The Influence of the Metal Mass Fraction Z, Age, and Mixing-length Parameter on the RGB Bump Magnitude for the M4 Cluster
文献类型:期刊论文
作者 | Song, Fen1,2; Li Y(李焱)2,3,4,5; Wu T(吴涛)2,3,5; Pietrinferni, Adriano6; Poon, Helen7; Xie, Yi1 |
刊名 | ASTROPHYSICAL JOURNAL |
出版日期 | 2018-12-20 |
卷号 | 869期号:2页码:15 |
ISSN号 | 0004-637X |
关键词 | globular clusters: individual (NGC 6121) Hertzsprung-Russell and C-M diagrams stars: evolution stars: general stars: low-mass |
DOI | 10.3847/1538-4357/aaecd3 |
产权排序 | 第3完成单位 |
文献子类 | Article |
英文摘要 | We identify the location of the RGB bump of M4 (NGC 6121) using the available photometric data, and measure VRGBB (similar to 13.57 +/- 0.04 mag). According to the observed [Fe/H], we compute theoretical isochrones with the scaled-solar composition in the MESA model and alpha-enhanced composition in the BaSTI model, respectively. Using a color-magnitude diagram, we compare these isochrones with the observed data to obtain the magnitude difference delta V-bump between the predicted and the observed bump magnitude. Based on the best fit of the MESA model with [Fe/H] = -1.05, [alpha/Fe] =0, alpha(MLT) = 2.0, and t = 13.3 Gyr, the bump magnitude difference delta V-bump is about 0.46 mag. Based on the best fit of the BaSTI model with alpha(MLT) = 2.2 similar to 2.4, [Fe/H] = -1.05, [alpha/Fe] = 0.4, and t = 12.5 Gyr, the bump magnitude difference delta V-bump is about 0.2 mag. To try and explain the bump magnitude differences, the metal mass fraction Z is enhanced as 0.0037, 0.00591, 0.0076, and 0.0085. Accordingly, delta V-RGBB vertical bar(t=12.0,alpha MLT =2.2, [alpha/Fe] = 0,Z=0.0076), delta V-RGBB vertical bar(t=12.0,alpha MLT) (=2.2, [alpha/Fe]=0, Z=0.0085), and delta V-RGBB vertical bar(t=11.0,alpha MLT=2.4,[alpha/Fe]=0,Z=0.0085) by the MESA model are 0, -0.01, and 0 mag, respectively. Increasing the assumed metallicity can decrease the discrepancy between the predicted and observed bump magnitudes. However, a metallicity increase large enough to resolve the offset, roughly similar to 0.60 dex for the MESA models, is ruled out by the spectroscopic data. |
学科主题 | 天文学 ; 恒星与银河系 |
URL标识 | 查看原文 |
出版地 | TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND |
WOS关键词 | GALACTIC GLOBULAR-CLUSTERS ; GIANT ; METALLICITY ; LUMINOSITY ; ABUNDANCES ; PHOTOMETRY ; EVOLUTION ; SEQUENCE |
资助项目 | NSFC of China[11333006] ; NSFC of China[11521303] ; NSFC of China[11373020] ; NSFC of China[11503079] ; NSFC of China[11603009] ; NSFC of China[11503076] ; NSFC of China[11773064] ; NSFC of China[11803009] ; foundation of Chinese Academy of Sciences[XDB09010202] ; Natural Science Foundation of Fujian Province[2016J05013] ; Natural Science Foundation of Fujian Province[2018J05006] ; Natural Science Foundation of Fujian Province[2018J05007] ; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences[OP201404] ; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences[201504150001] ; Yunnan Applied Basic Research Projects[2017B008] ; Scientific Research Foundation of Jimei University[ZQ2013013] |
WOS研究方向 | Astronomy & Astrophysics |
语种 | 英语 |
出版者 | IOP PUBLISHING LTD |
WOS记录号 | WOS:000453609600007 |
资助机构 | NSFC of China[11333006, 11521303, 11373020, 11503079, 11603009, 11503076, 11773064, 11803009] ; foundation of Chinese Academy of Sciences[XDB09010202] ; Natural Science Foundation of Fujian Province[2016J05013, 2018J05006, 2018J05007] ; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences[OP201404, 201504150001] ; Yunnan Applied Basic Research Projects[2017B008] ; Scientific Research Foundation of Jimei University[ZQ2013013] |
源URL | [http://ir.ynao.ac.cn/handle/114a53/18602] |
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 | Song, Fen |
作者单位 | 1.College of Science, Jimei University, Xiamen 361021, 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.Yunnan Observatories, Chinese Academy of Sciences, P.O. Box 110, Kunming 650011, People's Republic of China 4.University of Chinese Academy of Sciences, Beijing 100049, People's Republic of China 5.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, People's Republic of China 6.INAF-Osservatorio Astronomico d'Abruzzo, via M. Maggini, I-64100 Teramo, Italy 7.Department of Physical Science, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 7398526, Japan |
推荐引用方式 GB/T 7714 | Song, Fen,Li Y,Wu T,et al. The Influence of the Metal Mass Fraction Z, Age, and Mixing-length Parameter on the RGB Bump Magnitude for the M4 Cluster[J]. ASTROPHYSICAL JOURNAL,2018,869(2):15. |
APA | Song, Fen,Li Y,Wu T,Pietrinferni, Adriano,Poon, Helen,&Xie, Yi.(2018).The Influence of the Metal Mass Fraction Z, Age, and Mixing-length Parameter on the RGB Bump Magnitude for the M4 Cluster.ASTROPHYSICAL JOURNAL,869(2),15. |
MLA | Song, Fen,et al."The Influence of the Metal Mass Fraction Z, Age, and Mixing-length Parameter on the RGB Bump Magnitude for the M4 Cluster".ASTROPHYSICAL JOURNAL 869.2(2018):15. |
入库方式: OAI收割
来源:云南天文台
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