A New Model for Electron-capture Supernovae in Galactic Chemical Evolution

被引:18
作者
Jones, Samuel [1 ,2 ]
Cote, Benoit [3 ,4 ,5 ]
Ropke, Friedrich K. [6 ,7 ]
Wanajo, Shinya [8 ,9 ,10 ]
机构
[1] Los Alamos Natl Lab, X Computat Phys XCP Div, Los Alamos, NM 87545 USA
[2] Los Alamos Natl Lab, CTA, Los Alamos, NM 87545 USA
[3] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary
[4] Michigan State Univ, Natl Superconducting Cyclotron Lab, E Lansing, MI 48824 USA
[5] Ctr Evolut Elements, Joint Inst Nucl Astrophys, E Lansing, MI USA
[6] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, Philosophenweg 12, D-69120 Heidelberg, Germany
[7] Heidelberg Inst Theoret Studies, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany
[8] Albert Einstein Inst, Max Planck Inst Gravitat Phys, Muhlenberg 1, D-14476 Potsdam, Germany
[9] Sophia Univ, Dept Engn & Appl Sci, Chiyoda Ku, Tokyo 1028554, Japan
[10] RIKEN, iTHEMS Res Grp, Wako, Saitama 3510198, Japan
基金
美国国家科学基金会; 欧洲研究理事会;
关键词
nuclear reactions; nucleosynthesis; abundances; stars: evolution; Sun: abundances; supernovae: general; CHANDRASEKHAR-MASS MODELS; 8-10; M; STARS; NUCLEOSYNTHESIS; COLLAPSE; PROGENITORS; ENRICHMENT; RATES;
D O I
10.3847/1538-4357/ab384e
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We examine the contribution of electron-capture supernovae (ECSNe), low-mass SNe from collapsing Fe cores (FeCCSNe), and rotating massive stars to the chemical composition of the Galaxy. Our model includes contributions to chemical evolution from both thermonuclear ECSNe (tECSNe) and gravitational collapse ECSNe (cECSNe). We show that if ECSNe are predominantly gravitational collapse SNe but about 15% are partial thermonuclear explosions, the model is able to reproduce the solar abundances of several important and problematic isotopes including Ca-48, Ti-50, and Cr-54 together with Fe-58, Ni-64, Se-82, and Kr-86 and several of the Zn- Zr isotopes. A model in which no cECSNe occur, only tECSNe with low-mass FeCCSNe or rotating massive stars, proves also very successful at reproducing the solar abundances for these isotopes. Despite the small mass range for the progenitors of ECSNe and low-mass FeCCSNe, the large production factors suffice for the solar inventory of the above isotopes. Our model is compelling because it introduces no new tensions with the solar abundance distribution for a Milky Way model-only tending to improve the model predictions for several isotopes. The proposed astrophysical production model thus provides a natural and elegant way to explain one of the last uncharted territories on the periodic table of astrophysical element production.
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页数:8
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