前身星与Ⅱ型超新星爆发的数值模拟

广西师范大学学报（自然科学版） ›› 2012, Vol. 30 ›› Issue (3): 71-76.

前身星与Ⅱ型超新星爆发的数值模拟

张妙静, 杨建辉, 潘江洪

广西师范大学物理科学与技术学院,广西桂林541004

收稿日期:2012-06-07 出版日期:2012-09-20 发布日期:2018-12-04
通讯作者: 张妙静(1974—),女,广西梧州人,广西师范大学教授。E-mail:zhangmiaojing@sina.com
作者简介:张妙静,女,1974年3月生,汉族,教授。
基金资助:
国家自然科学基金资助项目(11065004)

Presupernova and Numerical Simulation of Type Ⅱ Supernova Explosion

ZHANG Miao-jing, YANG Jian-hui, PAN Jiang-hong

College of Physics and technology,Guangxi Normal University,Guilin Guangxi 541004,China

Received:2012-06-07 Online:2012-09-20 Published:2018-12-04

摘要/Abstract

摘要： 利用考虑物质回落与混合效应的前身星输入数据,在一维球对称瞬时爆发模型下数值模拟了质量为12～15 M_⊙Ⅱ型超新星的星核坍缩、激波传播、爆发能量等过程。计算结果表明:前身星的星核质量、密度、温度、物质构成等对II型超新星爆发有重要影响,不过,数值模拟仍不能实现超新星的瞬时爆发。

关键词: 超新星, 物质回落, 前身星, 坍缩, 爆发

Abstract: ased on the input data of presupernova with fallbackand mixing of matter,a simulation of type Ⅱ supernova explosion process is made,which includes core collapse,shock propagation and explosion energy.The explosion is simulated in prompt mechanism by one dimension spheral symmetry model with presupernovae mass of 12 M_⊙ to 15 M_⊙.The results show that the core mass,density,temperature and composition affect the type Ⅱ supernova explosion significantly,but theprompt mechanism cannot get the expecting explosion.

Key words: supernova, fallback, presupernova, collapse, explosion

中图分类号:

P145.3

张妙静, 杨建辉, 潘江洪. 前身星与Ⅱ型超新星爆发的数值模拟[J]. 广西师范大学学报（自然科学版）, 2012, 30(3): 71-76.

ZHANG Miao-jing, YANG Jian-hui, PAN Jiang-hong. Presupernova and Numerical Simulation of Type Ⅱ Supernova Explosion[J]. Journal of Guangxi Normal University(Natural Science Edition), 2012, 30(3): 71-76.

参考文献

[1] 张妙静,张栩宁,潘江洪,等.物质吸积的外赋AGB星参数化模型[J].广西师范大学学报:自然科学版,2009,27(1):17-20.
[2] 张妙静,韦怀勇,潘江洪.质量损失对贫金属AGB星表面丰度的影响[J].广西师范大学学报:自然科学版,2008,26(3):17-20.
[3] ZHANG Miao-jing,QIU Xiu-qiang,PAN Jiang-hong.The influence of anew model of progenitor staron supernova explosion[J].Chinese Astronomy and Astrophysics,2009,33(4):384-392.
[4] WOOSLEY S E,HEGER A,WEAVER T A.The evolution and explosion ofmassive stars[J].Reviews of Mordern Physics,2002,74(4):1015-1071.
[5] HEGER A,WOOSLEY S E.Nucleosynthesis and evolution of massive metal-free stars[J].The Astrophysical Journal,2010,724(1):341-373.
[6] WOOSLEY S E,WEAVER T A.The evolution and explosion of massive stars.Ⅱ.explosive hydrodynamics and nucleosynthesis[J].The Astrophysical JournalSupplement Series,1995,101(11):181-235.
[7] CHEVALIER R A.Neutron star accretion in a supernova[J].AstrophysicalJournal,1989,346(1):847-859.
[8] ILIADIS C,D'AURIA J M,STARRFIELD S,et al.Proton-induced thermonuclear reaction rates for A=20-40 nuclei[J].The Astrophysical Journal Supplement Series,2001,134(1):151-171.
[9] HOFFMAN R D,WOOSLEY S E,WEAVER T A.Nucleosynthesis below A=100in massive stars[J].The Astrophysical Journal,2001,549(2):1085-1092.
[10] SPITE M,CAYREL R,PLEZ B,et al.First star Ⅵ-aburdances of C,N,O,Li and mixing in extremely metal-poor giants.galactic evolution of the light elements[J].Astronomy and Astrophysics,2005,430(2):655-668.
[11] 张妙静,丘秀强,潘江洪,等.新前身星模型对超新星爆发的影响[J].天文学报,2009,50(2):145.
[12] 王贻仁,张锁春,谢佐恒,等.超新星爆发机制和数值模拟[M].郑州:河南科学出版社,2003.

Metrics

Viewed

Full text

Abstract

Cited

Shared

Discussed