对m56变星及其彩色星等图结构的新观测

IF 1.1 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Revista Mexicana de Astronomia y Astrofisica Pub Date : 2022-02-18 DOI:10.22201/ia.01851101p.2022.58.01.10

D. Deras, A. Ferro, I. B. Fierro, M. A. Yepez

{"title":"对m56变星及其彩色星等图结构的新观测","authors":"D. Deras, A. Ferro, I. B. Fierro, M. A. Yepez","doi":"10.22201/ia.01851101p.2022.58.01.10","DOIUrl":null,"url":null,"abstract":"We present a VI CCD photometric study and a membership analysis of the globular cluster M56 (NGC 6779). This produced a CMD decontaminated from field stars, which enabled a better confrontation with theoretical isochrones, zero-age horizontal branches (ZAHB) and post-ZAHB evolutionary tracks. Post He-flash evolutionary models with a He-core mass of 0.5 Mʘ and envelopes of 0.04 - 0.18 Mʘ, cover the complete horizontal branch. Models with total mass ≈ 0.68 Mʘ explain the RR Lyrae, while those with a mass ≈ 0.56 Mʘ and a very subtle envelope, explain the Pop II cepheids with a progenitor in the blue tail of the HB. Based on the Fourier decomposition of the V light curve of a single cluster member RRc star, we determined a metallicity of [Fe/H]ZW = −1.96 ± 0.09. Several independent distance determination approaches lead to a mean distance to M56 of ⟨d⟩ = 9.4 ± 0.4 kpc. Finally, we report 5 new variables: one SX Phe, three EB, and one Rrc.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.1000,"publicationDate":"2022-02-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"1","resultStr":"{\"title\":\"A NEW VISIT TO THE VARIABLE STARS IN M56 AND ITS COLOUR-MAGNITUDE DIAGRAM STRUCTURE\",\"authors\":\"D. Deras, A. Ferro, I. B. Fierro, M. A. Yepez\",\"doi\":\"10.22201/ia.01851101p.2022.58.01.10\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"We present a VI CCD photometric study and a membership analysis of the globular cluster M56 (NGC 6779). This produced a CMD decontaminated from field stars, which enabled a better confrontation with theoretical isochrones, zero-age horizontal branches (ZAHB) and post-ZAHB evolutionary tracks. Post He-flash evolutionary models with a He-core mass of 0.5 Mʘ and envelopes of 0.04 - 0.18 Mʘ, cover the complete horizontal branch. Models with total mass ≈ 0.68 Mʘ explain the RR Lyrae, while those with a mass ≈ 0.56 Mʘ and a very subtle envelope, explain the Pop II cepheids with a progenitor in the blue tail of the HB. Based on the Fourier decomposition of the V light curve of a single cluster member RRc star, we determined a metallicity of [Fe/H]ZW = −1.96 ± 0.09. Several independent distance determination approaches lead to a mean distance to M56 of ⟨d⟩ = 9.4 ± 0.4 kpc. Finally, we report 5 new variables: one SX Phe, three EB, and one Rrc.\",\"PeriodicalId\":49602,\"journal\":{\"name\":\"Revista Mexicana de Astronomia y Astrofisica\",\"volume\":\" \",\"pages\":\"\"},\"PeriodicalIF\":1.1000,\"publicationDate\":\"2022-02-18\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"1\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Revista Mexicana de Astronomia y Astrofisica\",\"FirstCategoryId\":\"101\",\"ListUrlMain\":\"https://doi.org/10.22201/ia.01851101p.2022.58.01.10\",\"RegionNum\":4,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q3\",\"JCRName\":\"ASTRONOMY & ASTROPHYSICS\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Revista Mexicana de Astronomia y Astrofisica","FirstCategoryId":"101","ListUrlMain":"https://doi.org/10.22201/ia.01851101p.2022.58.01.10","RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q3","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}

引用次数: 1

摘要

我们提出了球状星团M56 (ngc6779)的VI CCD光度研究和成员分析。这产生了一个不受外场恒星污染的CMD，从而能够更好地与理论等时线、零年龄水平分支(ZAHB)和后ZAHB进化轨迹进行对抗。后he闪演化模型的he核质量为0.5 M突，包壳质量为0.04 ~ 0.18 M突，覆盖了整个水平分支。总质量≈0.68 M突的模型解释了RR天琴座，而那些质量≈0.56 M突和非常微妙的包膜的模型解释了Pop II造父变星，其祖先位于HB的蓝色尾部。根据单个星团成员RRc星的V光曲线的傅里叶分解，我们确定了[Fe/H]的金属丰度ZW =−1.96±0.09。几个独立的距离确定方法导致⟨d⟩到M56的平均距离= 9.4±0.4 kpc。最后，我们报告了5个新的变量:一个SX Phe，三个EB和一个Rrc。

本文章由计算机程序翻译，如有差异，请以英文原文为准。

查看原文本刊更多论文

A NEW VISIT TO THE VARIABLE STARS IN M56 AND ITS COLOUR-MAGNITUDE DIAGRAM STRUCTURE

We present a VI CCD photometric study and a membership analysis of the globular cluster M56 (NGC 6779). This produced a CMD decontaminated from field stars, which enabled a better confrontation with theoretical isochrones, zero-age horizontal branches (ZAHB) and post-ZAHB evolutionary tracks. Post He-flash evolutionary models with a He-core mass of 0.5 Mʘ and envelopes of 0.04 - 0.18 Mʘ, cover the complete horizontal branch. Models with total mass ≈ 0.68 Mʘ explain the RR Lyrae, while those with a mass ≈ 0.56 Mʘ and a very subtle envelope, explain the Pop II cepheids with a progenitor in the blue tail of the HB. Based on the Fourier decomposition of the V light curve of a single cluster member RRc star, we determined a metallicity of [Fe/H]ZW = −1.96 ± 0.09. Several independent distance determination approaches lead to a mean distance to M56 of ⟨d⟩ = 9.4 ± 0.4 kpc. Finally, we report 5 new variables: one SX Phe, three EB, and one Rrc.

求助全文

通过发布文献求助，成功后即可免费获取论文全文。去求助

来源期刊

Revista Mexicana de Astronomia y Astrofisica 地学天文-天文与天体物理

CiteScore

1.30

自引率

10.00%

发文量

审稿时长

>12 weeks

期刊介绍： The Revista Mexicana de Astronomía y Astrofísica, founded in 1974, publishes original research papers in all branches of astronomy, astrophysics and closely related fields. Two numbers per year are issued and are distributed free of charge to all institutions engaged in the fields covered by the RMxAA.