The Athabasca Valles flood lava is among the most recent (<50 Ma) and best preserved effusive lava flows on Mars and was probably emplaced turbulently. The Williams et al. [2005] model of thermal erosion by lava has been applied to what we term "proximal Athabasca," the 75 km long upstream portion of Athabasca Valles. For emplacement volumes of 5000 and 7500 km3 and average flow thicknesses of ...

Accurate forecasts of lava flow length rely on estimates of eruption andmagma properties and, potentially more challengingly, on an understanding of the relative influence of characteristics such as the apparent viscosity, the yield strength of the flow core, or the strength of the lava’s surface crust. For basaltic lavas, the relatively high frequency of eruptions has resulted in numerous oppo...

Introduction: Lava flow surface morphology results from processes that occur during emplacement. Features such as tumuli and lava rises are indicators of flow inflation [1]. Tumuli in particular have been identified as possible indicators of lava tube location [2-5], indicating that their distribution on the surface of a lava flow is a function of the internal pathways of lava present during fl...

The 2D Cellular Automata model, MAGFLOW, simulates lava flows and an algorithm based on the Monte Carlo approach solves the anisotropic flow direction problem. The model was applied to reproduce a lava flow formed during the 2001 Etna eruption. This eruption provided the opportunity to verify the ability of MAGFLOW to simulate the path of lava flows which was made possible due to the availabili...

Fast-moving lava flows during the 2014–2015 eruption of Fogo volcano in Cape Verde engulfed 75% (n = 260) of buildings within three villages in the Chã das Caldeiras area, as well as 25% of cultivable agricultural land, water storage facilities and the only road into the area. The eruption had a catastrophic impact for the closeknit communities of Chã, destroying much of their property, land an...

Observations of terrestrial examples of lava and ice interaction have been combined with laboratory simulations to provide a framework for investigating lava and ice interaction on Mars. Identification of largeand small-scale characteristic features will indicate whether large quantities of meltwater were trapped or whether lava flow confinement occurred. These features should also enable the d...

[1] We present new evidence for volcanic eruptions and lava flow emplacement on Venus within the last several decades. An integrated study of a radar‐dark lava flow unit in Bereghinia Planitia on Venus (∼28°E, ∼39°N) based on Magellan data obtained in 1993 reveals a significant apparent microwave thermal emission excess, consistent with increased subsurface temperature due to very recent lava f...

Animating lava flowing down the slopes of a volcano brings several challenges: modeling the mechanical features of lava and how they evolve over time depending on temperature; computing, in a reasonable time, the interactions inside the flow, and between the flow and a complex terrain data-base; and lastly, rendering the visual aspect of the flow. The methods described rely on smoothed particle...

The rate at which lava emerges from a volcano is a fundamental property of the dynamics of the eruption. Intensive field measurements can capture this. However, for many, often cloud-covered, volcanoes with long-lived eruptions, spaceborne InSAR provides a potentially useful source of information. Repeated DEM creation at intervals allows the changing thickness of the lava flow field to be meas...

[1] Accurate lava flow unit thicknesses estimates are necessary to place constraints on volcanic flux estimates. We refine the technique of using the shape of crater size-frequency distribution (CSFD) curves to estimate the thickness of individual lunar mare flow units. We find that a characteristic knee often observed in CSFD curves is reasonably interpreted to represent the presence of two la...