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 | |
刊名 | ASTROPHYSICAL JOURNAL |
2019-08-10 | |
卷号 | 881期号:1页码:15 |
关键词 | asteroseismology stars: fundamental parameters stars: individual (HD 50230) stars: interiors stars: oscillations (including pulsations) |
ISSN号 | 0004-637X |
DOI | 10.3847/1538-4357/ab2ad8 |
产权排序 | 第1完成单位 |
文献子类 | Article |
英文摘要 | 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. |
学科主题 | 天文学 ; 恒星与银河系 ; 恒星物理学 ; 恒星形成与演化 |
URL标识 | 查看原文 |
出版地 | TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND |
资助项目 | NSFC 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] |
WOS关键词 | ROTATION |
WOS研究方向 | Astronomy & Astrophysics |
语种 | 英语 |
出版者 | IOP PUBLISHING LTD |
WOS记录号 | WOS:000481848600015 |
资助机构 | NSFC of China[11333006, 11503076, 11503079, 11773064, 11873084, 11521303] ; Yunnan Applied Basic Research Projects[2017B008] |
内容类型 | 期刊论文 |
源URL | [http://ir.ynao.ac.cn/handle/114a53/20865] |
专题 | 云南天文台_恒星物理研究组 云南天文台_中国科学院天体结构与演化重点实验室 |
通讯作者 | Wu T(吴涛) |
作者单位 | 1.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 |
推荐引用方式 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. |
个性服务 |
查看访问统计 |
相关权益政策 |
暂无数据 |
收藏/分享 |
除非特别说明,本系统中所有内容都受版权保护,并保留所有权利。
修改评论