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Distinguishing Core and Shell Helium-burning Subdwarf B Stars by Asteroseismology
Guo JJ(郭军军)1,2,3
Source PublicationASTROPHYSICAL JOURNAL
2018-10-10
Volume866Issue:1Pages:9
DOI10.3847/1538-4357/aadd05
Contribution Rank第1完成单位
Indexed BySCI
Keywordmethods: numerical stars: oscillations subdwarfs
Abstract

Subdwarf B stars are generally considered to be core helium-burning stars. However, most canonical sdB models have shown that they leave the sdB band (i.e., the region with 20,000 K <= T-eff 40,000 K and 5 <= log g <= 6.2) after they have ignited helium in the shell. This means there will be a few shell helium-burning stars that have exhausted their helium in the core yet may still be located on the sdB band and should be considered as sdB stars too. But because they have effective temperature and gravity close to those of core helium-burning sdB stars, we cannot distinguish the two kinds of star just by atmospheric parameters. Some sdB stars display multimode pulsations. We thought that asteroseismology could offer some methods to distinguish the two kinds of sdB star. Core and shell helium-burning sdB stars have some obvious differences in structure and evolutionary track, which results in some clear differences in their pulsation properties. So, we may distinguish them by their pulsation properties such as the rates of change of period of the p-mode sdB pulsators, the numbers of mixed modes, and the period spacings of the g-mode sdB pulsators. We suggest that there are two special sdB stars (V391 Pegasi and PG 1605+072) that are likely shell helium-burning sdB stars.

Funding ProjectNSFC of China[11333006] ; NSFC of China[11521303] ; NSFC of China[11773064] ; NSFC of China[11503076] ; foundation of Chinese Academy of Sciences[XDB09010202] ; Yunnan Applied Basic Research Projects[2017B008]
Funding OrganizationNSFC of China[11333006, 11521303, 11773064, 11503076] ; foundation of Chinese Academy of Sciences[XDB09010202] ; Yunnan Applied Basic Research Projects[2017B008]
Language英语
Subject Area天文学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherIOP PUBLISHING LTD
Publication PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-637X
URL查看原文
WOS IDWOS:000447200800006
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordCOMPACT PULSATORS ; SDB STARS ; DRIVING MECHANISM ; GRAVITY MODES ; EVOLUTION ; OSCILLATIONS ; PARAMETERS ; ATMOSPHERE ; CAMPAIGN ; K2
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/18032
Collection恒星物理研究组
中国科学院天体结构与演化重点实验室
Corresponding AuthorGuo JJ(郭军军)
Affiliation1.Yunnan Observatories, Chinese Academy of Sciences, P.O. Box 110, Kunming 650011, People's Republic of China
2.Key Laboratory for Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, P.O. Box 110, Kunming 650011, People's Republic of China
3.University of Chinese Academy of Sciences, Beijing 100049, People's Republic of China
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Guo JJ. Distinguishing Core and Shell Helium-burning Subdwarf B Stars by Asteroseismology[J]. ASTROPHYSICAL JOURNAL,2018,866(1):9.
APA Guo JJ.(2018).Distinguishing Core and Shell Helium-burning Subdwarf B Stars by Asteroseismology.ASTROPHYSICAL JOURNAL,866(1),9.
MLA Guo JJ."Distinguishing Core and Shell Helium-burning Subdwarf B Stars by Asteroseismology".ASTROPHYSICAL JOURNAL 866.1(2018):9.
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