Stardust interstellar dust calibration: Hydrocode modeling of impacts on Al‐1100 foil at velocities up to 300 km s−1 and validation with experimental data
Stardust interstellar dust calibration: Hydrocode modeling of impacts on Al‐1100 foil at velocities up to 300 km s−1 and validation with experimental data
复制标题
Stardust 星际尘埃校准：对速度高达 300 km s−1 的 Al-1100 箔片的影响进行 Hydrocode 建模并用实验数据进行验证
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发表时间：
2012
期刊：
影响因子：
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通讯作者：
M. Cole
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文献类型：
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作者：
M. Price;A. Kearsley;M. Burchell;L. Howard;J. Hillier;N. Starkey;P. Wozniakiewicz;M. Cole
摘要-我们介绍了影响Al-1100薄片的流体代码模拟的初步结果，这是为了帮助NASA星际尘埃任务星际尘埃收集盘的星际初步检查(ISPE)阶段进行的。我们使用Ansys的AUTODYN模拟了微米尺度和较小的抛射物对星尘箔(100 μm厚的Al-1100)的撞击，速度高达300 Km S−1。我们认为对星际集尘器箔的撞击可能是星际尘埃粒子、彗星上的星际尘埃粒子和小行星衍生轨道、β微流星体、太阳风中的纳米尘埃和航天器衍生的二次抛射的组合。因此，潜在冲击体的特征速度范围从<；<；1到几公里 S−1(二次抛射)，大约4-25 公里 S−1对于ISP和IdP，对于Meyer-Vernet等人报道的纳米尺度尘埃，高达数百公里 S−1。(2009)。目前还没有针对较高速度条件的广泛的实验校准，因此，这项工作的主要重点是使用流体代码模型来研究撞击坑的形态计量，作为一种手段来确定大约的撞击速度，从而确定起源。该模型根据现有的实验数据进行了验证，撞击速度高达约30 Km S−1，颗粒密度从2.4 kg m−3(玻璃)到7.8 kg m−3(铁)。给出了预测直径在10 0 nm~4 μm之间、密度在2.4~7.8 kg m−3之间的固体冲击器的弹坑深度和直径的插值式。
Abstract– We present initial results from hydrocode modeling of impacts on Al‐1100 foils, undertaken to aid the interstellar preliminary examination (ISPE) phase for the NASA Stardust mission interstellar dust collector tray. We used Ansys’ AUTODYN to model impacts of micrometer‐scale, and smaller projectiles onto Stardust foil (100 μm thick Al‐1100) at velocities up to 300 km s−1. It is thought that impacts onto the interstellar dust collector foils may have been made by a combination of interstellar dust particles (ISP), interplanetary dust particles (IDP) on comet, and asteroid derived orbits, β micrometeoroids, nanometer dust in the solar wind, and spacecraft derived secondary ejecta. The characteristic velocity of the potential impactors thus ranges from <<1 to a few km s−1 (secondary ejecta), approximately 4–25 km s−1 for ISP and IDP, up to hundreds of km s−1 for the nanoscale dust reported by Meyer‐Vernet et al. (2009) . There are currently no extensive experimental calibrations for the higher velocity conditions, and the main focus of this work was therefore to use hydrocode models to investigate the morphometry of impact craters, as a means to determine an approximate impactor speed, and thus origin. The model was validated against existing experimental data for impact speeds up to approximately 30 km s−1 for particles ranging in density from 2.4 kg m−3 (glass) to 7.8 kg m−3 (iron). Interpolation equations are given to predict the crater depth and diameter for a solid impactor with any diameter between 100 nm and 4 μm and density between 2.4 and 7.8 kg m−3.