论文标题
自一致的3D超新星型号从-7分钟到+7秒：1-甲虫的爆炸〜19太阳质量祖细胞
Self-consistent 3D Supernova Models From -7 Minutes to +7 Seconds: a 1-bethe Explosion of a ~19 Solar-mass Progenitor
论文作者
论文摘要
迄今为止，现代的三维（3D）超新星模拟尚未证明10^{51} erg的爆炸能量（= 1 bethe = 1b）或更多的可能用于非/慢螺旋的M <20 solar-Mass Mass Marar-Mass祖细胞中中微子驱动的SNE SNE SNE SNE。我们提出了第一个这样的模型，考虑到未旋转的太阳金属性18.88太阳能祖先，其最后7分钟的对流氧气壳燃烧在3D中模拟，并在崩溃之前显示出剧烈的氧气壳壳合并。使用Prometheus-Vertex代码计算了大量的3D SN模型，该代码改善了两臂方程与Boltzmann闭合的收敛性，现在可以完全利用隐式中微子转移治疗。用23个物种网络处理核燃烧。我们改变了角度的网格分辨率，并考虑了原始恒星（PNS）中的状态和隆隆形成的不同核方程，该恒星（PNS）需要六种物种运输，并在所有能量摩托群中偶联所有中微子口味。弹跳后施加精心的中微子运输直到约2秒。在一种情况下，模拟持续到7秒> 7秒，对中微子效应进行了近似处理，该效应允许无缝延续而无需瞬态。球形对称中微子驱动的风不会发展。取而代之的是，倾向下中微子加热物质的流体和流出的爆炸能量的单调升高，直到反弹后约7秒钟，当时即将爆发的冲击达到约50,000公里并进入He-layer。 Infinity爆炸能的融合值（减去量减少）约为1B，弹出的56NI质量高达0.087太阳能块，均在SN 1987a值的约10％之内。最终的NS质量和踢球约为1.65太阳能和超过450 km/s。
To date, modern three-dimensional (3D) supernova (SN) simulations have not demonstrated that explosion energies of 10^{51} erg (=1 bethe = 1B) or more are possible for neutrino-driven SNe of non/slow-rotating M < 20 solar-mass progenitors. We present the first such model, considering a non-rotating, solar-metallicity 18.88 solar-mass progenitor, whose final 7 minutes of convective oxygen-shell burning were simulated in 3D and showed a violent oxygen-neon shell merger prior to collapse. A large set of 3D SN-models was computed with the Prometheus-Vertex code, whose improved convergence of the two-moment equations with Boltzmann closure allows now to fully exploit the implicit neutrino-transport treatment. Nuclear burning is treated with a 23-species network. We vary the angular grid resolution and consider different nuclear equations of state and muon formation in the proto-neutron star (PNS), which requires six-species transport with coupling of all neutrino flavors across all energy-momentum groups. Elaborate neutrino transport was applied until ~2 seconds after bounce. In one case the simulation was continued to >7 seconds with an approximate treatment of neutrino effects that allows for seamless continuation without transients. A spherically symmetric neutrino-driven wind does not develop. Instead, accretion downflows to the PNS and outflows of neutrino-heated matter establish a monotonic rise of the explosion energy until ~7 seconds post bounce, when the outgoing shock reaches about 50,000 km and enters the He-layer. The converged value of the explosion energy at infinity (with overburden subtracted) is roughly 1B and the ejected 56Ni mass up to 0.087 solar masses, both within a few 10 percent of the SN 1987A values. The final NS mass and kick are about 1.65 solar masses and over 450 km/s, respectively.
