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• 1. [Article] Solidification and Morphology of Submarine Lavas: A Dependence on Extrusion Rate

  The results of recent laboratory experiments with wax extruded beneath relatively cold water may be extrapolated to predict the surface morphology of submarine lavas as a function of the extrusion rate ...

  Citation × Citation Citation Abstract Copy Title: Solidification and Morphology of Submarine Lavas: A Dependence on Extrusion Rate Author: Griffiths, Ross W., Fink, Jonathan H. Year: 1992 The results of recent laboratory experiments with wax extruded beneath relatively cold water may be extrapolated to predict the surface morphology of submarine lavas as a function of the extrusion rate and melt vIscosity. The experiments with solidifying wax indicated that the surface morphology was controlled by a single parameter, the ratio of the time taken for the surface to solidify, and a time scale for lateral flow. For submarine basalts a solution of the cooling problem (which is dominated by conduction in the lava but convective heat transfer in the water) and estimates of lava viscosities place this parameter within the empirically determined "pillowing" regime over a Wide range of extrusion rates. This result is consistent with the observation that pillow basalts are the most common products of submarine eruptions. Smoother surfaces corresponding to the various types .of submarine sheet flows are predicted for sufficiently rapid extrusions of basaltic magma. Still higher eruption rates ID regions of low topographic relief may produce submarine lava lakes. Minimum emplacement times can be calculated for submarine volocanic constructs of a single lava flow type. Title: Solidification and Morphology of Submarine Lavas: A Dependence on Extrusion Rate Author: Griffiths, Ross W., Fink, Jonathan H. Year: 1992 The results of recent laboratory experiments with wax extruded beneath relatively cold water may be extrapolated to predict the surface morphology of submarine lavas as a function of the extrusion rate and melt vIscosity. The experiments with solidifying wax indicated that the surface morphology was controlled by a single parameter, the ratio of the time taken for the surface to solidify, and a time scale for lateral flow. For submarine basalts a solution of the cooling problem (which is dominated by conduction in the lava but convective heat transfer in the water) and estimates of lava viscosities place this parameter within the empirically determined "pillowing" regime over a Wide range of extrusion rates. This result is consistent with the observation that pillow basalts are the most common products of submarine eruptions. Smoother surfaces corresponding to the various types .of submarine sheet flows are predicted for sufficiently rapid extrusions of basaltic magma. Still higher eruption rates ID regions of low topographic relief may produce submarine lava lakes. Minimum emplacement times can be calculated for submarine volocanic constructs of a single lava flow type. Close

• 2. [Article] The Morphology of Lava Flows in Planetary Environments: Predictions From Analog Experiments

  The rates of surface cooling and lateral spreading are evaluated for lava flows on the surface of Earth, Venus, Mars, the Moon, and 10. Differences between the flow morphologies expected in these environments ...

  Citation × Citation Citation Abstract Copy Title: The Morphology of Lava Flows in Planetary Environments: Predictions From Analog Experiments Author: Griffiths, Ross W., Fink, Jonathan H. Year: 1992 The rates of surface cooling and lateral spreading are evaluated for lava flows on the surface of Earth, Venus, Mars, the Moon, and 10. Differences between the flow morphologies expected in these environments are then predicted under the assumption that the results of recent laboratory simulations oflavas using wax extruded beneath cold water (Fink and Griffiths, 1990) can be carried over. These experiments involved the spreading of viscous liquid under gravity in the presence of a solidifying surface crust and revealed a set of four distinct surface morphologies. Transitions from one morphology to the next occurred in a well-defined sequence when the relative rates of surface solidification and lateral spreading were varied. In comparison with subaerial flows on Earth, the surface of lavas solidifies faster on Venus, where the dense atmosphere provides additional convective heat transfer. Lateral flow oflava is much slower under the smaller gravity of the Moon. Hence, for a given extrusion rate and viscosity, solid crust is predicted to form closer to the vent on both the Moon and Venus than on Earth. Equivalently, faster extrusion rates than those on Earth are required on the Moon, 10, and Venus in order to produce a given surface morphology. A comparison of observed structure, flow rates, and estimated viscosities for some well-documented terrestrial lava flows shows reasonable agreement with the predictions of the model. Extrapolation to extraterrestrial lavas is then illustrated by constraining the effusion rate for a Martian lava flow whose composition is assumed. Spectral information on the chemical composition of Martian flows to be sought by the thermal emission spectrometer on the Mars Observer mission, in conjunction with detailed morphologic observations from the Mars Observer camera, could allow much more accurate estimates of effusion rates for Martian lavas. Title: The Morphology of Lava Flows in Planetary Environments: Predictions From Analog Experiments Author: Griffiths, Ross W., Fink, Jonathan H. Year: 1992 The rates of surface cooling and lateral spreading are evaluated for lava flows on the surface of Earth, Venus, Mars, the Moon, and 10. Differences between the flow morphologies expected in these environments are then predicted under the assumption that the results of recent laboratory simulations oflavas using wax extruded beneath cold water (Fink and Griffiths, 1990) can be carried over. These experiments involved the spreading of viscous liquid under gravity in the presence of a solidifying surface crust and revealed a set of four distinct surface morphologies. Transitions from one morphology to the next occurred in a well-defined sequence when the relative rates of surface solidification and lateral spreading were varied. In comparison with subaerial flows on Earth, the surface of lavas solidifies faster on Venus, where the dense atmosphere provides additional convective heat transfer. Lateral flow oflava is much slower under the smaller gravity of the Moon. Hence, for a given extrusion rate and viscosity, solid crust is predicted to form closer to the vent on both the Moon and Venus than on Earth. Equivalently, faster extrusion rates than those on Earth are required on the Moon, 10, and Venus in order to produce a given surface morphology. A comparison of observed structure, flow rates, and estimated viscosities for some well-documented terrestrial lava flows shows reasonable agreement with the predictions of the model. Extrapolation to extraterrestrial lavas is then illustrated by constraining the effusion rate for a Martian lava flow whose composition is assumed. Spectral information on the chemical composition of Martian flows to be sought by the thermal emission spectrometer on the Mars Observer mission, in conjunction with detailed morphologic observations from the Mars Observer camera, could allow much more accurate estimates of effusion rates for Martian lavas. Close

• 3. [Article] Lava and Ice Interaction at Stratovolcanoes: Use of Characteristic Features to Determine Past Glacial Extents and Future Volcanic Hazards

  Structures resulting from lava and ice interaction are common at glaciated stratovolcanoes. During summit eruptions at stratovolcanoes, meltwater is produced and travels freely down steep slopes and thin ...

  Citation × Citation Citation Abstract Copy Title: Lava and Ice Interaction at Stratovolcanoes: Use of Characteristic Features to Determine Past Glacial Extents and Future Volcanic Hazards Author: Lescinsky, David T., Fink, Jonathan H. Year: 2000 Structures resulting from lava and ice interaction are common at glaciated stratovolcanoes. During summit eruptions at stratovolcanoes, meltwater is produced and travels freely down steep slopes and thin permeable valley glaciers, eroding the ice and enlarging preexisting glacial drainages. As a result, in this environment have produced few catastrophic floods. Lava flowing into the open channels and voids in the glaciers becomes confined and grows thicker, filling the available space and producing steep-sided bodies with smooth, bulbous contact surfaces. Quenching of lava against ice or by water forms small-scale features such as tensional fractures and glass. As the amount of meltwater in contact with the lava increases, the type and abundance of smaller-scale features become similar to those produced during subglacial eruptions in meltwater lakes. Identification of large- and small-scale lava-ice contact features in the field can be used to reconstruct paleoglacial extent and, combined with geochronology of lavas, to determine past paleoclimate. An understanding of lava-ice interaction allows us to better access the hazards posed by future eruptions at glaciated volcanoes. Title: Lava and Ice Interaction at Stratovolcanoes: Use of Characteristic Features to Determine Past Glacial Extents and Future Volcanic Hazards Author: Lescinsky, David T., Fink, Jonathan H. Year: 2000 Structures resulting from lava and ice interaction are common at glaciated stratovolcanoes. During summit eruptions at stratovolcanoes, meltwater is produced and travels freely down steep slopes and thin permeable valley glaciers, eroding the ice and enlarging preexisting glacial drainages. As a result, in this environment have produced few catastrophic floods. Lava flowing into the open channels and voids in the glaciers becomes confined and grows thicker, filling the available space and producing steep-sided bodies with smooth, bulbous contact surfaces. Quenching of lava against ice or by water forms small-scale features such as tensional fractures and glass. As the amount of meltwater in contact with the lava increases, the type and abundance of smaller-scale features become similar to those produced during subglacial eruptions in meltwater lakes. Identification of large- and small-scale lava-ice contact features in the field can be used to reconstruct paleoglacial extent and, combined with geochronology of lavas, to determine past paleoclimate. An understanding of lava-ice interaction allows us to better access the hazards posed by future eruptions at glaciated volcanoes. Close