The infancy of core-collapse supernova remnants
The infancy of core-collapse supernova remnants
复制标题
核心塌陷超新星遗迹的初期
DOI：
10.1093/mnras/stab116
复制
发表时间：
2020
影响因子：
4.8
通讯作者：
H. Janka
中科院分区：
文献类型：
--
作者：
M. Gabler;A. Wongwathanarat;H. Janka
我们提出了三维流体动力学模拟中微子驱动的超新星（SNe）与PROMETHEUS-HOTB代码，从冲击爆发，直到他们达到同源膨胀阶段后，大约一年的不对称膨胀喷出物。我们的计算延续了Wongwathanarat等人对两颗红超巨星（RSG）和两颗蓝超巨星（BSG）祖星的模拟，他研究了在爆炸的第一秒期间由流体动力学不稳定性产生的爆炸不对称性的增长以及随后由瑞利-泰勒不稳定性产生的碎片化。我们重点研究了由$^{56}$Ni到$^{56}$Fe的放射性衰变引起的加热以及由来自He/H壳层界面的反向激波压缩喷出物中心部分时形成的新的向外移动的激波引起的喷出物的后期加速和膨胀。富铁喷射物的平均速度在100 km/s和350 km/s之间增加，最快的百分之一的铁加速到1000 km/s。从1D模型中已知的这种“镍气泡效应”加速了我们3D模型中的镍块，并导致最初过密的富镍团块膨胀，这导致密度不足，延伸的手指，被压缩周围物质的过密皮肤包裹。我们还提供了体积和表面填充因子，以及一个球谐函数分析，以表征光谱的镍块大小定量。我们的四个模型中有三个给出的体积填充因子大于0.3，与观察对SN 1987 A的建议一致。
We present 3D hydrodynamic simulations of neutrino-driven supernovae (SNe) with the PROMETHEUS-HOTB code, evolving the asymmetrically expanding ejecta from shock breakout until they reach the homologous expansion phase after roughly one year. Our calculations continue the simulations for two red supergiant (RSG) and two blue supergiant (BSG) progenitors by Wongwathanarat et al., who investigated the growth of explosion asymmetries produced by hydrodynamic instabilities during the first second of the explosion and their later fragmentation by Rayleigh-Taylor instabilities. We focus on the late time acceleration and inflation of the ejecta caused by the heating due to the radioactive decay of $^{56}$Ni to $^{56}$Fe and by a new outward-moving shock, which forms when the reverse shock from the He/H-shell interface compresses the central part of the ejecta. The mean velocities of the iron-rich ejecta increase between 100 km/s and 350 km/s ($\sim$8-30\%), and the fastest one percent of the iron accelerates by up to $\sim$1000 km/s ($\sim$20-25\%). This 'Ni-bubble effect', known from 1D models, accelerates the bulk of the nickel in our 3D models and causes an inflation of the initially overdense Ni-rich clumps, which leads to underdense, extended fingers, enveloped by overdense skins of compressed surrounding matter. We also provide volume and surface filling factors as well as a spherical harmonics analysis to characterize the spectrum of Ni-clump sizes quantitatively. Three of our four models give volume filling factors larger than 0.3, consistent with what is suggested for SN 1987A by observations.
登录
查看更多内容
DOI：
10.3847/1538-4357/ab4b46
发表时间：
2019-10
期刊：
The Astrophysical Journal
影响因子：
--
作者：
P. Cigan;M. Matsuura;H. Gomez;R. Indebetouw;F. Abellán;M. Gabler;A. Richards;D. Alp;T. Davis;H. Janka;J. Spyromilio;M. Barlow;D. Burrows;E. Dwek;C. Fransson;B. Gaensler;J. Larsson;P. Bouchet;P. Lundqvist;J. Marcaide;C. Ng;Sangwook Park;P. Roche;J. V. van Loon;J. Wheeler;G. Zanardo
通讯作者：
P. Cigan;M. Matsuura;H. Gomez;R. Indebetouw;F. Abellán;M. Gabler;A. Richards;D. Alp;T. Davis;H. Janka;J. Spyromilio;M. Barlow;D. Burrows;E. Dwek;C. Fransson;B. Gaensler;J. Larsson;P. Bouchet;P. Lundqvist;J. Marcaide;C. Ng;Sangwook Park;P. Roche;J. V. van Loon;J. Wheeler;G. Zanardo
DOI：
10.3847/1538-4357/ab4ff2
发表时间：
2019-10
期刊：
The Astrophysical Journal
影响因子：
--
作者：
J. Larsson;C. Fransson;D. Alp;P. Challis;R. Chevalier;R. Kirshner;R. Kirshner;Stephen S. Lawrence;B. Leibundgut;P. Lundqvist;S. Mattila;K. Migotto;J. Sollerman;G. Sonneborn;J. Spyromilio;N. Suntzeff;J. Wheeler
通讯作者：
J. Larsson;C. Fransson;D. Alp;P. Challis;R. Chevalier;R. Kirshner;R. Kirshner;Stephen S. Lawrence;B. Leibundgut;P. Lundqvist;S. Mattila;K. Migotto;J. Sollerman;G. Sonneborn;J. Spyromilio;N. Suntzeff;J. Wheeler
9、10、11、12 和 13 M 星的三维超新星爆炸模拟
影响因子：
4.8
作者：
Burrows, Adam;Radice, David;Vartanyan, David
通讯作者：
Vartanyan, David
影响因子：
4.8
作者：
D. Vartanyan;A. Burrows;D. Radice;A. Skinner;J. Dolence
通讯作者：
D. Vartanyan;A. Burrows;D. Radice;A. Skinner;J. Dolence
SN 1987A 核心喷射物的深处：以 3D 形式看到的分子结构
DOI：
10.3847/2041-8213/aa784c
发表时间：
2017
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Abellán F
通讯作者：
Abellán F