Volatiles in glasses from Mauna Loa Volcano, Hawai'i: implications for magma degassing and contamination, and growth of Hawaiian volcanoes

Davis, Michael G.; Garcia, Michael O.; Wallace, Paul

doi:10.1007/s00410-002-0416-z

Cited by 60 publications

(79 citation statements)

References 66 publications

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“…Rhenium volatility in Hawaiian basalts have Ͻ200 ppm S, consistent with substantial degassing of the magmas in shallow chambers or at the surface (Moore and Fabbi, 1971;Swanson and Fabbi, 1973;Davis et al, 2003). Other glasses from both Ko'olau and Moloka'i have high S contents (880 -1427 ppm; Tables 1 and 2), similar to undegassed Hawaiian magmas (Moore and Fabbi, 1971;Davis et al, 2003).…”

mentioning

confidence: 58%

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Rhenium and chalcophile elements in basaltic glasses from Ko’olau and Moloka’i volcanoes: Magmatic outgassing and composition of the Hawaiian plume

Norman¹,

Garcia²,

Bennett³

2004

Geochimica et Cosmochimica Acta

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confidence: 58%

“…Those samples with the highest S contents must be close to S-saturation (see, e.g., Fig. 4 of Davis et al, 2003), although sulfides were not observed petrographically in any of the samples studied here. Most of the Ko'olau glasses and one of the Moloka'i samples Reference values (RV) for BCR-1, BIR-1, and BHVO-1 are from Govindaraju (1994).…”

Section: Sulfurmentioning

confidence: 84%

Rhenium and chalcophile elements in basaltic glasses from Ko’olau and Moloka’i volcanoes: Magmatic outgassing and composition of the Hawaiian plume

Norman¹,

Garcia²,

Bennett³

2004

Geochimica et Cosmochimica Acta

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“…When present, it is generally small (<0.5 mm). Many Lō`ihi lavas also have FeS globules in matrix glass (Byers et al, 1985;Yi et al, 2000), which are rarely observed in lavas from other Hawaiian volcanoes (e.g., Davis et al, 2003b).…”

Section: Petrography and Mineral Chemistry: Magma History Implicationsmentioning

confidence: 99%

Geology, geochemistry and earthquake history of Lṑihi Seamount, Hawaìi's youngest volcano

et al. 2006

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A half century of investigations are summarized here on the youngest Hawaiian volcano, Lō`ihi Seamount. It was discovered in 1952 following an earthquake swarm. Surveying in 1954 determined it has an elongate shape, which is the meaning of its Hawaiian name. Lō`ihi was mostly forgotten until two earthquake swarms in the 1970's led to a dredging expedition in 1978, which recovered young lavas. This led to numerous expeditions to investigate the geology, geophysics, and geochemistry of this active volcano. Geophysical monitoring, including a realtime submarine observatory that continuously monitored Lō`ihi's seismic activity for three months, captured some of the volcano's earthquake swarms. The 1996 swarm, the largest recorded in Hawai`i, was preceded by at least one eruption and accompanied by the formation of a ~300-m deep pit crater, renewing interest in this submarine volcano. Seismic and petrologic data indicate that magma was stored in a ~8-9 km deep reservoir prior to the 1996 eruption.Studies on Lō`ihi have altered conceptual models for the growth of Hawaiian and other oceanic island volcanoes and led to a refined understanding of mantle plumes. Petrologic and geochemical studies of Lō`ihi lavas showed that the volcano taps a relatively primitive part of the Hawaiian plume, producing a wide range of magma compositions. These compositions have become progressively more silica-saturated with time reflecting higher degrees of partial melting as the volcano drifts towards the center of the hotspot. Seismic and bathymetric data have highlighted the importance of landsliding in the early formation of an ocean island volcano.Lō`ihi's internal structure and eruptive behavior, however, cannot be fully understood without installing monitoring equipment directly on the volcano.

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“…Olivine phenocrysts with primitive major element compositions (Fo 88-91 [Davis et al, 2003;Norman and Garcia, 1999]) were measured for this study. Mg isotopic compositions of these phenocrysts range from e sc = À2.5 to +2.5 (Figure 1 and Table 1).…”

Section: Hawaiian Picritesmentioning

confidence: 99%

Magnesium isotopic composition of olivine from the Earth, Mars, Moon, and pallasite parent body

Norman

Yaxley

Bennett

et al. 2006

Geophysical Research Letters

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[1] To investigate the nebular history of material contributing to the terrestrial planets, and search for evidence of a high-temperature origin of the Moon, we measured Mg isotopic compositions of primitive olivines from the Earth, Moon, Mars, and pallasite parent body using laser-ablation multi-collector ICPMS. No temporal variation in the Earth's mantle since at least 3.8 Ga, and only limited variations in the compositions of mantle sources from diverse tectonic settings were found. Earth, Moon, Mars, and differentiated asteroids appear to have formed from a nebular reservoir that was homogeneous with respect to Mg isotopes. This implies either a minor role for evaporationcondensation in the inner solar system, or a limited variation in the proportion of refractory CAI-like material contributing to the terrestrial planets. The Mg isotopic composition of the Moon is identical to the Earth's mantle, placing strong constraints on any volatility-related fractionation that occurred during formation of the Moon.

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Volatiles in glasses from Mauna Loa Volcano, Hawai'i: implications for magma degassing and contamination, and growth of Hawaiian volcanoes

Cited by 60 publications

References 66 publications

Rhenium and chalcophile elements in basaltic glasses from Ko’olau and Moloka’i volcanoes: Magmatic outgassing and composition of the Hawaiian plume

Rhenium and chalcophile elements in basaltic glasses from Ko’olau and Moloka’i volcanoes: Magmatic outgassing and composition of the Hawaiian plume

Geology, geochemistry and earthquake history of Lṑihi Seamount, Hawaìi's youngest volcano

Magnesium isotopic composition of olivine from the Earth, Mars, Moon, and pallasite parent body

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