消失。     

2011年春夏季节长江中下游旱涝急转可能成因

利用1980-2011年观测的降水和美国NCEP/NCAR大气再分析等资料,采用经验正交分解（EOF）和线性回归等统计方法,讨论了2011年发生在长江中下游地区春夏旱涝急转的成因。结果表明：该年1-5月持续的La Nina事件导致西北太平洋副热带高压位置位于125°E以东,西北太平洋副热带高压西北侧的西南风伴随的水汽通量无法达到长江流域,从而导致了2011年长江流域1-5月份的持续性干旱现象。伴随La Nina的减弱,6月份的青藏高原的感热明显增强,诱发西北太平洋副热带高压自东向西北方向移动到110°E,引导西南风水汽向长江流域输送,而青藏高原对流的加强和向东移动与来自西北太平洋副热带高压西北侧的西南气流在长江中下游地区的汇合导致了6月份长江中下游降水的急剧增加,从而形成了2011年长江中下游地区春夏季节的旱涝急转。     

Edge‐on disk galaxies in the SDSS DR6: Fractions of bulgeless and other disk galaxies

The aim of this study is to determine the fractions of different spiral galaxy types, especially bulgeless disks, from a complete and homogeneous sample of 15 127 edge‐on disk galaxies extracted from the sixth data release from the Sloan Digital Sky Survey. The sample is divided in broad morphological classes and sub types consisting of galaxies with bulges, intermediate types and galaxies which appear bulgeless. A small fraction of disky irregulars is also detected. The morphological separation is based on automated classification criteria which resemble the bulge sizes and the flatness of the disks. Each of these broad classes contains about 1/3 of the total sample. Using strict criteria for selecting pure bulgeless galaxies leads to a fraction of 15% of simple disk galaxies. We compare this fraction to other galaxy catalogs and find an excellent agreement of the observed frequency of bulgeless galaxies. Although the fraction of simple disk galaxies in this study does not represent a “cosmic” fraction of bulgeless galaxies, it shows that the relative abundance of pure disks is comparable to other studies and offers a profound value of the frequency of simple disks in the local Universe. This fraction of simple disks emphasizes the challenge for formation and evolution models of disk galaxies since these models are hard pressed to explain the observed frequency of these objects (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

A new formula describing the scaffold structure of spiral galaxies

We describe a new formula capable of quantitatively characterizing the Hubble sequence of spiral galaxies including grand design and barred spirals. Special shapes such as ring galaxies with inward and outward arms are also described by the analytic continuation of the same formula. The formula is   r (φ) = A /log [ B tan   (φ/2 N )]  . This function intrinsically generates a bar in a continuous, fixed relationship relative to an arm of arbitrary winding sweep. A is simply a scale parameter while B , together with N , determines the spiral pitch. Roughly, greater N results in tighter winding. Greater B results in greater arm sweep and smaller bar/bulge, while smaller B fits larger bar/bulge with a sharper bar/arm junction. Thus B controls the 'bar/bulge-to-arm' size, while N controls the tightness much like the Hubble scheme. The formula can be recast in a form dependent only on a unique point of turnover angle of pitch – essentially a one-parameter fit, aside from a scalefactor. The recast formula is remarkable and unique in that a single parameter can define a spiral shape with either constant or variable pitch capable of tightly fitting Hubble types from grand design spirals to late-type large barred galaxies. We compare the correlation of our pitch parameter to Hubble type with that of the traditional logarithmic spiral for 21 well-shaped galaxies. The pitch parameter of our formula produces a very tight correlation with ideal Hubble type suggesting it is a good discriminator compared to logarithmic pitch, which shows poor correlation here similar to previous works. Representative examples of fitted galaxies are shown.     

Stochasticity in N-body simulations of disc galaxies

We demonstrate that the chaotic nature of N -body systems can lead to macroscopic variations in the evolution of collisionless simulations containing rotationally supported discs. The unavoidable stochasticity that afflicts all simulations generally causes mild differences between the evolution of similar models but, in order to illustrate that this is not always true, we present a case that shows an extreme bimodal divergence. The divergent behaviour occurs in two different types of code, and is independent of all numerical parameters. We identify and give explicit illustrations of several sources of stochasticity, and also show that macroscopic variations in the evolution can originate from differences at the round-off error level. We obtain somewhat more consistent results from simulations in which the halo is set-up with great care compared with those started from more approximate equilibria, but we have been unable to eliminate diverging behaviour entirely because the main sources of stochasticity are intrinsic to the disc. We show that the divergence is only temporary and that halo friction is merely delayed, for a substantial time in some cases. We argue that the delays are unlikely to arise in real galaxies, and that our results do not affect dynamical friction constraints on halo density. Stochastic variations in the evolution are inevitable in all simulations of disc–halo systems, irrespective of how they were created, although their effect is generally far less extreme than we find here. The possibility of divergent behaviour complicates comparison of results from different workers.     

Regularities in the distribution of star/gas complexes in the spiral arms of our galaxy and M31

The fragmentation of gaseous spiral arms in the outer Galaxy into superclouds has been studied using recently published data on the HI distribution in the Galactic disk. Regular chains of superclouds have been found or confirmed in the Cygnus (Outer) and Carina arms, with the spacings between the superclouds being concentrated near 0.1 and 0.2 of the solar Galactocentric distance. The star complexes in the northwestern arm of the galaxy M31 are spaced, on average, 1.2 kpc apart, with the most distinct chain of complexes being located in the arm region where Beck et al. (1989) detected a strong and wavy (along the arm) magnetic field. Its wavelength turns out to be related to the spacing between the complexes. In this arm, the HII regions lie inside the star complexes, which, in turn, are located inside the gas-dust lane. In contrast, the southwestern arm of M31 is split into a gas-dust lane and a dense stellar arm, which is not fragmented into star complexes. Here, the HII regions are located along the boundary between the gas-dust and stellar components of the arm; other evidence for the presence of a spiral shock wave triggering star formation is also observed, which is probably attributable to the large pitch angle of this segment of the southwestern arm. It may be suggested that the shock wave rapidly leads to star formation everywhere in this arm, while in the northwestern arm, where the shock wave is absent, star formation begins in the superclouds formed along the arm by the magneto-gravitational instability. This is how the chains of star complexes in the northwestern arm of M31 and, obviously, the chains of superclouds in the Carina and Cygnus arms of our Galaxy have been formed. The detection of a regularmagnetic field in the corresponding segments of these arms can be predicted.