No description available.

The San Rafael Volcanic Field, Utah, is a 4.6 Ma extinct monogenetic field that is found in the Northern Transition Zone of the Colorado Plateau. The field has been eroded, leaving the dikes, conduits, and sills visible. Within the sills we see evidences of immiscibility in the form of an intermediate syenite (~50 wt% SiO2) enclosed in a mafic shonkinite (~48 wt % SiO2). Field relations indicate that sills were formed due to single events (Richardson et al., 2015), which makes in-situ differentiation the process at the origin of both rock types. Geochemical data supports differentiation of syenite and shonkinite from a single melt. The syenites are more enriched in LREE than shonkinites. The rocks are enriched in LREE compared to an OIB source, indicating melting of a hydrated lithosphere interacting with an asthernospheric garnet peridotite. Olivine with a composition of Fo80-90 further support asthernospheric origin, and pyroxenes indicate that depth of crystallization would have begun around 33 Km, indicating that the melt would have pooled at the base of the crust as it traveled, supporting base of the lithosphere origins. Rhyolite-MELTS modeling further supports differentiation within the sills as the formations of feldspars, biotite and hornblende did not occur until ~800m which would have allowed for fractional crystallization to occur, leading to the immiscibility process and resulting formation of syenite and shonkinite.

Thesis (Ph. D.)--Washington State University, December 2007. / Includes bibliographical references.

Thesis (Ph. D.)--Massachusetts Institute of Technology and woods Hole Oceanographic Institution, 1982. / Bibliography: p. 265-290.

Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Earth and Planetary Science, 1982. / Supervised by William J. Jenkins. Includes bibliographical references (leaves 265-290).

The super-giant Oyu Tolgoi porphyry copper-gold deposits in the South Gobi desert, Mongolia, consist of multiple discrete porphyry centers aligned within a north-northeast trending, >6.5 km long, arc-transverse mineralized corridor. The porphyries are linked to a tectono-magmatic event at ~372 Ma within a Devonian to Carboniferous volcanic arc, and U-Pb (zircon) geochronology records magmatic activity from ~390 Ma to ~320 Ma. The Oyu Tolgoi district underwent at least three discrete periods of syn- to post-mineral shortening and there is evidence for at least three unconformities within the Paleozoic sequence. Although the deposits were formed in an active orogenic environment characterized by rapid uplift, their preservation is a reflection of climactic effects as well insulation from erosion by rapid burial under mass-wasted and pyroclastic material in the volcaniclastic apron of late-mineral dacitic volcanoes. The porphyry copper-gold deposits are spatially and temporally related to medium- to high-K calc-alkaline quartz monzodiorite (~372 Ma) and granodiorite (~366 Ma) intrusive phases that comprise the Late Devonian Oyu Tolgoi Igneous Complex (OTIC). Adakite-like wholerock compositions as well as zircon grains with high CeN/CeN*, EuN/EuN* and Yb/Gd in the sample populations from syn- and late-mineral porphyry intrusions are different from younger intrusions that are not related to porphyry Cu-Au deposit formation. Moreover, mixed zircon populations within OTIC intrusions indicate that efficient assimilation of material from different host rocks by a convecting magma chamber occurred. Mafic to intermediate volcanic units evolved from tholeiitic to calc-alkaline compositions, which is interpreted to be a reflection of marine arc maturation and thickening. Felsic rock suites are dominantly high-K calc-alkaline, regardless of age. Nd-isotopic geochemistry from all suites is consistent with magma derivation from depleted mantle in an intra-oceanic volcanic arc and lead isotopic compositions indicate that the sulfides in the porphyry Cu-Au deposits are genetically linked to the Late Devonian magmas. Magma mixing, adakite-like magmatism and rapid uplift and erosion in a juvenile marine arc setting differentiate the ore-stage geologic environment at Oyu Tolgoi from other settings in active and fossil volcanic arcs.

Thesis (M.S.)--Western Washington University, 2010. / Includes bibliographical references (leaves 45-51). Also issued online.

No description available.

My dissertation details the work I have done related to remote sensing of thermal activityon Io and thermal remote sensing used in the search for oases on Mars. At Io, I studiedtwo volcanoes, Tvashtar and Prometheus and their thermal activity. At Mars, I investigatedsuggestions of a possible oasis in one of the youngest volcanic regions, Cerberus Fossaeand nearby areas of SE Elysium.Tvashtar was the site of the first high-spatial-resolution observation of an extraterrestriallava curtain. The Tvashtar complex was also the site of a large, confined eruption a fewmonths after the fissure eruption. I discuss the work involved in estimating the brightnesstemperatures and power output of both eruptions as seen by the Galileo SSI. I also discusscooling and eruption-style models and their application to Tvashtar. In every geometricallycorrect observation of Prometheus, we have seen a 100 km tall SO2 gas and dust plumeabove its flow field. This plume and field migrated ~80 km between the Voyager and Galileo eras. I describe the work I performed in modeling the plume's creation as lava-volatileinteractions at the flow fronts.My Mars research entailed the search for thermal systems and constraints on nearsurfacewater ice in an equatorial region that contains some of the youngest lava flows onMars. This region, SE Elysium, also shows evidence of contemporaneous water and lava. Life as we know it requires a source of energy and liquid water, so a geologically youngregion containing both water and energy is an obvious place to study. I show, however, thatthe recent suggestions of extant near-surface water ice and possible endogenic energy escapeare not necessary, and that the thermal imaging of the region requires rock rather thanwater ice near the surface. I also show that the current instruments at Mars are insufficientfor the remote discovery of thermal reservoirs and then discuss some possible remedies.

Paterae (volcano-tectonic depressions) are among the most prominent topographic features on Io. They are unique, yet in some aspects they resemble calderas known and studied on Earth, Mars, and Venus. They have steep walls, flat floors, and arcuate margins, typical of terrestrial and Martian basalt shield calderas. However, they are much larger (2 km - 202 km diameter, mean 42 km 3 km) and typically lack obvious shields. They are often angular in shape or are found adjacent to mountains, suggesting tectonic influences on their formation. A preferential clustering of paterae at the equatorial sub- and anti-jovian regions is likely a surface expression of tidal massaging and convection in the asthenosphere. Paterae adjacent to mountains have a mean diameter 14 km 9 km larger than that for all paterae, which may indicate paterae grow larger in the fractured crust near mountains. Nightside and eclipse observations of Pele Patera by the Cassini and Galileo spacecraft reveal that much of Pele’s visible thermal emission comes from lava fountains within a topographically confined lava body, most likely a lava lake. Multiple filter images provided color temperatures of 1500 80 K from Cassini ISS data, and 1420 100 K from Galileo SSI data. Hotspots found within paterae (79% of all hotspots) exhibit a wide range of thermal behaviors in global eclipse images. Some hotspots are similar to Pele, consistently bright and confined; others, such as Loki, brighten or dim between observations and move to different locations within their patera. A model for patera formation begins with heating and convection within a high-temperature, low-viscosity asthenosphere. Magma rises through the cold, dense lithosphere either as diapirs [for thermal softening of the lithosphere and sufficiently large diapirs (20 km - 40 km diameter, >5 km thickness)] or through dikes. Magma reaches zones of neutral buoyancy and forms magma chambers that feed eruptions. Collapse over high-level chambers results in patera formation, filling of the patera with lava to create a lava lake, or lateral spreading of the magma chamber and subsequent enlargement of the patera by consuming crustal materials.