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The Influence of the Metal Mass Fraction Z, Age, and Mixing-length Parameter on the RGB Bump Magnitude for the M4 Cluster
Song, Fen1,2; Li Y(李焱)2,3,4,5; Wu T(吴涛)2,3,5; Pietrinferni, Adriano6; Poon, Helen7; Xie, Yi1
发表期刊ASTROPHYSICAL JOURNAL
2018-12-20
卷号869期号:2页码:15
DOI10.3847/1538-4357/aaecd3
产权排序第3完成单位
收录类别SCI
关键词globular clusters: individual (NGC 6121) Hertzsprung-Russell and C-M diagrams stars: evolution stars: general stars: low-mass
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.

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]
项目资助者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]
语种英语
学科领域天文学 ; 恒星与银河系
学科门类理学 ; 理学::天文学
文章类型Article
出版者IOP PUBLISHING LTD
出版地TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-637X
URL查看原文
WOS记录号WOS:000453609600007
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]GALACTIC GLOBULAR-CLUSTERS ; GIANT ; METALLICITY ; LUMINOSITY ; ABUNDANCES ; PHOTOMETRY ; EVOLUTION ; SEQUENCE
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/18603
专题恒星物理研究组
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
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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.
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