论文标题
在各向同性和各向异性场景中，在II-P型核心偏转超新星的块状喷射中的粉尘的形成，分布和红外发射
Formation, distribution, and IR emission of dust in the clumpy ejecta of Type II-P core-collapse supernovae, in isotropic and anisotropic scenarios
论文作者
论文摘要
在探索核心偏曲超新星射出中形成的灰尘特征时，观察性估计值和理论预测之间存在很大的差异。我们在爆炸后的前3000天内重新审视了典型的超新星喷射中粉尘产生的情况，并提高了人们对不断发展的物理条件和团块分布的了解。确定了喷射中灰尘的通用，不均匀的分布，并使用它，计算了相关的不混凝度和通量。对于模仿SN 1987a的射流的各向异性，椭圆形的几何形状，估计出现的通量对视角的依赖性。我们将HE-core从中心到外边缘建模为450个分层，块状，环形壳，以其独特的速度独特地识别，并以其丰度，密度以及气体和灰尘温度的变化为特征。我们发现，灰尘的形成开始于第450天和爆炸后第550天，并且一直持续到大约2800天，尽管最初的1600天是最有生产力的。总灰尘质量从第500天的大约10^-5 msun演变为第800天的10^-3 msun，最终以约0.06 msun饱和。富含O的粉尘（硅酸盐，氧化铝）的质量始终统治着富含C的粉尘（无定形碳，碳化硅）。碳灰尘的形成延迟到爆炸后2000天以上。我们表明，在第800天到1600天之间，不透明性是最大的，并且在那个时候抑制了富含O的灰尘物种的特征。发现沿椭圆形弹出的最小轴出现的通量被发现是最模糊的，而与该轴的16至21度之间的视角似乎与SN 1987a的第615天和775天的磁通量是最好的一致性。
Large discrepancies are found between observational estimates and theoretical predictions when exploring the characteristics of dust formed in the ejecta of core-collapse supernovae. We revisit the scenario of dust production in typical supernova ejecta in the first 3000 days after explosion, with an improved understanding of the evolving physical conditions and the distribution of the clumps. The generic, nonuniform distribution of dust within the ejecta was determined and using that, the relevant opacities and fluxes were calculated. The dependence of the emerging fluxes on the viewing angle was estimated for an anisotropic, ellipsoidal geometry of the ejecta that imitate SN 1987A. We model the He-core from the center to its outer edge as 450 stratified, clumpy, annular shells, uniquely identified by their distinct velocities and characterized by their variations in abundances, densities, and gas and dust temperatures. We find that the formation of dust starts between day 450 and day 550 post-explosion, and it continues until about day 2800, although the first 1600 days are the most productive. The total dust mass evolves from about 10^-5 Msun at day 500 to 10^-3 Msun at day 800, finally saturating at about 0.06 Msun. The masses of the O-rich dust (silicates, alumina) dominates the C-rich dust (amorphous carbon, silicon carbide) at all times; the formation of carbon dust is delayed beyond 2000 days post-explosion. We show that the opacities are largest between days 800 and 1600, and the characteristic spectral features of O-rich dust species are suppressed at those times. The fluxes emerging along the smallest axes of the ellipsoidal ejecta are found to be the most obscured, while a viewing angle between 16 and 21 degrees with that axis appears to be in the best agreement with the fluxes from SN 1987A at days 615 and 775.
