Laboratory Observation of C and O Emission Lines of the White Dwarf H1504+65-like Atmosphere Model

doi:10.3847/1538-4357/ac18c3

	Laboratory Observation of C and O Emission Lines of the White Dwarf H1504+65-like Atmosphere Model
	Ma, Bu-Bo 7; Ren, Jie-Ru 7; Wang, Shao-Yi 6; Hoffmann, Dieter H. H.7; Deng, Zhi-Gang 6; Qi, Wei 6; Wang, Xing 7; Yin, Shuai 7; Feng, Jian-Hua 7; Fan, Quan-Ping 6
刊名	ASTROPHYSICAL JOURNAL
	2021-10-01
卷号	920 期号:2 页码:9
关键词	White dwarf stars DQ stars
ISSN号	0004-637X
DOI	10.3847/1538-4357/ac18c3
通讯作者	Zhou, Wei-Min(zhouwm@caep.cn)
英文摘要	White dwarfs play important roles in stellar evolution and help us gauge the age of our galaxy. The white dwarf H1504+65, the hottest known post-asymptotic giant branch star, is peculiar due to its C- and O-rich but He- and H- deficient atmosphere whose composition cannot be well predicted by current stellar evolution models. The analysis of the elemental abundance and the benchmark of stellar atmospheric models depends heavily on spectral data under cosmic conditions, which are currently extremely scarce. We created a well-defined, uniform, relatively large-scale similar to millimeter plasma sample in the laboratory with a temperature and a C/O ratio similar to those of H1504+65's atmosphere. The emission spectra with high precision in the range of 10-80 nm were obtained and identified according to databases such as NIST and Kelly. A detailed comparison between our emission lines and the Chandra-observed white dwarf H1504+65 atmosphere's absorption lines was performed. The stongly isolated O VI lines in the range of 10-13 nm are observed in both cases. We observed a wealth of O V lines in the range of 13-14 nm that cannot be well identified or predicted by models due to the weak flux and also probably due to the blending effect of Fe group elements in the Chandra spectrum. Long-wavelength lines ranging from 14 to 80 nm, which are not observed in the Chandra spectrum because of the high interstellar neutral hydrogen column density, show abundant O IV-V, C IV lines, and strong O VI lines. Moreover, the intensities of the lines at 62.973 and 17.216 nm are analyzed to characterize the plasma temperature.
资助项目	National Key R&D Program of China[2019YFA0404900] ; Chinese Science Challenge Project[TZ2016005] ; National Natural Science Foundation of China[U2030104] ; National Natural Science Foundation of China[11775282] ; National Natural Science Foundation of China[11975174] ; China Postdoctoral Science Foundation[2017M623145] ; State Key Laboratory Foundation of Laser Interaction[SKLLIM1807] ; Fundamental Research Funds for the Central Universities
WOS关键词	STELLAR ; HYDROGEN ; SPECTRA ; OXYGEN ; STARS ; IONS
WOS研究方向	Astronomy & Astrophysics
语种	英语
出版者	IOP Publishing Ltd
WOS记录号	WOS:000709097700001
资助机构	National Key R&D Program of China ; Chinese Science Challenge Project ; National Natural Science Foundation of China ; China Postdoctoral Science Foundation ; State Key Laboratory Foundation of Laser Interaction ; Fundamental Research Funds for the Central Universities
内容类型	期刊论文
源URL	[http://119.78.100.186/handle/113462/136032]
专题	中国科学院近代物理研究所
通讯作者	Zhou, Wei-Min
作者单位	1.Shenzhen Univ Technol, Adv Mat Testing Technol Res Ctr, Shenzhen 518118, Peoples R China 2.Chinese Acad Sci, Inst Modern Phys, Lanzhou 730070, Peoples R China 3.China Acad Engn Phys, Grad Sch, Beijing 100088, Peoples R China 4.Inst Appl Phys & Computat Math, Beijing 100094, Peoples R China 5.Xian Technol Univ, Xian 710021, Peoples R China 6.China Acad Engn Phys, Laser Fus Res Ctr, Sci & Technol Plasma Phys Lab, Mianyang 621900, Sichuan, Peoples R China 7.Xi An Jiao Tong Univ, Sch Phys, MOE Key Lab Nonequilibrium Synth & Modulat Conden, Xian 710049, Peoples R China 8.Chinese Acad Sci, Inst Phys, Beijing Natl Lab Condensed Matter Phys, Beijing 100190, Peoples R China 9.Univ Chinese Acad Sci, Sch Phys Sci, Beijing 100049, Peoples R China 10.Xianyang Normal Univ, Xianyang 712000, Peoples R China
推荐引用方式 GB/T 7714	Ma, Bu-Bo,Ren, Jie-Ru,Wang, Shao-Yi,et al. Laboratory Observation of C and O Emission Lines of the White Dwarf H1504+65-like Atmosphere Model[J]. ASTROPHYSICAL JOURNAL,2021,920(2):9.
APA	Ma, Bu-Bo.,Ren, Jie-Ru.,Wang, Shao-Yi.,Hoffmann, Dieter H. H..,Deng, Zhi-Gang.,...&Zhao, Yong-Tao.(2021).Laboratory Observation of C and O Emission Lines of the White Dwarf H1504+65-like Atmosphere Model.ASTROPHYSICAL JOURNAL,920(2),9.
MLA	Ma, Bu-Bo,et al."Laboratory Observation of C and O Emission Lines of the White Dwarf H1504+65-like Atmosphere Model".ASTROPHYSICAL JOURNAL 920.2(2021):9.