The influence of metallicity on helium and CO core masses in massive stars

IF 0.8 4区 物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS Serbian Astronomical Journal Pub Date : 2023-01-01 DOI:10.2298/saj2306001p
Jelena Petrović
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Abstract

We present the results of 58 detailed evolutionary models of massive single stars and close binary systems with the Solar and Small Magellanic Cloud (SMC) metallicity computed with the MESA (Modules for Experiments in Stellar Astrophysics) numerical code. Helium core masses of single stars (30 M? - 75 M?) with metallicities of 0.02 and 0.0021 are in the range of 9.26 M? - 29.56 M? and 11.62 M? - 33.96 M?, respectively. Their carbon-oxygen (CO) core masses are between 5.44 M? and 25.04 M? vs. 8.23 M? and 28.38 M? for the Solar vs. SMC metallicity, accounting for an average difference of 25%. To investigate the influence of metallicity on helium and carbon-oxygen core masses in massive close Case A binary systems, detailed evolutionary models of binary systems in the mass range of 30 M? to 40 M? are calculated. The initial orbital period is set to 3 days and the accretion efficiency to 10%. The helium core mass range for primary stars with lower metallicity is 10.61 - 16.21 M? vs. 7.94 - 11.69 M? for z = 0.02. The resulting CO core masses of primary stars for the SMC metallicity are on average about 50% larger than for the Solar metallicity, so the effect is more prominent than in the case of single stars. The black hole formation limit for primary stars with the SMC metallicity is under 30 M?. While the least massive primary stars with Solar metallicity end up as neutron stars, all primary stars with the SMC metallicity and all secondary stars complete their evolution as black holes. The double compact objects resulting from the presented models are of two types: mixed neutron star-black hole systems (4 models) and double black holes (18 models). We also derive the relation between the final helium core mass and the carbon-oxygen core mass and show that it does not depend on metallicity. We confirm the CO/helium core mass ratio to be larger in binary systems than for single stars.
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金属丰度对大质量恒星中氦和CO核心质量的影响
用MESA (Modules for Experiments in Stellar Astrophysics)数值代码计算了58个具有太阳和小麦哲伦云(SMC)金属丰度的大质量单星和紧密双星系统的详细演化模型的结果。单星氦核质量(30m ?金属丰度为0.02和0.0021的金属在9.26 M?- 29.56米?11点62分?- 33.96米?,分别。它们的碳氧(CO)核心质量在5.44 M?25分04秒?vs. 8.23 M?28.38 M?对于Solar与SMC的金属丰度,占比平均相差25%。为了研究金属丰度对大质量紧密的Case A双星系统中氦和碳氧核心质量的影响,详细建立了质量范围为30 M?到40米?计算。初始轨道周期设置为3天,吸积效率设置为10%。金属丰度较低的主星的氦核质量范围为10.61 ~ 16.21 M?vs. 7.94 - 11.69 ?对于z = 0.02。SMC金属丰度的主恒星的CO核心质量比太阳金属丰度的主恒星的CO核心质量平均大50%左右,因此这种效应比单星的情况更为突出。具有SMC金属丰度的主星的黑洞形成极限在30 μ M以下。而质量最小的具有太阳金属丰度的主星最终成为中子星,所有具有SMC金属丰度的主星和所有的副星都完成了黑洞的演化。由这些模型得到的双致密天体有两种类型:混合中子星-黑洞系统(4个模型)和双黑洞(18个模型)。我们还推导了最终氦核质量与碳氧核质量之间的关系,并表明它不依赖于金属丰度。我们确认双星系统的CO/氦核心质量比大于单星。
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来源期刊
Serbian Astronomical Journal
Serbian Astronomical Journal ASTRONOMY & ASTROPHYSICS-
CiteScore
1.00
自引率
0.00%
发文量
6
审稿时长
12 weeks
期刊介绍: Serbian Astronomical Journal publishes original observations and researches in all branches of astronomy. The journal publishes: Invited Reviews - review article on some up-to-date topic in astronomy, astrophysics and related fields (written upon invitation only), Original Scientific Papers - article in which are presented previously unpublished author''s own scientific results, Preliminary Reports - original scientific paper, but shorter in length and of preliminary nature, Professional Papers - articles offering experience useful for the improvement of professional practice i.e. article describing methods and techniques, software, presenting observational data, etc. In some cases the journal may publish other contributions, such as In Memoriam notes, Obituaries, Book Reviews, as well as Editorials, Addenda, Errata, Corrigenda, Retraction notes, etc.
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