Distinguishing Core and Shell Helium-burning Subdwarf B Stars by Asteroseismology
文献类型：期刊论文
| 作者 | Guo JJ(郭军军)1,2,3
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| 刊名 | ASTROPHYSICAL JOURNAL
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| 出版日期 | 2018-10-10 |
| 卷号 | 866期号:1页码:9 |
| 关键词 | methods: numerical stars: oscillations subdwarfs |
| ISSN号 | 0004-637X |
| DOI | 10.3847/1538-4357/aadd05 |
| 产权排序 | 第1完成单位 |
| 通讯作者 | Guo, Jun-Jun(guojunjun@ynao.ac.cn) |
| 文献子类 | Article |
| 英文摘要 | 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. |
| 学科主题 | 天文学 |
| URL标识 | 查看原文 |
| WOS关键词 | COMPACT PULSATORS ; SDB STARS ; DRIVING MECHANISM ; GRAVITY MODES ; EVOLUTION ; OSCILLATIONS ; PARAMETERS ; ATMOSPHERE ; CAMPAIGN ; K2 |
| 资助项目 | NSFC 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] |
| WOS研究方向 | Astronomy & Astrophysics |
| 语种 | 英语 |
| WOS记录号 | WOS:000447200800006 |
| 出版者 | IOP PUBLISHING LTD |
| 资助机构 | NSFC of China ; foundation of Chinese Academy of Sciences ; Yunnan Applied Basic Research Projects |
| 源URL | [http://ir.ynao.ac.cn/handle/114a53/18031]  |
| 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 | Guo JJ(郭军军) |
| 作者单位 | 1.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 |
| 推荐引用方式 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. |
入库方式： OAI收割
来源：云南天文台
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