爱格耐F.M.EXNER传

二月七日(民国十九年)平旦,奥大利中央气象学及地力学研究院院长,维也纳大学大地物理学教授爱格耐卒於维也纳。一心悸病,而促其寿纪,而当代气象学,丧一硕儒,而德意志气象学者之林,丧一模楷,而故旧朋好,丧一信友。年来爱格耐君,体气日渐颓败,凡有幸得     

太阳过渡区爆发事件的观测及理论研究进展

太阳过渡区爆发事件是过渡区重要的小尺度活动现象之一,常被过渡区的紫外和极紫外谱线观测到。典型的爆发事件的寿命为60～360 s,现象出现时谱线形状呈非高斯形,谱像两翼显示双向喷流结构,喷流速度大致在100 km·s~(-1),与色球局地阿尔芬速度相当。普遍认为其产生原因为小尺度快速磁重联。主要回顾了爆发事件的观测特征及其光谱学诊断方法,阐述了爆发事件的物理形成机制及与其他过渡区小尺度结构的联系,并讨论其在太阳风形成和日冕加热过程中对物质及能量输运的影响。最后对未来爆发事件的研究提出了展望。     

利用水文地球化学和水文物理学方法分析定襄七岩泉水氡异常

自2008年以来,定襄七岩泉水氡测值处于相对高值状态,为了核实该异常,利用水文地球化学和水文物理学方法进行分析,结果认为：七岩泉泉水补给来源主要是大气降水,当累计连续降雨量超过一定阈值（116 mm）时,水氡测值明显下降;降雨仅对水氡测项的短临动态造成干扰,年变动态不受影响。调查发现,与七岩泉相距不远的静乐井水位出现准同步高值现象,综合分析认为,七岩泉水氡高值异常反映了区域内地壳应力的变化。     

辽源市人工增雨工作的发展思考

一人工增雨的原理 人工增雨以云物理学为基础,通过在大气中播撒各种催化剂,使大气中的云物理结构发生变化,从而达到增加降水的效果。     

北京地区一次持续性大雾的宏观物理特征

通过分析北京地区2004年11月30日和12月2日出现的两场大雾生成的天气背景,大雾生成阶段和消散阶段的温度、湿度、气压和风场特征,探讨北京地区大雾的宏观物理特征。所用数据资料是通过系留气球探测所得,分析了气象要素的廓线和时间剖面图特征,从而得到了北京地区有雾生成时的天气背景特征;辐射雾与平流雾的能见度变化区别,雾生成时、持续阶段及雾消散前温度场、湿度场的变化特征;逆温层在辐射雾和平流雾中的形成原因和作用都不同;比湿值增大是判断有暖湿平流带来水汽的重要指标;气压变化平稳、缓慢,使强对流没有发生,逆温层不能被冲破,雾能长时间维持。     

WRF模式对澳洲一次热带深对流系统的模拟研究

利用WRF(Weather Research Forecast)模式和1 °×1 °NCEP全球分析资料对2005年11月16日澳大利亚北部Tiwi岛上的一次热带深对流个例进行了数值模拟,对模式网格分辨率和微物理参数化方案的影响进行了敏感性试验,并与实测资料进行了对比。试验结果显示：模式较好地再现了这次热带对流云的日变化特征,即早期降水由沿岸的海风锋初始对流形成,之后出现单体合并现象并最终形成成熟的深对流系统。但是,模式在模拟深对流系统出现的时间及位置方面仍然需要改进。敏感性试验显示,就本次个例而言,二重嵌套方案在降水分布以及降水强度方面的模拟结果比非嵌套方案更接近实际探测。另外,微物理过程参数化方案对降水量的模拟也有一定影响,采用Purdue Lin方案的模拟结果更接近于实测情况。     

地震沉积学探讨及应用

地震沉积学是在油气勘探开发的需要下产生的,具有鲜明的技术特色和良好的应用前景。文章阐述了地震沉积学的概念和学科特点,认为地震沉积学可以按研究尺度分为地震地貌学和储层地震学,从应用角度提出了地震沉积学的研究思路,并首次提出最小等时研究单元的概念,即三相（地震相,测井相,岩芯相）结合研究时井震统一的尺度,是沉积分析时一个最小的地质成图单元。文章选择鄂尔多斯盆地塔巴庙D气田上古生界岩性油气藏为例,阐述了地震沉积学分析技术在沉积相分析方面的应用方法,展示了地震沉积学研究技术在建立精细等时地层格架,岩相物理分析,多属性地震相分析等方面良好的学科优势。     

研究人员的好参考书、研究生入门的好教材——《太阳活动区物理》

专著<太阳活动区物理>最近由南京大学出版社出版和发行.该专著由作者,南京大学方成院士、丁明德教授和陈鹏飞教授,以多年来的太阳物理学研究和指导研究生的科研为基础,并结合国内外太阳物理学最新研究成果编写而成的,主要阐述了研究太阳活动区和各种太阳活动现象的观测事实、基本理论、基本方法和主要研究成果.     

PDR diagnostics study with CLOUDY

A series of plane-parallel photodissociation region (PDR) models are calculated using the spectral synthesis code CLOUDY. These models span a wide range of physical conditions, with gas densities of n = 102 - 106 cm-3 and incident far-ultraviolet (FUV) fields of G0 = 100 - 106 (where Go is the FUV flux in units of the local interstellar value), which are comparable with various astrophysical environments from interstellar diffuse clouds to the dense neutral gas around galactic compact HII regions. Based on the calculated results, we study the thermal balance of PDR gas and the emissions of [ CII ], [ CI ] and [ OI ] fine-structure lines under different physical conditions. The intensities and strength ratios of the studied lines, which are frequently used as PDR diagnostics, are presented using contour diagrams as functions of n and Go. We compare the calculated PDR surface gas temperatures T8 with those from Kaufman et al. and find that Ts from our models are systematically higher over most of the adopted n-G0 parameter space. The predicated line intensities and ratios from our work and those from Kaufman et al. can be different by a factor greater than 10, and such large differences usually occur near the border of our parameter space. The different methods of treating the dust grain physics, the change of H2 formation and dissociation rates, and the improvement in the radiation transfer of line emissions in our CLOUDY models are likely to be the major reasons for the divergences. Our models represent an up-to-date treatment of PDR diagnostic calcula- tions and can be used to interpret observational data. Meanwhile, the uncertainties in the treatment of microphysics and chemical processes in PDR models have significant effects on PDR diagnostics.     

A super-high angular resolution principle for coded-mask X-ray imaging beyond the diffraction limit of a single pinhole

High angular resolution X-ray imaging is always useful in astrophysics and solar physics. In principle, it can be performed by using coded-mask imaging with a very long mask-detector distance. Previously, the diffraction-interference effect was thought to degrade coded-mask imaging performance dramatically at the low energy end with its very long mask-detector distance. The diffraction-interference effect is described with numerical calculations, and the difffraction-interference cross correlation reconstruction method (DICC) is developed in order to overcome the imaging performance degradation. Based on the DICC, a super-high angular resolution principle (SHARP) for coded-mask X-ray imaging is proposed. The feasibility of coded mask imaging beyond the diffraction limit of a single pinhole is demonstrated with simulations. With the specification that the mask element size is 50 × 50 μm2 and the mask-detector distance is 50 m, the achieved angular resolution is 0.32arcsec above about 10keV and 0.36arcsec at 1.24keV (λ = 1 nm), where diffraction cannot be neglected. The on-axis source location accuracy is better than 0.02 arcsec. Potential applications for solar observations and wide-field X-ray monitors are also briefly discussed.