星际型CH_3CN－H_2含超精细能级的碰撞跃迁速率系数的理论计算

利用ＩＯＳ近似模型，计算了星际分子云条件下Ｅ型ＣＨ３ＣＮ－Ｈ２含超精细能级的的碰撞跃迁速率系数。其温度范围是２０Ｋ－１４０Ｋ。为研究分子云与恒星形成区的物理、化学性质提供了大量有用的基础分子数据。     

W51A的谱线与连续谱研究——CO,NH3谱线与3mm连续谱

以研究星系旋臂上大质量星形成区为目的，对W51 IRS1为中心的5′×4′(约等于11pc×9pc)天区的3.4mm的连续谱和CO(J=1.0)线作观测，并对NH₃(1,1),(2,2),(3,3)和(4,4)四反演线作同时观测.氨分子的谱形分析和辐射转移统计平衡计算结果表明,在波长3.4mm连续谱的W51 IRS1,IRS2以及(e1/e2)源中心方向的NH₃反演线谱有来自HⅡ区前的氨分子的相对发射线红移的吸收特征；由东部边缘区向中心,有密度3～10倍的递增趋势,进一步显示了光学不可见的分子云核的塌缩现象.在以IRS1为中心40″为半径的圆内的各个射电、近(远)红外、UCHⅡ源所形成的外场辐射对区内分子(例如NH₃)的激发产生不可忽略的影响.CO(J=1.0)的谱形在此圆区内由东到西发生由不对称的双峰(约等于60,68km·s^-1)转化为三峰,即与致密电离氢区G49.4-0.3成协的约等于53 km·s^-1分量亦在谱线上呈现.可见40″圆区内有明显的大质量星形成的各种活动迹象.     

The interstellar methanol masers and their environments

To promote the understanding of massive star formation processes, we have studied the 6.6 GHz methanol (CH3OH) masers and their environments-- the dense cores and the outer regions of the molecular cloud. The physics of the CH3OH maser or the thermal emission formation region is studied by fitting the observational data of the 6.6 GHz 51-60 A+ and the 107 GHz 31-40 A+ CH3OH maser emission, using the radiative transfer calculations. The type II characteristics of the 6.6 GHz CH3OH maser are confirmed by the calculation results. A greater intensity of the radiation field leads to an increase in the peak intensity of the maser; however, high densities tend to turn off the maser. The calculation results show that to be a maser the 6.6 GHz CH3OH emission needs a radiation field of 150-300 K and a density not higher than 107cm-3, while the 107 GHz emission requires a radiation field of 210-300 K and a density not higher than 3×106 cm-3. The 6.6 GHz line is maser towards all six studied sources, while the 107 GHz line is maser towards Cep A only. Moreover, the former's intensity is much stronger than the latter. The radiative transfer calculations also indicate that the 6.6 GHz maser emission is so strong that the requirements of its formation (e.g. The radiation field, the density and the kinetic parameters) can only be satisfied at a certain stage of the processes of the massive star formation. Therefore it is often used as one of the most prominent tracers for the massive star formation regions. The calculation results of the simultaneous observations of (1,1) through (4,4) inversion lines of the ammonia (NH3) indicate that both the temperature and the density in the 6.6 GHz CH3OH maser formation regions are higher than that of the NH3 line formation regions. Furthermore, the common fact of |Vlsr(CO)| ＞ |Vlsr(NH3)| ＞ |Vlsr(CH3OH 6.6GHz maser)| in all six sources implies the ongoing developing trends of those gas flows driven by the masers.     

世纪之交的天体物理与原子分子物理

20世纪的后叶 ,原子与分子的射电谱线揭示了光学不可见的冷宇宙 ,银河系最大天体 -巨分子云和恒星形成过程的一个普遍存在的重要的相 -双极外流。近十年发射的红外天文卫星ISO,通过对原子与分子的红外谱线的观测 ,在研究动能温度数百度以上的富碳、富氧演化星包层 ,行星状星云、年轻星和恒星形成区复合体的物理与动力学性质方面取得重要的结果 ,并向原子与分子物理学家提出许多问题和要求。原子与分子物理与天体物理在急剧的发展中将互相激发 ,碰撞出更绚丽的火花。     

全等三角形创新题例析

全等三角形是初中生必须掌握的三角形两大知识点之一.三角形全等为解决线段相等、角相等的问题提供了重要工具,也是各省市中考的热门内容.近些年来出现了很多新颖别致的试题以及新编制的练习题,引起师生的关注.现举例解析.     

前沿与基础：宇宙物质和过程的研究与原子分子物理

原子、分子是物质结构的第一个微观层次，是通向下两个微观层次———原子核和粒子的大门．原子分子物理在宇宙物质和过程的研究中起到基础理论的重要作用，而宇宙物质和过程的前沿研究则向原子分子物理提供了许多新的生长点．天体中有无止境的原子分子物理问题有待于人们探讨与研究     

原子分子物理—研究宇宙物质的基础科学

艹勾清泉教授所从事、发展和传授的原子、分子结构理论在天体物理、天体化学、固体物理、材料科学以及极端条件物理的发展中起到基础理论的重要作用。他的研究群体活跃在各个相关的基础与应用领域里     

ATOMIC AND MOLECULAR PHYSICS AND ASTROPHYSICS

In astronomy,distant objects are studied through observation of electro-magnetic radiation of various wavelengths or through detection of cosmic rayparticles.The spectrum of the radiation consists of continuum and discrete-line components.Except for the continuous emission from the space plasmasor from the solid particles with finite temperature,most of the spectral fea-tures reflect the nature of the atoms or molecules in space which emit or ab-sorb the radiation.Then,how can one obtain the new astronomical informa-     

天体原子、离子和分子射电谱线研究进展

简述天体原子、离子和分子射电谱线自首次探测至今,半个世纪以来的研究进展.展示空间特有的非地球稳定的自由基、同位素、同位素分子和离子及其相关的过程.天体微波激射(MASER)因能提供恒星诞生与死亡的珍贵信息成为本文之侧重点.