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High-precision Asteroseismology in a Slowly Pulsating B Star: HD 50230
Wu T(吴涛)1,2,3; Li Y(李焱)1,2,3,4
Source PublicationASTROPHYSICAL JOURNAL
2019-08-10
Volume881Issue:1Pages:15
DOI10.3847/1538-4357/ab2ad8
Contribution Rank第1完成单位
Indexed BySCI
Keywordasteroseismology stars: fundamental parameters stars: individual (HD 50230) stars: interiors stars: oscillations (including pulsations)
Abstract

The slowly pulsating B star HD 50230, which is in fact a hybrid B-type pulsator, has been observed by CoRoT for at least 137 days. Nearly equidistant period spacing patterns are found among eight modes that are extracted from the oscillation spectrum with more than 500 frequencies. However, it is thought to be most likely accidental by Szewczuk et al. In the present work, we analyze the eight modes in depth with the chi(2)-matching method. Based on the best-fitting model (model MA), we find that they can be well explained as sequences of consecutive dipolar (l, m) = (1, 0). The period discrepancies between observations and the best-fitting model are within 100 s except for the outlier, which is up to 300 s. Based on the calculated chi(2)-minimization models, we find that, for pure g-mode oscillations, the buoyancy radius, Lambda(0), can be precisely measured with the chi(2)-matching method between observations and calculations. It represents the "propagation time" of the g-mode from the stellar surface to the center. It is of Lambda(0) = 245.78 +/- 0.59 mu Hz with a precision of 0.24%. In addition, we also find that HD 50230 is a metal-rich (Z(init) = 0.034-0.043) star with a mass of M = 6.15-6.27 M-circle dot. It is still located in the hydrogen-burning phase with central hydrogen of X-C = 0.298-0.316 (or = X-C = 0.306(-0.008)(+0.010)); therefore, it has a convective core with a radius of R-cc = 0.525-0.536 R-circle dot (or R-cc = 0.531(-0.006)(+0.005) R-circle dot). In order to interpret the structure of the observed period spacing pattern well, the convective core overshooting (f(ov) = 0.0175-0.0200) and the extra diffusion mixing (log D-mix = 3.7-3.9) should be taken into account in theoretical models.

Funding ProjectNSFC of China[11333006] ; NSFC of China[11503076] ; NSFC of China[11503079] ; NSFC of China[11773064] ; NSFC of China[11873084] ; NSFC of China[11521303] ; Yunnan Applied Basic Research Projects[2017B008]
Funding OrganizationNSFC of China[11333006, 11503076, 11503079, 11773064, 11873084, 11521303] ; Yunnan Applied Basic Research Projects[2017B008]
Language英语
Subject Area天文学 ; 恒星与银河系 ; 恒星物理学 ; 恒星形成与演化
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:000481848600015
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordROTATION
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/20866
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 AuthorWu T(吴涛)
Affiliation1.Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, People's Republic of China
2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, People's Republic of China
3.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, People's Republic of China
4.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
Wu T,Li Y. High-precision Asteroseismology in a Slowly Pulsating B Star: HD 50230[J]. ASTROPHYSICAL JOURNAL,2019,881(1):15.
APA Wu T,&Li Y.(2019).High-precision Asteroseismology in a Slowly Pulsating B Star: HD 50230.ASTROPHYSICAL JOURNAL,881(1),15.
MLA Wu T,et al."High-precision Asteroseismology in a Slowly Pulsating B Star: HD 50230".ASTROPHYSICAL JOURNAL 881.1(2019):15.
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