Impact of the new ^(12)C+^(12)C reaction rate on presupernova nucleosynthesis  

作　　者：辛文宇 野本憲一 赵刚 吴文博 Wenyu Xin;Ken'ichi Nomoto;Gang Zhao;Wenbo Wu(CAS Key Laboratory of Optical Astronomy,National Astronomical Observatories,Chinese Academy of Sciences,Bejing 10o101,China;School of Astronomy and Space Science,University of Chinese Academy of Sciences,Beijing 100049,China;Kavli Institute for the Physics and Mathematics of the Universe(WPI),The University of Tokyo Institutes for Advanced Study,The University of Tokyo,Kashiwa,Chiba277-8583,Japan)

机构地区：[1]CAS Key Laboratory of Optical Astronomy,National Astronomical Observatories,Chinese Academy of Sciences,Bejing 10o101,China [2]School of Astronomy and Space Science,University of Chinese Academy of Sciences,Beijing 100049,China [3]Kavli Institute for the Physics and Mathematics of the Universe(WPI),The University of Tokyo Institutes for Advanced Study,The University of Tokyo,Kashiwa,Chiba277-8583,Japan

出　　处：《Chinese Physics C》2023年第3期206-217,共12页中国物理C（英文版）

基　　金：Supported by the National Natural Science Foundation of China(11988101,11890694);the National Key R&D Program of China(2019YFA0405502);K.Nomoto is supported by the World Premier International Research Center Initiative(WPI),MEXT,Japan,and the Japan Society for the Promotion of Science(JSPS)KAKENHIgrant(JP17K05382,JP20K04024,JP21H04499)。

摘　　要：The ^(12)C+^(12)C reaction rate plays an essential role in stellar evolution and nucleosynthesis.Nevertheless,the uncertainties of this reaction rate are still large.We calculate a series of stellar evolution models with the near solar abundance from the zero-age main-sequence through presupernova stages for initial masses of 20 M_(⊙) to 40 M_(⊙).The ^(12)C+^(12)C reaction rates from two different studies are used in our investigation.One is the rate obtained using the Trojan Horse Method(THM)by Tumino et al.[Nature 557(7707),687(2018)],and the other was obtained by Mukhamedzhanov et al.[Physical Review C 99(6),064618(2019)](Muk19).Then,comparisons of the nucleosynthesis and presupernova isotopic abundances are conducted.In particular,we find that in the C burning shell,models with the THM produce a smaller amount of ^(23)Na and some neutron-rich isotopes than Muk19.The difference in the abundance ratios of Na/Mg,S/Mg,Ar/Mg,and K/Mg between the two models are apparent.We compare Na/Mg obtained from our theoretical presupernovae models with Na/Mg in stellar atmospheres observed with high-resolution spectra as well as from the latest galactic chemical evolution model.Although Na/Mg obtained using the THM is within 2σ of the observed stellar ratio,the theoretical uncertainty on Na/Mg introduced by the uncertainty of the ^(12)C+^(12)C reaction rate is almost equivalent to the standard deviation of astronomical observations.Therefore,a more accurate ^(12)C+^(12)C reaction rate is crucial.

关 键 词：reaction rate presupernova NUCLEOSYNTHESIS massive stars 

分 类 号：P145.3[天文地球—天体物理]