| 1. | It suggests that high velocity outflow is easier to occur in massive star formation region
这说明大质量恒星形成区更容易产生高速外流。 |
| 2. | This indicates that there are a lot of high density clumps with different velocities around the massive star formation , which is likely to originate from outflow
这说明在在大质量恒星形成区存在大量的速率不同的高密度分子团块。它们可能起源于外流之中。 |
| 3. | Eventually mode a and b coexist in the wake , which confirms the previous studies . besides , the present paper finds that downstream the streamwise
从圆柱表面到旋涡形成区、到近尾迹再到下游尾迹流向涡结构从模式a转换到模式b 、双涡对模式、再恢复为模式a 。 |
| 4. | Because of the connection between outflow and accretion seen in low - mass stars , surveys of molecular outflows in high - mass ysos can shed light on this debate
因为在低质量恒星形成中外流与吸积相联系，在大质量恒星形成区搜寻分子外流将有助于解决这种争论。 |
| 5. | This breath - taking view spans about 13 degrees across the center of the well - known constellation with the great orion nebula , the closest large star forming region , just right of center
这幅动人心弦的影像涵盖了著名的猎户座中心大约13度的天区，猎户座大星云这个离最邻近的大型恒星形成区，则在影像的中右方。 |
| 6. | To search for high - velocity molecular emission toward massive star formation regions , and to study the connections between h2o masers , iras objects and outflow properties , we carried out a co observation for a h2o maser sample . we found that most of the objects have excess high velocity emission produced by outflows ; we find a significant correlation between co line full widths and iras luminosities . the widths are proportional to the iras luminosities
通过在大质量恒星形成区搜寻高速分子辐射，并且研究它们与星际h _ 2o脉泽源和所联系的红外源之间的关系，我们发现绝大多数源都存在着气体的高速运动并且它们是由分子外流产生的；我们同时发现在co分子的谱线全宽和所对应源的红外光度之间存在很好的相关性，线宽随红外光度增加而变大。 |
| 7. | ( 1 ) in newly - constructed stage and early stage of reclamation , the most important factor of runoff is 30min rainfall intensity . in later stage of reclamation , the most important one is 45min rainfall intensity . and the runoff capacity is the most important influence factor to soil erosion always ; ( 2 ) on the certain degree , loosening surface has an active function to infiltration condition but not to conserve soil ; ( 3 ) the most runoff is formed on platform of stackpile and the soil erosion often happens in the slope ; ( 4 ) stone - soiled dumps have an advantage over soil at respect of erosion resistance so that soil is not adapt in covering slope ; ( 5 ) grass has a better role in conservation of water and soil than arbor in early stage of reclamation ; ( 6 ) arbor - arboret - hemp mix is the best model for conservation
结果显示：在未复垦时期和复垦初期， 30min降雨强度对径流影响最大，复垦后期径流与45min雨强相关性最强，而径流量对土壤侵蚀量的影响始终最大；通过疏松地表岩土只在一定程度上改善地表的入渗条件，并不能起到保土的作用；平台为径流的主要形成区，而土壤侵蚀主要集中在斜坡；土石混排坡的土壤抗蚀性比覆土坡的要大得多，在排土场形成过程中不宜用厚层黄土覆坡；在复垦初期，纯草模式水土保持效果明显好于纯乔模式。 |
| 8. | In order to better understand the excited mechanism of masers , we have studied the time variability of 22 ghz h2o masers in ggd25 , an outburst with the time scales of 4 day was detected . the time variation was probably caused by a collsion pump which led to changes in the pump input
为了更好地理解脉泽的产生机制以及脉泽和恒星形成区的一些典型现象，如它们所联系的远红外源之间的关系，我们研究了22ghzh _ 2o脉泽源的时变以及所有已知的6 . 7ghz甲醇脉泽源的统计性质。 |
| 9. | We have analyised the observed results of low and high spatial resolution observations of molecular line emission toward regions of high - mass star formation which have contributed to the understanding of the physical conditions , morphologies , and dynamics of the molecular gas in the immediate vicinity of recently formed massive stars
本文研究了来自大质量恒星形成区的一些分子谱线的低分辨率和高分辨率观测结果。这些结果有助于我们了解在最近形成的大质量恒星附近分子气体的物理条件，形态以及动力学结构。 |
