Dust Formation in Core Collapse Supernovae

超新星（SN）不仅锻造了H，He，Li之外的化学元素-使多样化的化学（和生物学）成为可能-它们也是宇宙尘埃的来源，这对行星的形成至关重要。附近恒星的化学丰度异常表明，SN向我们的母分子云注入了富集的物质，但对行星形成的影响尚不清楚。为了更好地了解SN的可能影响，该团队将使用3D模拟来模拟核心塌陷SN中的尘埃形成。将计算尘埃颗粒丰度的变化，并将其与陨石太阳前颗粒中元素和同位素比率的实验室数据进行比较。加入尘埃形成的数值模拟与实验室同位素分析的陨石在不断变化的SN残留物将导致更好地了解前者是如何转化为后者。该奖项还将支持研究生培训以及基于拟议研究的天文馆演示设计。本研究的三个主要目的是：（1）预测超新星遗迹结构演化过程中的尘埃成分。这包括计算喷出物的同位素组成和计算尘埃的形成/破坏;（2）使用实验室测量和文献结果将模拟尘埃颗粒的同位素组成与太阳前尘埃颗粒的同位素组成进行比较;（3）评估颗粒作为早期太阳系同位素异常的来源。 一系列超新星爆炸将使用该团队的超新星光滑粒子流体动力学（SNSPH）代码进行建模。将进行模拟，从喷出物的爆炸“发射”到残余物演变的Sedov阶段。将使用PRISM后处理代码计算模拟中每个SNSPH粒子的同位素产额。随后的尘埃形成计算将使用nuDust，它将气相化学、颗粒形成、颗粒生长以及颗粒破坏和风化结合起来。nuDust还将使用材料的模拟热力学历史来预测SNSPH模拟中每个颗粒中尘埃颗粒的组成和尺寸分布。实验室测量和出版的高精度同位素数据，粒度和矿物学的汇编，从各种全岩陨石，钙铝夹杂物，和星尘颗粒将被用来评估同位素之间的相关性和非-该奖项反映了NSF的法定使命，并被认为是值得支持的，使用基金会的知识价值和更广泛的影响审查标准进行评估。

Supernovae (SN) not only forge chemical elements beyond H, He, & Li - making possible a diverse chemistry (and biology) - they are also sources of cosmic dust, which is essential for the formation of planets. Chemical abundance anomalies among nearby stars suggest the injection of enriched material into our parent molecular cloud by SN, with unclear implications for planet formation. To better understand the possible impact of SN, the team will model dust formation in core-collapse SN using 3D simulations. Dust grain abundance variations will be calculated and compared with laboratory data on elemental and isotopic ratios in pre-solar grains from meteorites. Joining numerical simulations of dust formation in evolving SN remnants with laboratory isotopic analysis of meteorites will lead to a better understanding of how the former is transformed into the latter. This award will also support graduate student training as well as the design of planetarium presentations based on the proposed research. The three main objectives of this study are: (1) predicting the dust composition of SN remnant structures as the they evolve. This includes computing the ejecta's isotopic composition and calculating dust formation/destruction; (2) comparing the modeled dust grain's isotopic composition with those of pre-solar dust grains using laboratory measurements and results from the literature; and (3) assessing grains as a source of isotopic anomalies in the early solar system. A suite of supernova explosions will be modeled using the team's Supernova Smooth Particle Hydrodynamic (SNSPH) code. Simulations will be carried out from the explosive "launch" of the ejecta to the Sedov phase of the remnant evolution. Isotopic yields of each SNSPH particle in the simulations will be calculated using the PRISM post-processing code. Subsequent dust formation calculations will use use nuDust, which couples gas phase chemistry, grain formation, grain growth as well as grain destruction and weathering. nuDust will also use the simulated thermodynamic histories of the material to predict the composition and size distribution of dust grains in each particle of the SNSPH simulation. Laboratory measurements and a compilation of published high precision isotopic data, grain sizes, and mineralogies from a variety of whole-rock meteorites, calcium-aluminum inclusions, and stardust grains will be used to assess isotopic correlations between and among non-carbonaceous and carbonaceous chondrite reservoirs in the context of new models produced by this work.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.