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Image-based modelling of lateral magma flow: the Basement Sill Antarctica

机译:基于图像的岩浆横向流动建模:南极地下室

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摘要

The McMurdo Dry Valleys magmatic system, Antarctica, provides a world-class example of pervasive lateral magma flow on a continental scale. The lowermost intrusion (Basement Sill) offers detailed sections through the now frozen particle microstructure of a congested magma slurry. We simulated the flow regime in two and three dimensions using numerical models built on a finite-element mesh derived from field data. The model captures the flow behaviour of the Basement Sill magma over a viscosity range of 1–104 Pa s where the higher end (greater than or equal to 102 Pa s) corresponds to a magmatic slurry with crystal fractions varying between 30 and 70%. A novel feature of the model is the discovery of transient, low viscosity (less than or equal to 50 Pa s) high Reynolds number eddies formed along undulating contacts at the floor and roof of the intrusion. Numerical tracing of particle orbits implies crystals trapped in eddies segregate according to their mass density. Recovered shear strain rates (10−3–10−5 s−1) at viscosities equating to high particle concentrations (around more than 40%) in the Sill interior point to shear-thinning as an explanation for some types of magmatic layering there. Model transport rates for the Sill magmas imply a maximum emplacement time of ca 105 years, consistent with geochemical evidence for long-range lateral flow. It is a theoretically possibility that fast-flowing magma on a continental scale will be susceptible to planetary-scale rotational forces.
机译:南极麦克默多干旱谷的岩浆系统提供了一个遍及全球的横向岩浆流动的世界一流例子。最下层的侵入(基底门槛)提供了拥挤的岩浆浆液的现在冻结的微粒微观结构的详细部分。我们使用基于从现场数据得出的有限元网格建立的数值模型来模拟二维和三维流动状态。该模型捕获了粘度范围为1–10 4 Pa s的基底槛岩浆的流动行为,其中较高端(大于或等于10 2 Pa s )对应于晶体比例在30%至70%之间变化的岩浆。该模型的一个新颖特征是发现了沿侵入层底部和顶部的波浪状接触形成的瞬时,低粘度(小于或等于50 Pa s)的高雷诺数涡流。粒子轨道的数值追踪表明,涡流中捕获的晶体根据其质量密度而分离。在粘度等于高颗粒浓度(大约40%以上)的情况下,恢复的剪切应变率(10 −3 –10 −5 s −1 ) )在西尔(Sill)内部指向剪切稀化,以解释那里的某些岩浆层。基尔岩浆​​的模型运移速率暗示最大进位时间约为10 5 年,这与长程侧向流的地球化学证据一致。从理论上讲,大陆尺度上快速流动的岩浆很容易受到行星尺度旋转力的影响。

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