星爆后星系NGC4736核区的环状结构

在１９９２年３月３１日至４月２日期间，我们利用云南天文台１ｍ望远镜２号ＣＣＤ和缩焦装置，对环星系ＮＧＣ４７３６进行了Ⅴ和Ⅰ波段深曝光观测。在经过Ｒｉｃｈａｒｄｓｏｎ－Ｌｕｃｙ图象复原以及自适应滤波两种方法处理后，发现仅仅在Ⅴ波段图象上，其核区存在一个直径约为１０″的环状结构。     

Circular Polarization in Pulsar Integrated Profiles： Updates

We update the systematic studies of circular polarization in integrated pulse profiles by Han et al. Data of circular polarization profiles are compiled. Sense reversals can occur in core or cone components, or near the intersection between components. The correlation between the sense of circular polarization and the sense of position angle variation for conal-double pulsars is confirmed with a much large database. Circular polarization of some pulsars has clear changes with frequency. Circular polarization of millisecond pulsars is marginally different from that of normal pulsars.     

A Catalog of Luminous Infrared Galaxies in the IRAS Survey and Second Data Release of SDSS

We selected a sample of luminous infrared galaxies by cross-identification of the Faint Source Catalogue (FSC) and Point Source Catalogue (PSC) of the IRAS Survey with the Second Data Release of the SDSS. The size of our sample is 1267 for FSC and 427 for PSC by using the 2σ significance level cross-section. The "likelihood ratio" method is used to estimate the individual's reliability and for defining two more reliable subsamples (908 for FSC and 356 for PSC). A catalog of infrared, optical and radio data is compiled and will be used in further work. Some statistical results show that luminous infrared galaxies are quite different from ultra-luminous infrared galaxies. The AGN fractions of galaxies at different infrared luminosities and the radio-infrared correlations are consistent with the previous studies.     

活动星系核（AGN）的宽线区（BLR）（Ⅱ）

ＡＧＮ天体的主要特征之一，就是它们的光谱中有宽而强的发射线，因此，这些宽发射线的产生区域ＢＬＲ为人们提供了一个了解ＡＧＮ天体物理本质的独特而重要的场。在文中围绕讨论了ＢＬＲ基本物理特征，评述近年来有关的理论和观测研究进展及其现状在文（Ⅱ）中主要涉及ＢＬＲ的几何结构和尺度及其运动学研究的进展和现状。     

3C390.3的弱秒差距尺度喷流及其变化

通过对射电星系３Ｃ３９０．３在历元１９８９．２９及６ｃｍ波长的ＶＬＢＩ观测数据的多软件包成象，辨认出其弱秒差距尺度喷流中几个分离的节，将它们和以前发表及未发表的同一波长的成象结果比较，显示了该源弱秒差距尺度喷流的弯曲和反喷流，并重新证认了喷流中节的视超光速运动。     

星系的恒星速度弥散度的归算方法

星系的恒星视向速度分布是星系动力学模型的重要观测约束,其特征参数包括速度弥散度、分布轮廓以及红移。这些参数对研究星系的动力学、结构和演化以及中央黑洞的质量等都具有重要的价值。该文全面总结了从星系光谱归算星系的恒星视向速度分布及其弥散度的各种方法,以及对观测和处理的一些要求。这些方法都假设星系谱线可看作是模板星光谱经多普勒位移并加宽后的线性叠加。提取尽可能多的星系内部恒星运动信息、减少模板星失配的影响、简化误差分析,是这些方法追求的目标。     

A Statistical Model for Predicting the Average Abundance Patterns of Heavier Elements in Metal-Poor Stars

We have collected nearly all the available observed data of the elements from Ba to Dy in halo and disk stars in the metallicity range -4.0 <[Fe/H]< 0.5. Based on the observed data of Ba and Eu, we evaluated the least-squares regressions of [Ba/Fe] on [Fe/H], and [Eu/H] on [Ba/H]. Assuming that the heavy elements (heavier than Ba) are produced by a combination of the main components of s- and r-processes in metal-poor stars, and choosing Ba and Eu as respective representative elements of the main s- and the main r-processes, a statistical model for predicting the Galactic chemical evolution of the heavy elements is presented. With this model, we calculate the mean abundance trends of the heavy elements La, Ce, Pr, Nd, Sm, and Dy with the metallicity. We compare our results with the observed data at various metallicities, showing that the predicted trends are in good agreement with the observed trends, at least for the metallicity range [Fe/H]> -2.5. Finally, we discuss our results and deduce some importa     

“视界”与退行速度大于光速的星系可否被观测到的问题

对于“我们能否观测到退行速度大于光速的星系”这个问题，目前大多数宇宙学家将回答：“不能，因为这些星系处在我们的视界之外”，这里的思想是，相对论宇宙学中的速度必须由相对论多普勒红移公式来定义，然而在宇宙学中，红移是“宇宙学”的而非“多产勒”的，并且有一个速度的独立定义可以应用。     

活动星系核的多波段能谱及其发射机制──Ⅱ．红外连续辐射能谱

本文讨论了１６个红外强ＰＧ类星体的红外辐射能谱。我们假设这些活动星系核的红外谱是由非热辐射机制和尘埃的热辐射共同产生的，通过对红外包的最佳拟合，我们发现大多数ＰＧ类星体的红外包位于７一２４μ的中远红外区，尘埃的热辐射机制能很好地产生观测到的红外包。通过模拟能定量地说明尘埃产生的热致辐射在这些天体的红外谱中的相对重要性，在模型与观测值之间的拟合中，我们得到了在这些天体中核加热的尘埃区的大小、尘埃的分布等模型参数。