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.     

星际分子及其谱线

介绍了星际分子及其谱线的研究历史和现状,分析了如何从分子谱线探索恒星形成区的物理化学性质,简述了探测星际分子谱线的大型射电望远镜.     

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。     

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.     

星际分子及其谱线

介绍了星际分子及其谱线的研究历史和现状，分析了如何从分子谱线探索恒星形成区的物理化学性质，简述了探测星际分子谱线的大型射电望远镜。     

超致密电离氢区周围的CO高速气体

给出了与星际水脉泽源和超致密电离氢区成协的77个恒星形成区的高速¹²CO（J＝1-0）分子辐射的搜寻结果. 目的是调查高速分子外流、星际H2O脉泽源和它们所联系的红外源之间的关系. 样本满足WC标准，即：lg(F_25μm/F_12μm)＞0.57和lg(F_60μm/F_12μm)＞1.3.绝大多数源都存在着气体的高速运动，在1σT*_a水平处，几乎70％的源的谱线全宽(FW）超过15 km·s^-1，15％的源则超过了30 km·s^-1.这个结果极大地超过了小质量恒星形成区所得到的值.在CO分子的FW，半峰全宽（FWHM）和源的红外光度之间存在清楚的相关性，两种线宽的值正比于红外光度的值.这些关系表明了亮源能够注入更多的能量进入它周围物质中从而产生更强有力的外流使得CO分子的线宽增大.从CO分子和水脉泽的峰值速度的对应关系中发现一些水脉泽源相对于其附近的气体呈现出大的蓝移，这也许是由非饱和脉泽放大了背景源引起的.     

High-velocity gas associated ultracompact HII regions

We present the results of a survey for high-velocity¹²CO (1-0) emission associated H₂O masers and ultracompact (UC) HII regions. The aim is to investigate the relationship between H₂O masers, CO high-velocity gas (HVG) and their associated infrared sources. Our sample satisfies Wood & Churchwell criterion. Almost 70 % of the sources have full widths (FWs) greater than 15 km · s^-1 atT* _a = 100 mK and 15 % have FWs greater than 30 km · s^-1 In most of our objects there is excess high velocity emission in the beam. There is a clear correlation between CO line FWs and far-infrared luminosities: the FW increases with the FIR luminosity. The relation suggests that more luminous sources are likely to be more energetic and able to inject more energy into their surroundings. As a result, larger FW of the CO line could be produced. In most of our sources, the velocities of peak of the H₂O emission are in agreement with those of the CO cloud, but a number of them have a large blueshift with respect to the CO peak. These masers might stem from the amplifications of a background source, which may amplify some unobservable weak masers to an observable level.     

介孔钛纳米复合团簇应用于光热-光动力疗法

在本文,采用水热法合成了一种新型的介孔二氧化钛/碳/亚甲蓝复合纳米团簇(TiO₂@C-MB),并应用于肿瘤细胞的光动力(PDT)和光热治疗(PTT)。系统中介孔二氧化钛作为有效的光敏剂,MB作为重要的光敏添加剂以改善二氧化钛纳米晶的光化学效应,并将其光响应区域拓宽至光动力学疗法的理想治疗窗(650~900 nm)。柠檬酸在水热条件下被还原成碳并裹覆在二氧化钛表面。碳层表现出良好的光热效果,也充当多功能的电子受体以加速生成单线态氧。该纳米团簇不仅可以保持肿瘤细胞内部高浓度的MB和二氧化钛以产生大量的单线态氧杀死肿瘤细胞,而且可以避免MB退化失活。     

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.