Open star clusters in the spiral arms of our Galaxy

We consider the age distributions of open star clusters attributed to three segments of Galactic spiral arms. The smoothed distributions of clusters on the age-Galactocentric angle plane show a great nonuniformity. The time dependence of the formation rate of Galactic disk clusters recovered by taking into account selection effects and dynamical evolution of clusters shows that, on average, the formation rate of open star clusters decreases with time. This is in agreement with the increase in star formation rate into the past, as follows from the study of this process by the method of stellar population synthesis. The present time is the epoch of a current maximum of the cluster formation rate. In addition to the current maximum, there have been at least three more maxima with a period of 300–400 Myr and a duration of no more than 300 Myr. The age distributions are consistent with the pattern of star formation governed by the successive passages of density waves through each examined volume of the Galactic disk. The spiral structure becomes more complex when passing from the inner regions of the Galaxy to its outer regions.     

超新星爆发与暗晕中重子物质的丢失

讨论了在以冷暗物质为主的宇宙中,超新星爆发对矮星系演化的反馈作用。建立了星系的质量丢失模型,提出了理论模型与观测进行比较的方法。对数值计算结果的理论分析表明,当星系外围存在一个暗物质晕时,由超新星爆发引起的质量丢失虽然受到了极大的限制,却不像人们预期的那么困难。如果假定星系的形成红移为ｚ＝２～８,那么,在所选取的参数范围内,理论计算和观测结果是相符合的。这种定性上的符合显示出,星系的质量越小,它们就形成得越早．     

Satellite and ship observations of Kuroshio warm-core ring 93A off Sanriku, northwestern North Pacific, in spring 1997

Synoptic ship and satellite observations were performed of the Kuroshio warm-core ring (KWCR) 93A and its adjacent waters, off Sanriku, northwestern North Pacific, between early April and late June 1997. The temporal and spatial distribution of chlorophylla (Chl-a) and sea surface temperature in the study area were analyzed using data from ADEOS Ocean Color and Temperature Scanner (OCTS) and NOAA Advanced Very High Resolution Radiometer (AVHRR). The objective of this study was to describe the temporal and spatial variability of the spring bloom and understand its relationship with the changes in the hydrographic structure of these waters in and around KWCR 93A. The maximum value of Chl-a concentration in the ring was less than 1 mg/m³ during April. The spring bloom in the ring occurred early in May and the relatively high maximum (>1.0 mg/m³) continued from early in May to mid-June. In late June, a ship-observed surface Chl-a concentration of less than 0.4 mg/m³ suggests that the spring bloom had already declined in and around KWCR 93A. Double spiral structures of warm and cold streamers appeared from late April to mid-May, which may have an influence on the occurrence of the spring bloom in and around the ring. In this episodic event, the warm streamer can maintain the available potential energy of the ring and the strength of upwelling around the ring. The cold streamer provided water with a high Chl-a concentration to the surface layer of the ring. In order to understand the temporal and spatial variability of Chl-a distribution in the ring, the behavior of the warm and cold streamers needs to be taken into consideration.     

旋涡星系颜色梯度的研究进展

旋涡星系的颜色梯度反映了其星族构成沿径向的分布,包含了星系恒星形成历史的信息.因此,对旋涡星系颜色梯度的研究有助于理解星系的形成和演化过程.大部分旋涡星系存在负的颜色梯度,其主要原因是旋涡星系存在星族梯度.颜色梯度与星系的面亮度之间存在内禀的相关,表明质量面密度在星系的形成和演化过程中具有重要作用.     

CT强化幅度与食管癌病理形态学和血管内皮生长因子表达间的关系

目的:对56例食管癌患者血管内皮生长因子(VEGF)表达结果与CT强化峰值参数间进行对照,研究其相关性,为食管癌的影像学诊断及早期发现提供参考依据。方法:56例患者均于术前行CT平扫+动态增强扫描,记录不同扫描时期病灶的CT平扫值、增强峰值;VEGF在正常食管粘膜和食管癌组织中的表达用免疫组织化学法(SP法)测定。所有数据均通过SPSS 21.0统计软件处理。结果:VEGF的表达增强可能是鳞状细胞癌恶性度增高及发生淋巴结转移的标志,CT扫描增强幅度与食管癌中VEGF表达强弱无关。结论:VEGF的表达增强可能是鳞状细胞癌的发生及淋巴结发生转移的标志,CT扫描中病灶增强幅度不能反应肿瘤淋巴结的转移。      

Catalogue of Shakhbazian compact groups of galaxies. IX

The nineth part of the catalogue of Shakhbazian groups contains the positions and references of all the galaxies of the following 48 groups (north of δ < +2°30'): Shkh 216, 217, 218, 219, 220, 221, 222, 223, 224, 225, 226, 227, 228, 229, 230, 231, 232, 233, 234, 235, 236, 237, 238, 239, 240, 242, 243, 244, 245, 246, 247, 248, 249, 250, 251, 253, 254, 255, 256, 257, 258, 259, 260, 328, 338, 339, 340, 340a. For the estimation of the coordinates the Digitized Sky Survey was used.     

On the emptiness of voids

The observability of a galaxy population inside of voids is estimated by assuming a void population similar to the one of nearby field galaxies in density as well as in morphological mixture. Obviously an extension to apparent magnitudes beyond m = 22 for a complete sample of galaxies in a sufficient large field is needed to get reliable information on a void population.