Discovery of Multiple outflows in IRAS 06056＋2131

We report a discovery of multiple outflows in IRAS 06056 2131. The high angular resolution image (～ 15“) of CO(1-0) emission reveals that the structure of outflow is very complicated. The outflow appears to be everywhere.Its configuration only show a bipolar outflow at observation of both low resolution and low signal-to-noise ratio,while two bipolar outflows can be detected when observed by both high resolution and high signal-to-noise ratio mapping. This result is significant in the understanding of the physical processes that occur at early phase of massive stars.     

Orion KL超水微波激射辐射的“宁静相”物理特征

利用紫金山天文台青海观测站的13.7m的射电望远镜,观测OrionKL分子云的水微波激射辐射发现这个区的微波激射活动处于”宁静”状态,峰值流量为3×10⁴Jy,大约比爆发相微波激射辐射低两个数量级宁静水微波激射处于完全饱和的辐射过程,微波激射活动区的亮温度为3×10¹³K,氢分子数密度为8×10¹⁴m^-3,微波激射辐射两能级之间的布居反转粒子数密度为5×10⁵(H₂O)m相似文献   

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.     

乌鲁木齐25 m射电望远镜首次水脉泽观测

在乌鲁木齐天文站的25 m射电望远镜上,安装了一套新的谱线接收系统,其终端频谱分析器为声表面波频谱仪,在世界上这是第1次实际应用于射电天文观测.对于这类新的频谱分析器,仔细地考虑了谱线观测的天文校准问题.用这套谱线接收系统观测了一批强弱不等的银河系内水脉泽源,给出了W49N,W3(OH),2248+600和1909+090的观测谱.发现W49N高速脉泽子源的LSR速度覆盖从-330一直延展到146 km/s,这是这个源观测到的最宽的速度范围.与意大利Medicina 32 m天线的观测结果比较以后,发现W3(OH)谱中LSR速度为 -52 km/s 的脉泽子源有激烈的流量密度变化.     

VY CMa水脉泽辐射的短时标变化

利用紫金山天文台青海观测站的13.7m毫米波射电望远镜,在1993年8月26日～9月24日的近1个月的时间里,每天监视大犬座VY(VYCMa)红超巨星拱星气体壳层中水脉泽辐射.发现一个强度相对变化为20%～25%,周期为10.3d的类正弦的快速振荡.这是迄今在红巨星中发现的变化周期最短的水脉泽辐射、给出了这个源的水分子脉泽谱线以及它的变化形态;利用细管状的完全饱和水脉泽辐射理论,估计了脉泽活动区的物理性质;初步分析了这种快速变化的成因.     

年青恒星形成区ON1的物理特征

本文给出了波长1.3cm和2cm上,恒星形成区ON1的VLA连续辐射射电图。用壳模型计算获得氢Ⅱ区的电子数密度大约为10⁴/cm³量级,整个氢Ⅱ区的总质量为10^-3太阳质量,电离气体的中心很可能是一颗非常年青的B类恒星。详细分析了壳型氢Ⅱ区辐射的谱形态,并导出一组从谱分析获得氢Ⅱ区物理参量的方程。对于ON1,热星风扫积而成的壳层大约为0.005pc,电子数密度随径向分布的幂指数为2.6,壳层中的平均电子数密度为10⁴/cm³。我们认为对于那些不能分辨而又有壳型结构的氢Ⅱ区,谱分析可能是获得源结构讯息和物理性质的有效途径。