LAMOST光谱库中的OB星研究
发布时间：2021-10-27 00:25
大质量星（通常是指质量大于8M⊙）是宇宙中元素增丰和再电离的主要原因,因此它们在其宿主星系的演化过程中扮演了重要的作用。OB星作为大质量恒星,主要通过紫外辐射、星风损失和最终的核塌缩超新星爆炸等方式,对宇宙中的星际介质、元素增丰、恒星形成和星系演化等产生重要的影响。另外,OB星具有短寿命的特点,也是研究恒星形区成、分子云分布的重要探针。目前,国际上已知的银河系OB星样本主要来自于太阳邻域其数目有限,因而证认出更多的覆盖空间范围更广的银河系OB星样本,对于研究银河系的结构、恒星形成及与大质量星相关的恒星物理有着重要的意义。本工作基于LAMOST DR4的庞大恒星光谱数据,研究了银河系OB星的光谱特征和空间分布,发展了基于精确的光谱计算得到的谱指数方法,利用该方法成功挑选出了11,676颗OB星,其中包括59颗O型星和11,627颗B型星,并经过了人眼的反复检验。事实证明,我们的谱指数方法可以有效地剔除大量的非OB星样本,大大提高了工作效率。由于时间原因,我们无法用眼睛完成所有OB星的光谱型和光度型分类工作。我们只是从中挑选出了1,505颗OB星,并用眼睛进行了详细的...
【文章来源】：河北师范大学河北省
【文章页数】：47 页
【学位级别】：硕士
【部分图文】：
LAMOST光谱中的典型的OB星光谱，红色的代表O9V，蓝色的代表B3V识别出HeI4009，40264121,4144,4387,4471,4713吸收线：HeII4200,4541,4686吸收谱线，氢的巴耳末线在4202(Hδ),4341(H),还有MgII4481，CII4267也识别出来
O2 和 O3 的区别在巴耳末线的强度（即谱线的等值情况下，O3 光谱中的巴耳末线强度要强于 O2。6：存在 He I 的谱线, He II4541 和 He I4471 的比值大于 1。线也是一个判断标准。He II4541/He I4471 的比值小于 1，同时 He I4471 与 He II另外 O7 中还存在弱的 N III4634-4640-4642 发射线。- O9： He I 线开始出现并且逐渐增强， N III4634-4640-4I4686 与 He I4471 吸收线的比值，和 He II4686 与 O II465高低的标准。O9 光谱中的 Si IV4089 也要强于 O II 的 407
1.3 O2V-O9V 的主序星光谱，图中标注的谱线是 He I+II4026、He I4144、4387、4471吸收谱线:He II4200、4541、4686 的吸收谱线。在 O2V 和 O3V 型星中 的是 N IV4058射谱线，N V4606-4620 的吸收谱线和 N III4634-4640-4642 发射谱线.（图中均为 MK分类系统的标准星）
【参考文献】：
期刊论文
[1]Spectral classification of stars based on LAMOST spectra[J]. Chao Liu,Wen-Yuan Cui,Bo Zhang,Jun-Chen Wan,Li-Cai Deng,Yong-Hui Hou,Yue-Fei Wang,Ming Yang,Yong Zhang. Research in Astronomy and Astrophysics. 2015(08)
[2]The Large Sky Area Multi-Object Fiber Spectroscopic Telescope （LAMOST）[J]. Xiang-Qun Cui2, Yong-Heng Zhao1, Yao-Quan Chu3, Guo-Ping Li2, Qi Li1, Li-Ping Zhang2, Hong-Jun Su1, Zheng-Qiu Yao2, Ya-Nan Wang2, Xiao-Zheng Xing3, Xin-Nan Li2, Yong-Tian Zhu2, Gang Wang1, Bo-Zhong Gu2, A-Li Luo1, Xin-Qi Xu2, Zhen-Chao Zhang2, Gen-Rong Liu2, Hao-Tong Zhang1, De-Hua Yang2, Shu-Yun Cao1, Hai-Yuan Chen2, Jian-Jun Chen1, Kun-Xin Chen2, Ying Chen1, Jia-Ru Chu3, Lei Feng1, Xue-Fei Gong2, Yong-Hui Hou2, Hong-Zhuan Hu3, Ning-Sheng Hu2, Zhong-Wen Hu2, Lei Jia1, Fang-Hua Jiang2, Xiang Jiang2, Zi-Bo Jiang2, Ge Jin3, Ai-Hua Li2, Yan Li4, Ye-Ping Li2, Guan-Qun Liu2, Zhi-Gang Liu3, Wen-Zhi Lu2, Yin-Dun Mao4, Li Men1, Yong-Jun Qi2, Zhao-Xiang Qi4, Huo-Ming Shi1, Zheng-Hong Tang4, Qing-Sheng Tao2, Da-Qi Wang1, Dan Wang1, Guo-Min Wang2, Hai Wang2, Jia-Ning Wang2, Jian Wang3, Jian-Ling Wang1, Jian-Ping Wang3, Lei Wang2, Shu-Qing Wang1, You Wang2, Yue-Fei Wang2, Ling-Zhe Xu2, Yan Xu1, Shi-Hai Yang2, Yong Yu4, Hui Yuan1, Xiang-Yan Yuan2, Chao Zhai3, Jing Zhang5, Yan-Xia Zhang1, Yong Zhang2, Ming Zhao4, Fang Zhou2, Guo-Hua Zhou2, Jie Zhu2 and Si-Cheng Zou1 1 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; 2 Nanjing Institute of Astronomical Optics and Technology, National Astronomical Observatories, Chinese Academy of Sciences, Nanjing 210042, China 3 University of Science and Technology of China, Hefei 230026, China 4 Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China 5 Institute of Architecture Design and Research, Chinese Academy of Sciences, Beijing 100190, China. Research in Astronomy and Astrophysics. 2012(09)
[3]LAMOST spectral survey——An overview[J]. Gang Zhao 1 , Yong-Heng Zhao 1 , Yao-Quan Chu 1 , 2 , Yi-Peng Jing 3 and Li-Cai Deng 1 1 Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China;2 University of Science and Technology of China, Hefei 230026, China 3 Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China. Research in Astronomy and Astrophysics. 2012(07)
本文编号：3460497
【文章来源】：河北师范大学河北省
【文章页数】：47 页
【学位级别】：硕士
【部分图文】：
LAMOST光谱中的典型的OB星光谱，红色的代表O9V，蓝色的代表B3V识别出HeI4009，40264121,4144,4387,4471,4713吸收线：HeII4200,4541,4686吸收谱线，氢的巴耳末线在4202(Hδ),4341(H),还有MgII4481，CII4267也识别出来
O2 和 O3 的区别在巴耳末线的强度（即谱线的等值情况下，O3 光谱中的巴耳末线强度要强于 O2。6：存在 He I 的谱线, He II4541 和 He I4471 的比值大于 1。线也是一个判断标准。He II4541/He I4471 的比值小于 1，同时 He I4471 与 He II另外 O7 中还存在弱的 N III4634-4640-4642 发射线。- O9： He I 线开始出现并且逐渐增强， N III4634-4640-4I4686 与 He I4471 吸收线的比值，和 He II4686 与 O II465高低的标准。O9 光谱中的 Si IV4089 也要强于 O II 的 407
1.3 O2V-O9V 的主序星光谱，图中标注的谱线是 He I+II4026、He I4144、4387、4471吸收谱线:He II4200、4541、4686 的吸收谱线。在 O2V 和 O3V 型星中 的是 N IV4058射谱线，N V4606-4620 的吸收谱线和 N III4634-4640-4642 发射谱线.（图中均为 MK分类系统的标准星）
【参考文献】：
期刊论文
[1]Spectral classification of stars based on LAMOST spectra[J]. Chao Liu,Wen-Yuan Cui,Bo Zhang,Jun-Chen Wan,Li-Cai Deng,Yong-Hui Hou,Yue-Fei Wang,Ming Yang,Yong Zhang. Research in Astronomy and Astrophysics. 2015(08)
[2]The Large Sky Area Multi-Object Fiber Spectroscopic Telescope （LAMOST）[J]. Xiang-Qun Cui2, Yong-Heng Zhao1, Yao-Quan Chu3, Guo-Ping Li2, Qi Li1, Li-Ping Zhang2, Hong-Jun Su1, Zheng-Qiu Yao2, Ya-Nan Wang2, Xiao-Zheng Xing3, Xin-Nan Li2, Yong-Tian Zhu2, Gang Wang1, Bo-Zhong Gu2, A-Li Luo1, Xin-Qi Xu2, Zhen-Chao Zhang2, Gen-Rong Liu2, Hao-Tong Zhang1, De-Hua Yang2, Shu-Yun Cao1, Hai-Yuan Chen2, Jian-Jun Chen1, Kun-Xin Chen2, Ying Chen1, Jia-Ru Chu3, Lei Feng1, Xue-Fei Gong2, Yong-Hui Hou2, Hong-Zhuan Hu3, Ning-Sheng Hu2, Zhong-Wen Hu2, Lei Jia1, Fang-Hua Jiang2, Xiang Jiang2, Zi-Bo Jiang2, Ge Jin3, Ai-Hua Li2, Yan Li4, Ye-Ping Li2, Guan-Qun Liu2, Zhi-Gang Liu3, Wen-Zhi Lu2, Yin-Dun Mao4, Li Men1, Yong-Jun Qi2, Zhao-Xiang Qi4, Huo-Ming Shi1, Zheng-Hong Tang4, Qing-Sheng Tao2, Da-Qi Wang1, Dan Wang1, Guo-Min Wang2, Hai Wang2, Jia-Ning Wang2, Jian Wang3, Jian-Ling Wang1, Jian-Ping Wang3, Lei Wang2, Shu-Qing Wang1, You Wang2, Yue-Fei Wang2, Ling-Zhe Xu2, Yan Xu1, Shi-Hai Yang2, Yong Yu4, Hui Yuan1, Xiang-Yan Yuan2, Chao Zhai3, Jing Zhang5, Yan-Xia Zhang1, Yong Zhang2, Ming Zhao4, Fang Zhou2, Guo-Hua Zhou2, Jie Zhu2 and Si-Cheng Zou1 1 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; 2 Nanjing Institute of Astronomical Optics and Technology, National Astronomical Observatories, Chinese Academy of Sciences, Nanjing 210042, China 3 University of Science and Technology of China, Hefei 230026, China 4 Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China 5 Institute of Architecture Design and Research, Chinese Academy of Sciences, Beijing 100190, China. Research in Astronomy and Astrophysics. 2012(09)
[3]LAMOST spectral survey——An overview[J]. Gang Zhao 1 , Yong-Heng Zhao 1 , Yao-Quan Chu 1 , 2 , Yi-Peng Jing 3 and Li-Cai Deng 1 1 Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China;2 University of Science and Technology of China, Hefei 230026, China 3 Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China. Research in Astronomy and Astrophysics. 2012(07)
本文编号：3460497
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