Lunar Mare Lava Flow Dynamics and Emplacement: Predictions of Non-Newtonian Flow Dynamics, Syn- and Post-emplacement Cooling and Volatile Release Patterns, and Vertical and Lateral Flow Structure Development

Lionel Wilson, James W. Head
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Abstract

We apply basic principles of magma ascent from deep source regions and its eruption into a low-gravity vacuum environment to develop a theoretical treatment of the fluid dynamics and thermodynamics of mare basalt lava flow emplacement and evolution on the Moon. The vacuum conditions influenced the release of volatiles in magma passing through lava fountains, thus controlling the syn- and post-emplacement vesicularity of the resulting deposits. To explain observed lengths and volumes of Mare Imbrium–type flows, high (106–105 m3 s−1) initial magma eruption rates were needed. Combined with low lunar magma viscosity, these caused flows to be initially turbulent. Resulting high radiative heat loss and consequent high crystallization rates caused rapid non-Newtonian rheological evolution and suppression of turbulence at tens of kilometers from vents. Slower cooling rates in the subsequent laminar parts of flows imply distinctive crystal growth rate histories. In a four-phase sequence, (i) initial transient dike-tip gas release followed by (ii) Hawaiian fire fountain activity with efficient volatile loss (iii) transitioned to (iv) Strombolian explosions in a lava lake. Late-stage lava now able to retain volatiles intruded and inflated existing flow deposits after flow front advance ceased. Volatiles forced out of solution by second boiling as lava cooled caused additional inflation. Low gravity and lack of atmospheric pressure commonly produced very vesicular lava. Escape of such lava through cracks in flow crusts is a possible source of ring-moat dome structures; collapse of such lava may explain irregular mare patches.
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月球母岩熔岩流动力学和置换:非牛顿流体动力学、同步和置换后冷却与挥发物释放模式以及垂直和侧向流动结构发展的预测
我们运用岩浆从深源区上升并在低重力真空环境中喷发的基本原理,对月球上马雷玄武岩熔岩流的喷放和演化的流体动力学和热力学进行了理论研究。真空条件影响了岩浆通过熔岩喷泉时的挥发物释放,从而控制了所形成的沉积物的同步和置换后泡状结构。要解释所观测到的英布里姆马雷型熔岩流的长度和体积,需要较高的(106-105 立方米/秒-1)初始岩浆喷发率。加上月球岩浆粘度较低,这些因素导致流动最初是湍流的。由此产生的高辐射热损失和随之而来的高结晶率导致了快速的非牛顿流变演化,并抑制了距喷口数十公里处的湍流。随后层流部分的冷却速率较慢,这意味着晶体生长速率历史与众不同。在一个四阶段序列中,(i) 最初的瞬态堤顶气体释放,然后是(ii) 夏威夷火泉活动,并伴有有效的挥发损失(iii) 过渡到(iv) 熔岩湖中的血栓爆炸。晚期熔岩现在能够保留挥发物,在流锋停止前进后,侵入并膨胀了现有的流沉积物。熔岩冷却时,二次沸腾迫使挥发物从溶液中脱出,造成了更多的膨胀。低重力和缺乏大气压力通常会产生非常泡状的熔岩。这种熔岩通过流壳的裂缝流出,可能是环状穹隆结构的来源;这种熔岩的坍塌可能是不规则母岩斑块的原因。
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