| W51M分子云中H和He复合线的观测研究 |
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| 引用本文： | 张燕坤,朱逢尧,唐孟尧,秦胜利,汪敏.W51M分子云中H和He复合线的观测研究[J].天文学报,2020,61(2):13-29. |
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| 作者姓名： | 张燕坤 朱逢尧 唐孟尧 秦胜利 汪敏 |
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| 作者单位： | 中国科学院云南天文台昆明650011;中国科学院大学北京100049,中国科学院上海天文台上海200030,云南大学天文系昆明650011,云南大学天文系昆明650011,中国科学院云南天文台昆明650011;中国科学院大学北京100049 |
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| 基金项目： | 国家自然科学基金项目(U1631121)资助 |
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| 摘 要： | W51M (W51 Main)是一个和HⅡ区成协的大质量恒星形成区,在其中可以探测到众多的分子谱线和H、He射电复合线.中国科学院上海天文台基于天马65 m望远镜对W51M的观测数据,证认了主量子数在74–117之间的H、He复合发射线,其中主量子数在74–78之间的H和He的α复合线均被探测到.结合H和He复合线的多普勒致宽,算出该HⅡ区的电子温度约为7400 K, He+/H+的离子丰度比约为0.09,这与已有的研究基本吻合.考虑高信噪比的复合线,即H(n)α(74n78),计算得出W51M的平均湍动速度是13.767 km·s-1.通过确定W51M或其他HⅡ区中的复合线,获取电子温度、湍动速度以及其他物理参量,在电子数密度、元素丰度、恒星形成率等方面进行了探讨,对分子谱线以及其他波段的复合线研究具有借鉴意义.
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| 关 键 词： | 谱线:复合线 星际介质:H_Ⅱ区 星际介质:云 星际介质:分子 厘米:星际介质 |
| 收稿时间： | 2019/7/2 0:00:00 |
Observation of H and He Recombination Lines in W51M Molecular Cloud |
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| ZHANG Yan-kun,ZHU Feng-yao,TANG Meng-yao,QIN Sheng-li and WANG Min.Observation of H and He Recombination Lines in W51M Molecular Cloud[J].Acta Astronomica Sinica,2020,61(2):13-29. |
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| Authors: | ZHANG Yan-kun ZHU Feng-yao TANG Meng-yao QIN Sheng-li and WANG Min |
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| Affiliation: | Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011;University of Chinese Academy of Sciences, Beijing 100049,Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030,Department of Astronomy, Yunnan University, Kunming 650011,Department of Astronomy, Yunnan University, Kunming 650011 and Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011;University of Chinese Academy of Sciences, Beijing 100049 |
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| Abstract: | W51M (W51 Main) is a massive star-forming region associated with the H$_II$ region, in which numerous molecular lines, H and He recombination lines can be detected. Study of these lines is helpful to understand the properties and physical environment of W51M. Based on the observation data of the Tianma 65-meter telescope, owned by Shanghai Astronomical Observatory, Chinese Academy of Sciences, the H and He recombination lines of the main quantum number between 74 and 117 were detected. Combined with their Doppler broadening, the electron temperature of the nebula was calculated. It was found that the electron temperature of the H$_II$ region was about 7400K, and the He+/H+ ionic abundance ratio was about 0.09, which was basically consistent with previous results. Considering the high signal-to-noise ratio of those recombination lines, i.e. H$(n) \alpha(74\leqslant n \leqslant 78)$, the calculated average turbulent velocity of W51M is 13.767kmcdots-1. This work discusses the identification of recombination lines in W51M or other H$_II$ regions, and the acquisition of electron temperature, turbulent velocity, and other physical parameters, such as electron number density, the element abundance, and star formation rate. So it is of positive significance for future study. |
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| Keywords: | spectral lines: recombination lines interstellar medium (ISM): H$_II$ region ISM: clouds ISM: molecules centimeter: ISM |
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