Multiphase eruptions associated with the lunar craters Tycho and Aristarchus
Multiphase volcanic eruptions associated with lunar craters Tycho and Aristarchus
Fielder, G.↗
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Multiphase eruptions associated with the lunar craters Tycho and Aristarchus
Multiphase eruptions associated with lunar craters Tycho and Aristarchus - lava flow charts
Fielder, G.↗
The Hekla fires - A preliminary report of the 1970 Mount Hekla volcanic eruption. A report from the Smithsonian Insitution Center for Short-Lived Phenomena, 15 June 1970
Describing eruption in region of Mt. Hekla, Iceland and toxic hazards from volcanic ash
Thorarinsson, S.↗
Highlights of the Surtsey eruption - 1963 - 1967
Chronological summary of Surtsey volcano eruption from 1963 to 1967
Sigvaldason, G.↗
Hekla and the 1970 eruption
Reporting eruption of Hekla volcano from May through June 1970
Hoffer, J. M.↗
Fluorine-bearing ash from the Hekla eruption, 1970 - Distribution, effect on environment, and implications for Mediterranean archeology and geomythology
Investigating effects of Hekla volcano eruption on environment and economy of Iceland
Vitaliano, D. B.↗
A two-dimensional stratospheric model of the dispersion of aerosols from the Fuego volcanic eruption
Observational data of the pre- and post-volcanic aerosols from the eruption of the Volcan de Fuego in Guatemala (15 deg N) in October 1974 were used in conjunction with predictions of a 2-D circulation model to gain better understanding of the transport, chemical and sedimentation processes which determine the stratospheric aeosol layer.
Remsberg, E. E.↗
Vulcanian eruption mechanisms
Volcanological observations of explosive eruptions show that previous estimates of pre-explosion gas pressures may be overestimated by an order of magnitude.
Self, S.↗
Scanning Electron Microscopy and Petrography of Glassy Particles Produced by Lava Fountain Eruptions
A conceptual model of a lava fountain consists of a vent, spatter ramparts, fountain column, downwind plume and associated pumice deposits. Glassy particles produced by lava fountain eruptions consist primarily of sideromelane glass and minor to moderate amounts of vesicles and crystals. Particles are classified on the basis of morphology as: (1) spherical, (2) elongate, (3) glass-coated mineral grain, (4) shard, (5) reticulite, (6) composite particle, and (7) lithic fragment.
Ladle, G. H.↗
Mount Agung eruption provides test of a global climate perturbation
The Mt. Agung volcanic eruption in 1963 is used as a test case to examine the climatic response to a global-scale radiative perturbation of the earth's atmosphere.
Hansen, J. E.↗
The infrared variability of the eruptive variable HM Sagittae
Recent near infrared observations have been obtained of the peculiar eruptive variable HM Sagittae which show a general decrease in the flux levels between 1 and 5 microns during 1977-1978. The existing data are yet too sparse to ascertain the nature of the variability; however, both the IR and visual observations confirm the close resemblance of HM Sge to V1016 Cyg. A model of a binary symbiotic system containing a late type variable may be consistent with the current data.
Slovak, M. H.↗
Modeling lunar volcanic eruptions
Simple physical arguments are used to show that basaltic volcanos on different planetary bodies would fountain to the same height if the mole fraction of gas in the magma scaled with the acceleration of gravity. It is suggested that the actual eruption velocities and fountain heights are controlled by the velocities of sound in the two phase gas/liquid flows. These velocities are in turn determined by the gas contents in the magma. Predicted characteristics of Hawaiian volcanos are in excellent accord with observations. Assuming that the only gas in lunar volcano is the CO which would be produced if the observed Fe metal in lunar basalts resulted from graphite reduction, lunar volcanos would fountain vigorously, but not as spectacularly as their terrestrial counterparts. The volatile trace metals, halogens, and sulfur released would be transported over the entire moon by the transient atmosphere. Orange and black glass type pyroclastic materials would be transported in sufficient amounts to produce the observed dark mantle deposits.
Housley, R. M.↗
Photometric and radar observations of an excited eruption in the Zarnitsa-2 experiment
In a controlled experiment a ground photometer and radar station recorded an increase in night sky luminescence following injection of an electron beam into the atmosphere from a rocket at altitudes 80 to 154 km. A main and supplementary scattering and luminescene regions were observed. The effect is presumed to be due to electron eruption induced by artificial action on the magnetosphere.
Adeyshvili, T. G.↗
Trajectories of the Mount St. Helens eruption plume
The plume of the major eruption of Mount St. Helens on May 18, 1980 penetrated 10 to 11 km into the stratosphere, attaining heights of 22 to 23 km. Wind shears rapidly converted the plume from an expanding vertical cone to a thin, slightly inclined lamina. The lamina was extruded zonally in the stratosphere as the lower part moved eastward at jet stream velocities, while the upper part slowly moved westward in the region of nonsteady transition from the westerlies to the summer stratospheric easterlies. Trajectories computed to position the NASA U-2 aircraft for sampling in the plume are described. Plume volume after 8 hours of strong volcanic emission is estimated at 2,000,000 cu km. Only about 1% of this volume is attributed to the volcano; the rest was entrained from the environment.
Danielsen, E. F.↗
Gaseous constituents in the plume from eruptions of Mount St. Helens
Measurements in the stratosphere of gaseous constituents in the plume of Mount St. Helens were obtained during five flights of the NASA U-2 aircraft between 19 May and 17 June 1980. Mixing ratios from gas chromatographic measurements on samples acquired about 24 hours after the initial eruption show considerable enhancement over nonvolcanic concentrations for sulfur dioxide (more than 1000 times), methyl chloride (about 10 times), and carbon disulfide (more than 3 times). The mixing ratio of carbonyl sulfide was comparable to nonvolcanic mixing ratios although 3 days later it was enhanced two to three times. Ion chromatography measurements on water-soluble constituents are also reported. Very large concentrations of chloride, nitrate, and sulfate ions were measured, implying large mixing ratios for the water-soluble gaseous constituents from which the anions are derived. Measurements of radon-222 present in the plume are also reported.
Inn, E. C. Y.↗
Trace element composition of the Mount St. Helens plume - Stratospheric samples from the 18 May eruption
Atmospheric particulate material collected from the stratosphere in the plume of the 18 May 1980 eruption of the Mount St. Helens volcano was quite similar in composition to that of ash that fell to the ground in western Washington. However, there were small but significant differences in concentrations of some elements with altitude, indicating that the stratospheric material was primarily produced from fresh magma, not fragments of the mountain.
Vossler, T.↗
Volcanic origin of the eruptive plumes on Io
A quadruple long exposure of Io in eclipse exhibits faint auroral emission from the eruptive plumes. No luminous spots in the vents, predicted by Gold, were observed. Heat from the interior of Io appears to be the predominant source of energy in the plume.
Cook, A. F.↗
Ascent and eruption of basaltic magma on the earth and moon
The ascent and emplacement of basaltic magma on the earth and moon is modeled by the application of geological and physical observations and constraints. Relatively simple mathematical models of the motion of gas/liquid mixtures are shown to be adequate in the treatment of basaltic eruptions, provided that allowance is made for the coalescence of gas bubbles and that realistic geological and petrochemical constraints are applied to the numerical values of variables. Because gas exsolution from magmas on the earth and moon commonly occur at depths of less than 2 km, it is generally convenient to consider separately the rise of bubble-free magmatic liquid at depth in a planetary crust and the more complex motions occurring near the surface with gas exsolution.
Wilson, L.↗