The physical and chemical evolution of magmatic fluids in near-solidus silicic magma reservoirs: Implications for the formation of pegmatites

2021 ◽  
2019 ◽  
Author(s):  
Jordan Lubbers ◽  
◽  
Adam J.R. Kent ◽  
Frank Tepley ◽  
Dawid Szymanowski

Geofluids ◽  
2018 ◽  
Vol 2018 ◽  
pp. 1-22 ◽  
Author(s):  
Ane K. Engvik ◽  
Heinrich Taubald ◽  
Arne Solli ◽  
Tor Grenne ◽  
Håkon Austrheim

New stable isotopic data from mineral separates of albite, scapolite, amphibole, quartz, and calcite of metasomatic rocks (Bamble lithotectonic domain) give increased knowledge on fluid type, source, and evolution during metamorphism. Albite from a variety of albitites givesδ18OSMOWvalues of 5.1–11.1‰, while quartz from clinopyroxene-bearing albitite gives 11.5–11.6‰.δ18OSMOWvalues for calcite samples varies between 3.4 and 12.4‰and shows more consistentδ13C values of −4.6 to-6.0‰. Amphibole from scapolite metagabbro yields aδ18OSMOWvalue of 4.3 to 6.7‰andδDSMOWvalue of −84 to −50‰, while the scapolite givesδ18OSMOWvalues in the range of 7.4 to10.6‰. These results support the interpretation that the original magmatic rocks were metasomatised by seawater solutions with a possible involvement from magmatic fluids. Scapolitisation and albitisation led to contrasting chemical evolution with respect to elements like P, Ti, V, Fe, and halogens. The halogens deposited as Cl-scapolite were dissolved by albitisation fluid and reused as a ligand for metal transport. Many of the metal deposits in the Bamble lithotectonic domain, including Fe-ores, rutile, and apatite deposits formed during metasomatism. Brittle to ductile deformation concurrent with metasomatic infiltration illustrates the dynamics and importance of metasomatic processes during crustal evolution.


2012 ◽  
Vol 10 (H16) ◽  
pp. 341-341
Author(s):  
Jonathan Braine

AbstractThe physical and chemical evolution of galaxies is intimately linked to star formation, We present evidence that molecular gas (H2) is transformed into stars more quickly in smaller and/or subsolar metallicity galaxies than in large spirals – which we consider to be equivalent to a star formation efficiency (SFE). In particular, we show that this is not due to uncertainties in the N(H2)/Ico conversion factor. Several possible reasons for the high SFE in galaxies like the nearby M33 or NGC 6822 are proposed which, separately or together, are the likely cause of the high SFE in this environment. We then try to estimate how much this could contribute to the increase in cosmic star formation rate density from z = 0 to z = 1.


2021 ◽  
Author(s):  
Ben Ellis ◽  
et al.

Supplemental Figures S1–S8 (additional compositional information relevant to this study), and a supplemental dataset (all new data for this study and reference materials).<br>


2021 ◽  
Author(s):  
Ben Ellis ◽  
et al.

Supplemental Figures S1–S8 (additional compositional information relevant to this study), and a supplemental dataset (all new data for this study and reference materials).<br>


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