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AE Ursae Majoris - a delta Scuti star in the Hertzsprung Gap
Niu, Jia-Shu1,2,3,4; Fu, Jian-Ning1; Li, Yan5; Yang, Xiao-Hu1,6; Zong, Weikai1,7,8; Xue, Hui-Fang1; Zhang, Yan-Ping1; Liu, Nian1; Du, Bing6; Zuo, Fang6
2017-06-01
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume467Issue:3Pages:3122-3139
AbstractWe analyse the photometric data and spectroscopic data collected on the d Scuti star AE Ursae Majoris ( AE UMa). The fundamental and the first overtone frequencies are confirmed as f(0) = 11.625 60 c d(-1) and f(1) = 15.031 24 c d(-1), respectively, from the frequency content by analysing light curves over 40 nights, spanning from 2009 to 2012. Additionally, another 37 frequencies are identified as either the harmonics or the linear combinations of the fundamental and the first overtone frequencies, among which 25 are newly detected. The rate of period change of the fundamental mode is determined as (1/P-0)(dP(0)/dt) = 5.4(+/- 1.9) x 10(-9) yr(-1) as revealed from the O - C diagram based on the 84 newly determined times of maximum light combined with those derived from the literature. The spectroscopic data suggest that AEUMa is a Population I d Scuti star. With these physical properties, we perform theoretical explorations based on the stellar evolution codeMESA on this target, considering that the variation of pulsation period is caused by secular evolutionary effects. We finally constrain AE UMa with physical parameters as follows: mass of 1.805 +/- 0.055M(circle dot), radius of 1.647 +/- 0.032 x 10(11) cm, luminosity of 1.381 +/- 0.048(log L/L-circle dot) and age of 1.055 +/- 0.095 x 10(9) yr. AE UMa can be the (Population I) d Scuti star that locates just after the second turn-off of its evolutional track leaving the main sequence, a star in the phase of the Hertzsprung Gap with a helium core and a hydrogen-burning shell.
SubtypeArticle
KeywordTechniques: Photometric Techniques: Spectroscopic Stars: Individual: Ae Uma Stars: Oscillations Stars: Variables: Delta Scuti
WOS HeadingsScience & Technology ; Physical Sciences
Funding OrganizationJoint Fund of Astronomy of National Natural Science Foundation of China (NSFC) ; Joint Fund of Astronomy of National Natural Science Foundation of China (NSFC) ; Chinese Academy of Sciences(U1231202) ; Chinese Academy of Sciences(U1231202) ; NSFC(11673003) ; NSFC(11673003) ; National Basic Research Program of China (973 Program)(2014CB845700 ; National Basic Research Program of China (973 Program)(2014CB845700 ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; 2013CB834900) ; 2013CB834900) ; Joint Fund of Astronomy of National Natural Science Foundation of China (NSFC) ; Joint Fund of Astronomy of National Natural Science Foundation of China (NSFC) ; Chinese Academy of Sciences(U1231202) ; Chinese Academy of Sciences(U1231202) ; NSFC(11673003) ; NSFC(11673003) ; National Basic Research Program of China (973 Program)(2014CB845700 ; National Basic Research Program of China (973 Program)(2014CB845700 ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; 2013CB834900) ; 2013CB834900)
DOI10.1093/mnras/stx125
WOS KeywordSERIES ENSEMBLE PHOTOMETRY ; STELLAR ASTROPHYSICS MESA ; SX PHOENICIS STARS ; EQUATION-OF-STATE ; PERIOD CHANGES ; BL CAMELOPARDALIS ; MASS STARS ; PULSATION ; OPACITIES ; ASTEROSEISMOLOGY
Indexed BySCI
Language英语
Funding OrganizationJoint Fund of Astronomy of National Natural Science Foundation of China (NSFC) ; Joint Fund of Astronomy of National Natural Science Foundation of China (NSFC) ; Chinese Academy of Sciences(U1231202) ; Chinese Academy of Sciences(U1231202) ; NSFC(11673003) ; NSFC(11673003) ; National Basic Research Program of China (973 Program)(2014CB845700 ; National Basic Research Program of China (973 Program)(2014CB845700 ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; 2013CB834900) ; 2013CB834900) ; Joint Fund of Astronomy of National Natural Science Foundation of China (NSFC) ; Joint Fund of Astronomy of National Natural Science Foundation of China (NSFC) ; Chinese Academy of Sciences(U1231202) ; Chinese Academy of Sciences(U1231202) ; NSFC(11673003) ; NSFC(11673003) ; National Basic Research Program of China (973 Program)(2014CB845700 ; National Basic Research Program of China (973 Program)(2014CB845700 ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; 2013CB834900) ; 2013CB834900)
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000398419400048
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/8229
Collection光学天文研究部
Affiliation1.Beijing Normal Univ, Astron Dept, Beijing 100875, Peoples R China
2.Chinese Acad Sci, CAS Key Lab Theoret Phys, Beijing 100190, Peoples R China
3.Chinese Acad Sci, KITPC, Inst Theoret Phys, Beijing 100190, Peoples R China
4.Univ Chinese Acad Sci, Sch Phys Sci, 19A Yuquan Rd, Beijing 100049, Peoples R China
5.Chinese Acad Sci, Yunnan Observ, Natl Astron Observ, POB 110, Kunming 650011, Peoples R China
6.Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China
7.Univ Toulouse, IRAP, UPS OMP, F-31400 Toulouse, France
8.CNRS, IRAP, 14 Ave Edouard Belin, F-31400 Toulouse, France
Recommended Citation
GB/T 7714
Niu, Jia-Shu,Fu, Jian-Ning,Li, Yan,et al. AE Ursae Majoris - a delta Scuti star in the Hertzsprung Gap[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2017,467(3):3122-3139.
APA Niu, Jia-Shu.,Fu, Jian-Ning.,Li, Yan.,Yang, Xiao-Hu.,Zong, Weikai.,...&Zuo, Fang.(2017).AE Ursae Majoris - a delta Scuti star in the Hertzsprung Gap.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,467(3),3122-3139.
MLA Niu, Jia-Shu,et al."AE Ursae Majoris - a delta Scuti star in the Hertzsprung Gap".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 467.3(2017):3122-3139.
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