Revisiting Impacts of Nuclear Burning for Reviving Weak Shocks in Neutrino-driven Supernovae
Revisiting Impacts of Nuclear Burning for Reviving Weak Shocks in Neutrino-driven Supernovae
复制标题
重新审视核燃烧对中微子驱动的超新星中微弱冲击的影响
DOI：
10.1088/0004-637x/782/2/91
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发表时间：
2014
期刊：
影响因子：
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通讯作者：
N. Nishimura
中科院分区：
文献类型：
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作者：
Nakamura;K.; Takiwaki;T;Kotake;K.;N. Nishimura
我们重新审视核燃烧对核心坍缩超新星的中微子驱动爆炸的潜在影响。通过改变中微子的光度和衰变时间来获得具有或不具有13同位素α网络的一维和二维（分别为1D和2D）模型中的参数爆炸，我们研究了包含核燃烧对4种祖模型的弹跳后动力学的影响；15.0 M☉的恒星有3颗，11.2 M☉的恒星有1颗。我们发现激波后面的落入物质的核燃烧所产生的能量供应可以为激波膨胀提供能量，特别是对于在没有核燃烧的情况下只产生边际爆炸的模型。当激波锋面穿过富硅层和/或稍后接触富氧层时，这些模型通过核能沉积获得能量。根据中微子的光度和衰变时间，与没有核燃烧的模型相比，有核燃烧的模型的爆炸诊断能量增加了几倍。我们指出，这些特征在一维和二维的Limongi-Chieffi祖模型中最为显著，因为该祖模型具有一个巨大的氧层，其内缘半径是所使用的祖模型中最小的，这意味着激波在弹跳后可以在更短的时间尺度上接触到丰富的燃料。二维的能量差（~ 0.1-0.2× 10 51 erg）通常小于一维的（最多~ 0.6× 10 51 erg）。这是因为二维模型中中微子驱动的对流和激波不稳定性提高了中微子的加热效率，使得核燃烧的贡献相对于一维模型相对较小。考虑到祖模型的不确定性，我们的结果表明，核燃烧应该仍然是促进中微子驱动爆炸发生的重要因素之一。
We revisit potential impacts of nuclear burning on the onset of the neutrino-driven explosions of core-collapse supernovae. By changing the neutrino luminosity and its decay time to obtain parametric explosions in one-and two-dimensional (1D and 2D, respectively) models with or without a 13 isotope α network, we study how the inclusion of nuclear burning could affect the postbounce dynamics for 4 progenitor models; 3 for 15.0 M☉ stars and 1 for an 11.2 M☉ star. We find that the energy supply due to the nuclear burning of infalling material behind the shock can energize the shock expansion, especially for models that produce only marginal explosions in the absence of nuclear burning. These models are energized by nuclear energy deposition when the shock front passes through the silicon-rich layer and/or later as it touches the oxygen-rich layer. Depending on the neutrino luminosity and its decay time, the diagnostic energy of the explosion increases up to a few times 10 50 erg for models with nuclear burning compared to the corresponding models without. We point out that these features are most remarkable for the Limongi–Chieffi progenitor in both 1D and 2D because the progenitor model possesses a massive oxygen layer, with an inner-edge radius that is smallest among the employed progenitors, which means that the shock can touch the rich fuel on a shorter timescale after bounce. The energy difference is generally smaller (∼ 0.1–0.2× 10 51 erg) in 2D than in 1D (at most∼ 0.6× 10 51 erg). This is because neutrino-driven convection and the shock instability in 2D models enhance the neutrino heating efficiency, which makes the contribution of nuclear burning relatively smaller compared to 1D models. Considering uncertainties in progenitor models, our results indicate that nuclear burning should remain one of the important ingredients to foster the onset of neutrino-driven explosions.