Journal of Petrology Advance Access published online on January 7, 2009
Journal of Petrology, doi:10.1093/petrology/egn068
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Rhyolites and their Source Mushes across Tectonic Settings
Department of Earth and Space Sciences, University of Washington, Box 351310, Seattle, WA 98195-1310, USA
Received June 16, 2008; Revised typescript accepted November 19, 2008
| ABSTRACT |
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Evolved magmas, including highly explosive rhyolites, are mainly generated by extraction of viscous melts from solid residues either in (1) partial melting zones within the crust (dominantly up-temperature evolution with newly formed silicic melt), or in (2) long-lived crystallizing mush zones fed by mafic to intermediate magmas (dominantly down-temperature evolution with residual silicic melt). Although both processes undoubtedly occur and are generally coupled, allowing for mixing between mantle and crustal components, we argue that combined field, thermal, geochemical, and geophysical observations favor residual melt extraction from crystalline mushes as the likely scenario in all tectonic settings. Depending on the main melting process in the mantle, two end-member differentiation trends occur: (1) a dry lineage leading to hot-reduced rhyolites and granites in magmatic provinces fueled by decompression melting of the mantle; (2) a wet lineage leading to cold-oxidized rhyolites and granites in subduction zones dominated by flux melting of the mantle.
KEY WORDS: rhyolite; REE; differentiation; plutonic–volcanic connection; mush
| INTRODUCTION |
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The origin of rhyolites deserves much attention as they generate some of the largest volcanic eruptions on record (see issue of Elements on Supervolcanoes, February 2008). One possible mechanism to produce these high-viscosity, volatile-rich, but generally crystal-poor magmas is by extracting interstitial melt trapped within large, upper crustal mush zones (defined as as mixture of crystals and silicate liquid whose mobility is inhibited by a high fraction of solid particles Bachmann & Bergantz, 2004
50–60 vol. % crystals, Marsh, 1981
A potential geochemical test for this hypothesis is to compare the composition of aplites with high-silica rhyolites. Aplites are highly evolved, fine-grained dyke-like structures, commonly found within granitic bodies (sensu lato), which are thought to also form by interstitial melt extraction from highly crystalline silicic magmas (e.g. Jahns & Tuttle, 1963
; Miller & Mittlefehldt, 1984
; Hibbard & Watters, 1985
; Eichelberger et al., 2006
). This geochemical comparison between aplites and high-silica rhyolites was recently attempted by Glazner et al. (2008
), who reported significant differences in Sr, Y and rare earth element (REE) concentrations between them, and therefore challenged the hypothesis that voluminous high-silica rhyolites could be derived by melt extraction from large crystalline mushes of granodioritic composition.
The purpose of this paper is to re-examine the relationship between rhyolites, silicic plutons (granite sensu lato) and aplites from different tectonic settings (convergent margins, divergent margins, and hotspots, fueled by different mantle melting regimes). When integrating independent lines of evidence from geochemical, geophysical and field observations, we argue that rhyolites, silicic plutons and aplites have a clear genetic connection. This connection appears not to be restricted to any particular tectonic setting as co-magmatic silicic plutons, rhyolites, and aplites in a given magmatic province typically represent respectively the solidified mush zones, and the interstitial liquids extracted from them at different stages of evolution.
| TRACE ELEMENTS AND CRYSTAL RESIDUES |
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The Earth's magmatism can be roughly divided in two main trends on the basis of the dominant melting process in the mantle. In a convergent margin environment, mafic magmas (the primary drive of the Earth's magmatism; e.g. Hildreth, 1981
The difference in PH2O and fO2 that prevails in the source regions of the different tectonic settings leads to different mineral assemblages. For example, the stability of hydrous minerals, clinopyroxene and oxides is enhanced at the expense of plagioclase in subduction zones (e.g. Holloway & Burnham, 1972
; Gaetani et al., 1993
). Because the mineral assemblage present during magma evolution controls the concentrations of trace elements in igneous rocks (e.g. Rollinson, 1993
), silicic magmas produced in wet environments show significant differences in trace element concentrations from those in dry environments at comparable silica contents.
As pointed out by Christiansen (2005
) and Christiansen & McCurry (2008
), rhyolites can be divided in two categories: (1) the hot–dry–reduced rhyolites, occurring mostly above areas of mantle upwelling (hotspots and continental rifts); (2) the cold–wet–oxidized rhyolites, typically found in subduction zones. This observation appears robust despite the presence of hot–dry–reduced rhyolites in some subduction zones (e.g. Puyehue rhyolite, Gerlach et al., 1988
) and cold–wet–oxidized examples in extensional environments (e.g. Bishop Tuff; Hildreth, 1979
; even if the Bishop Tuff magma is not as oxidized as most arc rocks, e.g. Scaillet & Evans, 1999
). Both types of rhyolites have very similar major element concentrations, but show different trace element contents; in particular, for rare earth elements (REE, Fig. 1). In wet–oxidized environments, crystallization of amphibole and titanite, which sequester middle REE (MREE) and heavy REE (HREE) (+ Y) (Frey et al., 1978
; Hildreth, 1979
; Lipman, 1987
; Wones, 1989
; Bachmann et al., 2005
; Davidson et al., 2007a
; Glazner et al., 2008
), produces an increasingly pronounced U-shaped pattern with progressive differentiation. A deep Eu negative anomaly is not expected, because (1) plagioclase crystallization (which removes Eu and Sr from the melt) can be delayed in water-rich environments (e.g. Johannes & Holtz, 1996
), and (2) titanite and amphibole do not take up Eu as much as the other REE (lower partition coefficient for Eu than adjacent REE; e.g. Bachmann et al., 2005
). In contrast, the dry, reduced magmas crystallize abundant olivine, pyroxenes, and plagioclase, which do not host REE (except Eu in plagioclase). This assemblage produces REE patterns that show deep, negative Eu anomalies with otherwise fairly straight and distinctively high light REE (LREE) and HREE concentrations [the seagull pattern of Glazner et al. (2008
)].
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With the exception of garnet, phases other than amphibole, titanite and plagioclase are unlikely to play a major role in the shape of REE patterns. In highly evolved systems (>70 wt % SiO2), REE-rich mineral phases such as allanite, chevkenite, and monazite are common (e.g. Wolff & Storey, 1984
Rhyolites, silicic plutons, and aplites from similar tectonic environments have REE patterns that match those described above (seagull vs MREE–HREE depleted; Fig. 1). Most arc rhyolites [e.g. data from Andean rhyolites of Glazner et al. (2008, fig. 1c) and examples from the Aegean Arc, the Andes and the Taupo Volcanic zone (Fig. 1; see also supplementary data and figure, available for downloading at http//:www.petrology.oxfordjournals.org; Bryant et al., 2006
; Wilson et al., 2006
)] have lower MREE and HREE than high-silica rhyolites from hotspot systems and continental rifts. Conversely, REE patterns of aplites from titanite-free hosts (Glazner et al. 2008
, fig. 1d) and alkaline leuco-granite (e.g. Charoy & Raimbault, 1994
), are much more seagull-like, resembling the patterns of rhyolites from hotspots or continental rifts (e.g. Yellowstone, Coso, and Long Valley systems). Glazner et al. (2008
) did not reach this conclusion because their focus was on REE (and Sr, Y) concentrations in aplites from the Tuolumne Intrusive Suite, produced by a regional magmatic pulse related to Cretaceous subduction (Bateman & Chappell, 1979
), and they compared them with high-silica rhyolites from several magmatic centers not directly resulting from subduction processes [Yellowstone area, Coso volcanic field, SW Nevada volcanic field, Long Valley magmatic system (Glazner et al., 2008
, fig. 1b)], although all tectonic settings were compared in their fig. 1c.
Admittedly, some aplites do form more pronounced U-shaped patterns than even the wettest, coldest rhyolites, but this should be expected. Aplites are mostly generated very late in the evolution of large plutonic bodies and are commonly associated with pegmatites, as pointed out by Glazner et al (2008
) and several others [at least as far back as Jahns & Tuttle (1963
), including those in the Tuolumne Intrusive Suite, studied by Fournier (1968
)]. Aplites are typically mobilized after high-silica rhyolites, and therefore record more extreme differentiation patterns (particularly in REE) in water-rich and high-fO2 environments. Highly evolved cupolas in plutonic bodies (leuco-granites) present the same characteristics (i.e. U-shaped REE patterns; e.g. Lipman, 1987
; Bryant et al., 2006
). In addition, we expect a continuum of REE pattern between the two types of rhyolites; the wettest rhyolites from areas of mantle upwelling (e.g. Bishop Tuff) can have patterns that overlap with arc rhyolites (e.g. Glazner et al., 2008
, fig. 1b), and the driest arc-related rhyolites can have seagull-like patterns (e.g. Mitropolous & Tarney, 1992
).
| VOLATILES, MUSH TEMPERATURE AND ERUPTABILITY |
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Apart from the difference in REE patterns between rhyolites and aplites, other arguments have been raised against the mush extraction model for hot–dry rhyolites (e.g. Streck & Grunder, 2008
As for rhyolites, granites (sensu lato) have been categorized as hot–dry or cold–wet on the basis of geochemical arguments and zircon saturation temperatures (e.g. Clemens et al., 1986
; Frost & Frost, 1997
; King et al., 2001
; Miller et al., 2003
). Therefore, we propose that in hotspot systems and continental rifts, source mushes have hot–dry granitoïd compositions (e.g. Barbarin, 1990
; Frost & Frost, 1997
; Frost et al., 1999
; Edwards & Frost, 2000
; Schmitt et al., 2000
), leading to high-silica rhyolites such as those found in Yellowstone, Coso, and SW Nevada, whereas convergent margins have mushes of cold–wet granodioritic composition (which sometimes erupt as large crystal-rich ignimbrites called the Monotonous Intermediates; Lindsay et al., 2001
; Bachmann et al., 2002
; Maughan et al., 2002
; Bachmann et al., 2005
) and will lead to arc rhyolites (Bachmann et al., 2007a
; Hildreth, 2007
; Fig. 2).
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We concur that magmas with intermediate compositions between basalts and rhyolites, which could act as source mush zones for hot–dry–reduced rhyolites in hotspot systems and continental rifts (Streck & Grunder 2008
The paucity of erupted intermediate magmas is a likely consequence of the same fundamental difference that generates distinct types of REE patterns: abundance of volatiles in the magmatic crustal column. As demonstrated by the seminal work of Geist et al. (1995
) on rhyolites from Volcàn Alcedo (Galapagos Archipelago), evolved magmas are expected to be eruptible only after they become saturated with volatiles (either by progressive enrichment as a result of crystallization of anhydrous phases and/or addition from the surrounding crust). In both tectonic settings, basalts generally erupt from deep sources by processes independent of volatile saturation, but when these mafic magmas stall in the crust (triggering differentiation), the compositions of subsequently erupted magmas depends on the relative timing of volatile saturation and rheological lock-up, as follows.
In volatile-rich systems, under upper crustal conditions, volatile saturation is reached at intermediate compositions, increasing the likelihood that such compositions will be erupted (Fig. 3). Therefore, andesite–dacitic compositions dominate the volcanic record in subduction zones (e.g. Gill, 1981
). More evolved compositions (rhyolites) are rare in subduction zones (Hildreth, 2007
) because (1) their parental magmas (andesite or dacite) erupt, and (2) when they do form, rapid crystallization induced by volatile exsolution renders these volatile-laden systems generally too crystal-rich to erupt (Cashman & Blundy, 2000
; Miller et al., 2003
).
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In drier systems, rheological lock-up by cooling-induced crystallization is reached before volatile saturation for the intermediate compositions. Therefore, most alkaline andesites and dacites do not erupt. More differentiation is required for volatiles to accumulate and eruption to occur (Fig. 3), leading to the observed bimodal distribution of chemical compositions of erupted products in hotspots and continental rifts.
| DISTILLING RHYOLITES |
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Silicic magmas can form either by partial melting of metaigneous and metasedimentary supracrustal materials (see recent references e.g. Bindeman et al., 2008
Melting of pre-existing crustal rocks has been a popular hypothesis for decades, and has become the paradigm for generating silicic magmas following the recognition of restitic material (xenoliths and xenocrystic material) in most large silicic units (e.g. Friedman et al., 1974
; Worner et al., 1985
; Chappell et al., 1987
; Gunnarsson et al., 1998
; Charlier et al., 2007
; Bindeman et al., 2008
; Bryan et al., 2008
). In addition, unambiguous isotopic evidence for recycling of crustal material (e.g. Faure, 2001
; Davidson et al., 2007b
) indicates that silicic magmas are open to mass exchange with surrounding crust, and the presence in the rock record of peraluminous felsic rocks suggests that some evolved magmas may be pure partial melts of pelitic material (Munksgaard, 1984
; Pichavant et al., 1988
; Mahood et al., 1996
; Zeck & Williams, 2002
; Clarke et al., 2005
). Lastly, at least since the publication of the famous memoir by Tuttle & Bowen (1958
), crustal melting is thought to alleviate the heat and room problems associated with the emplacement of large bodies of silicic magmas in the mid- to upper crust.
However, modeling efforts to better constrain the heat budget in basalt–crust interaction (Barboza et al., 1999
; Babeyko et al., 2002
; Dufek & Bergantz, 2005
; Annen et al., 2006
) has led to different views, particularly for the large and abundant metaluminous units. State-of-the-art numerical simulations of the energy balance between mafic magmas and the pre-existing crust illustrate how difficult it is to form volumetrically significant amounts of pure crustal melts, even in the deep crust (Barboza et al., 1999
; Babeyko et al., 2002
; Dufek & Bergantz, 2005
; Annen et al., 2006
). A very high heat flow from the mantle is required (> 60 mW/m2; Babeyko et al., 2002
), and even in these hot conditions, only the lowermost crust can melt in any significant amounts (using the well-constrained melting behaviors of pelites and amphibolites; Barboza et al., 1999
; Babeyko et al., 2002
; Dufek & Bergantz, 2005
; Annen et al., 2006
). Even remelting young intrusive rocks requires large amounts of enthalpy and volatiles (Brown, 2007
). Heat and water that inevitably escape during solidification must be replenished by the incoming magmas (e.g. Miller et al., 2003
).
In addition to the numerical models of heat and mass transfer within the crust, field observations in exposed crustal sections (the natural laboratories) are also in disagreement with crustal melting being the dominant process in producing voluminous silicic magma bodies. Crustal sections, although sparse (Barboza & Bergantz, 2000
; Greene et al., 2006
; Jagoutz et al., 2007
; Hacker et al., 2008
), suggest that widespread crustal melting does not occur even when large pools of mafic melts intrude the lower to mid-crust (Barboza & Bergantz, 2000
). Careful investigations of these sections (Voshage et al., 1990
; Barboza et al., 1999
; Greene et al., 2006
; Jagoutz et al., 2007
) all conclude that fractional crystallization of mantle-derived basalts occurring synchronously with some assimilation (energy-constrained AFC; e.g. Reiners et al., 1995
; Bohrson & Spera, 2001
; Thompson et al., 2002
) is the dominant differentiation process.
We argue that, by analogy to basaltic lenses in mid-ocean ridges (e.g. Sinton & Detrick, 1992
), magmas feeding upper continental crust reservoirs are also generated by interstitial liquid extraction from crystalline mushes (Fig. 4; see also Wickham, 1987
; Quick et al., 1994
). The presence of crustal restitic material in silicic magmas (including xenocrysts) can be reconciled by partial assimilation of wall-rocks (both in the lower and upper crust; e.g. DePaolo, 1981
; DePaolo et al., 1992
; Bohrson & Spera, 2001
; Beard et al., 2004
, 2005), and does not necessarily require an origin by pure crustal melting. Most silicic magmas bodies unquestionably undergo open-system behavior and can blend components from both the mantle and the crust [many decades of references, at least since Daly (1914
) and Bowen (1928
)]. Energy-efficient reactive bulk assimilation has been recognized in both plutonic (Voshage et al., 1990
; Beard et al., 2004
, 2005) and volcanic (Charlier et al., 2007
) environments.
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| THE CHEMICALLY AND THERMALLY OPEN-SYSTEM MUSH MODEL AS THE EARTH'S WAY OF PRODUCING SILICIC MAGMAS |
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The varieties of physical processes that produce distinct trends of magmatic differentiation are rarely fully expressed through a single chemical index or line of evidence. The mush model discussed herein is based on specific and explicit links between plutons and volcanic systems, and much of the supporting evidence, including field relationships, temporal–compositional relationships and geophysical observations, has been summarized elsewhere (Bachmann & Bergantz, 2004
| SUPPLEMENTARY DATA |
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Supplementary data for this paper are available at Journal of Petrology online.
| ACKNOWLEDGEMENTS |
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We acknowledge the financial support of the Swiss National Science Foundation to O.B. and NSF EAR-0440391 and EAR-0711551 to G.W.B. Many thanks go to Calvin Miller, Jonathan Miller, Jim Beard, Denny Geist, and Peter Lipman for constructive comments on earlier versions of this manuscript, and to Bruce Marsh, Eric Christiansen and an anonymous reviewer for thoroughly assessing this work. The efficient editorial handling by Ron Frost is also gratefully acknowledged.
*Corresponding author. E-mail: bachmano{at}u.washington.edu
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