Hubbry Logo
SerpentinizationSerpentinizationMain
Open search
Serpentinization
Community hub
Serpentinization
logo
8 pages, 0 posts
0 subscribers
Be the first to start a discussion here.
Be the first to start a discussion here.
Serpentinization
Serpentinization
Serpentinization
View on Wikipedia
from Wikipedia

Chromitic serpentinite from Styria Province, Austria

Serpentinization is a hydration and metamorphic transformation of ferromagnesian minerals, such as olivine and pyroxene, in mafic and ultramafic rock to produce serpentinite.[1] Minerals formed by serpentinization include the serpentine group minerals (antigorite, lizardite, chrysotile), brucite, talc, Ni-Fe alloys, and magnetite.[1][2] The mineral alteration is particularly important at the sea floor at tectonic plate boundaries.[3][4]

Formation and petrology

[edit]
Serpentinite partially made of chrysotile, from Dobšiná, Slovakia

Serpentinization is a form of low-temperature (0 to ~600 °C) [5] metamorphism of ferromagnesian minerals in mafic and ultramafic rocks, such as dunite, harzburgite, or lherzolite. These are rocks low in silica and composed mostly of olivine ((Mg2+, Fe2+)2SiO4), pyroxene (XY(Si,Al)2O6), and chromite (approximately FeCr2O4). Serpentinization is driven largely by hydration and oxidation of olivine and pyroxene to serpentine group minerals (antigorite, lizardite, and chrysotile), brucite (Mg(OH)2), talc (Mg3Si4O10(OH)2), and magnetite (Fe3O4).[2] Under the unusual chemical conditions accompanying serpentinization, water is the oxidizing agent, and is itself reduced to hydrogen, H
2. This leads to further reactions that produce rare iron group native element minerals, such as awaruite (Ni
3Fe) and native iron; methane and other hydrocarbon compounds; and hydrogen sulfide.[1][6]

During serpentinization, large amounts of water are absorbed into the rock, increasing the volume, reducing the density and destroying the original structure.[7] The density changes from 3.3 to 2.5 g/cm3 (0.119 to 0.090 lb/cu in) with a concurrent volume increase on the order of 30-40%.[8] The reaction is highly exothermic, releasing up to 40 kilojoules (9.6 kcal) per mole of water reacting with the rock, and rock temperatures can be raised by about 260 °C (500 °F),[9][10] providing an energy source for formation of non-volcanic hydrothermal vents.[11] The hydrogen, methane, and hydrogen sulfide produced during serpentinization are released at these vents and provide energy sources for deep sea chemotroph microorganisms.[12][9]

Formation of serpentine minerals

[edit]

Olivine is a solid solution of forsterite, the magnesium endmember of (Mg2+, Fe2+)2SiO4, and fayalite, the iron endmember, with forsterite typically making up about 90% of the olivine in ultramafic rocks.[13] Serpentine can form from olivine via several reactions:

Reaction 1a tightly binds silica, lowering its chemical activity to the lowest values seen in common rocks of the Earth's crust.[14] Serpentinization then continues through the hydration of olivine to yield serpentine and brucite (Reaction 1b).[15] The mixture of brucite and serpentine formed by Reaction 1b has the lowest silica activity in the serpentinite, so that the brucite phase is very important in understanding serpentinization.[14] However, the brucite is often blended in with the serpentine such that it is difficult to identify except with X-ray diffraction, and it is easily altered under surface weathering conditions.[16]

A similar suite of reactions involves pyroxene-group minerals:

Reaction 2a quickly comes to a halt as silica becomes unavailable, and Reaction 2b takes over.[17] When olivine is abundant, silica activity drops low enough that talc begins to react with olivine:

This reaction requires higher temperatures than those at which brucite forms.[16]

The final mineralogy depends both on rock and fluid compositions, temperature, and pressure. Antigorite forms in reactions at temperatures that can exceed 600 °C (1,112 °F) during metamorphism, and it is the serpentine group mineral stable at the highest temperatures. Lizardite and chrysotile can form at low temperatures very near the Earth's surface.[18]

Breakdown of diopside and formation of rodingites

[edit]

Ultramafic rocks often contain calcium-rich pyroxene (diopside), which breaks down according to the reaction:

This raises both the pH, often to very high values, and the calcium content of the fluids involved in serpentinization. These fluids are highly reactive and may transport calcium and other elements into surrounding mafic rocks. Fluid reaction with these rocks may create metasomatic reaction zones enriched in calcium and depleted in silica, called rodingites.[19]

Formation of magnetite and hydrogen

[edit]
See also: Schikorr reaction

In most crustal rock, the chemical activity of oxygen is prevented from dropping to very low values by the fayalite-magnetite-quartz (FMQ) buffer.[20] The very low chemical activity of silica during serpentinization eliminates this buffer, creating highly reducing conditions[14] that allow water to oxidize ferrous (Fe2+
) ions in fayalite. This reaction modifies minerals and liberates hydrogen gas:[1][21][22]

Studies of serpentinites suggest that in nature iron minerals are first converted to ferroan brucite, that is, brucite containing Fe(OH)2,[23] which then undergoes the Schikorr reaction in the anaerobic conditions of serpentinization:[24][25]

Maximum reducing conditions, and the maximum rate of production of hydrogen, occur when the temperature of serpentinization is between 200 and 315 °C (392 and 599 °F)[26] and when fluids are carbonate undersaturated.[1] If the original ultramafic rock (the protolith) is peridotite, which is rich in olivine, considerable magnetite and hydrogen are produced. When the protolith is pyroxenite, which contains more pyroxene than olivine, iron-rich talc is produced with no magnetite and only modest hydrogen production. Infiltration of silica-bearing fluids during serpentinization can suppress both the formation of brucite and the subsequent production of hydrogen.[27]

Chromite present in the protolith will be altered to chromium-rich magnetite at lower serpentinization temperatures. At higher temperatures, it will be altered to iron-rich chromite (ferrit-chromite).[28] During serpentinization, the rock is enriched in chlorine, boron, fluorine, and sulfur. Sulfur will be reduced to hydrogen sulfide and sulfide minerals, though significant quantities are incorporated into serpentine minerals, and some may later be reoxidized to sulfate minerals such as anhydrite.[29] The sulfides produced include nickel-rich sulfides, such as mackinawite.[30]

Methane and other hydrocarbons

[edit]

Laboratory experiments have confirmed that at a temperature of 300 °C (572 °F) and pressure of 500 bars, olivine serpentinizes with release of hydrogen gas. In addition, methane and complex hydrocarbons are formed through reduction of carbon dioxide. The process may be catalyzed by magnetite formed during serpentinization.[6] One reaction pathway is:[24]

Metamorphism at higher pressure and temperature

[edit]

Lizardite and chrysotile are stable at low temperatures and pressures, while antigorite is stable at higher temperatures and pressure.[31] Its presence in a serpentinite indicates either that serpentinization took place at unusually high pressure and temperature or that the rock experienced higher grade metamorphism after serpentinization was complete.[2]

Infiltration of CO2-bearing fluids into serpentinite causes distinctive talc-carbonate alteration.[32] Brucite rapidly converts to magnesite and serpentine minerals (other than antigorite) are converted to talc. The presence of pseudomorphs of the original serpentinite minerals shows that this alteration takes place after serpentinization.[2]

Serpentinite may contain chlorite (a phyllosilicate mineral), tremolite (Ca2(Mg5.0-4.5Fe2+0.0-0.5)Si8O22(OH)2), and metamorphic olivine and diopside (calcium-rich pyroxene). This indicates that the serpentinite has been subject to more intense metamorphism, reaching the upper greenschist or amphibolite metamorphic facies.[2]

Above about 450 °C (842 °F), antigorite begins to break down. Thus serpentinite does not exist at higher metamorphic facies.[12]

Extraterrestrial production of methane by serpentinization

[edit]

The presence of traces of methane in the atmosphere of Mars has been hypothesized to be a possible evidence for life on Mars if methane was produced by bacterial activity. Serpentinization has been proposed as an alternative non-biological source for the observed methane traces.[33][34] In 2022 it was reported that microscopic examination of the ALH 84001 meteorite, which came from Mars, shows that indeed the organic matter it contains was formed by serpentinization, not by life processes.[35][36]

Using data from the Cassini probe flybys obtained in 2010–12, scientists were able to confirm that Saturn's moon Enceladus likely has a liquid water ocean beneath its frozen surface. A model suggests that the ocean on Enceladus has an alkaline pH of 11–12.[37] The high pH is interpreted to be a key consequence of serpentinization of chondritic rock, that leads to the generation of H
2, a geochemical source of energy that can support both abiotic and biological synthesis of organic molecules.[37][38]

Environment of formation

[edit]
Ophiolite of the Gros Morne National Park, Newfoundland. Ophiolites characteristically have a serpentinite component.

Serpentinization occurs at mid-ocean ridges, in the forearc mantle of subduction zones, in ophiolite packages, and in ultramafic intrusions. [3][4]

Mid-ocean ridges

[edit]

Conditions are highly favorable for serpentinization at slow to ultraslow spreading mid-ocean ridges.[8] Here the rate of crustal extension is high compared with the volume of magmatism, bringing ultramafic mantle rock very close to the surface where fracturing allows seawater to infiltrate the rock.[11]

Serpentinization at slow spreading mid-ocean ridges can cause the seismic Moho discontinuity to be placed at the serpentinization front, rather than the base of the crust as defined by normal petrological criteria.[39][8] The Lanzo Massif of the Italian Alps shows a sharp serpentinization front that may be a relict seismic Moho.[40]

Subduction Zones

[edit]

Forearc mantle

[edit]

Serpentinization is an important phenomenon in subduction zones that has a strong control on the water cycle and geodynamics of a subduction zone. [41] Here mantle rock is cooled by the subducting slab to temperatures at which serpentinite is stable, and fluids are released from the subducting slab in great quantities into the ultramafic mantle rock.[41] Direct evidence that serpentinization is taking place in the Mariana Islands island arc is provided by the activity of serpentinite mud volcanoes. Xenoliths of harzburgite and (less commonly) dunite are occasionally erupted by the mud volcanoes, giving clues to the nature of the protolith.[42]

Because serpentinization lowers the density of the original rock, serpentinization may lead to uplift or exhumation of serpentinites to the surface, as has taken place with the serpentinite exposed at the Presidio of San Francisco following cessation of subduction.[43]

Serpentinized ultramafic rock is found in many ophiolites. Ophiolites are fragments of oceanic lithosphere that has been thrust onto continents, a process called obduction. [44] They typically consist of a layer of serpentinized harzburgite (sometimes called alpine peridotite in older writings), a layer of hydrothermally altered diabases and pillow basalts, and a layer of deep water sediments containing radiolarian ribbon chert.[45]

Hydration of forearc mantle due to the water expelled from deeper part of the subducting plate. Adapted from Hyndman and Peacock (2003)

Implications

[edit]

Limitation on earthquake depth

[edit]

Seismic wave studies can detect the presence of large bodies of serpentinite in the crust and upper mantle, since serpentinization has a huge impact on shear wave velocity. A higher degree of serpentinization will lead to lower shear wave velocity and higher Poisson's ratio.[46] Seismic measurements confirm that serpentinization is pervasive in forearc mantle.[47] The serpentinization can produce an inverted Moho discontinuity, in which seismic velocity abruptly decreases across the crust-mantle boundary, which is the opposite of the usual behavior. The serpentinite is highly deformable, creating an aseismic zone in the forearc, at which serpentinites slide at stable plate velocity. The presence of serpentinite may limit the maximum depth of megathrust earthquakes as they impede rupture into the forearc mantle.[46]

See also

[edit]

References

[edit]
[edit]
Revisions and contributorsEdit on WikipediaRead on Wikipedia

Serpentinization

View on Grokipedia
from Grokipedia
Serpentinization is a geochemical process involving the hydration and metamorphic alteration of ultramafic rocks, primarily composed of and , when they react with under low-temperature conditions (typically below 400°C), resulting in the formation of serpentine minerals (such as , , and ), , , and molecular (H₂). This oxidizes iron (Fe²⁺) in the primary minerals while reducing , producing H₂ as a key byproduct through reactions like 3Fe₂SiO₄ + 2H₂O → 2Fe₃O₄ + 3SiO₂ + 2H₂. The process significantly increases the rock's volume by up to 50%, leading to fracturing that facilitates further fluid infiltration and reaction progression. Serpentinization predominantly occurs in tectonic settings such as mid-ocean ridges, zone forearcs, and continental margins, where ultramafic mantle rocks are exposed to circulating aqueous fluids in hydrothermal systems. On , it has been active since the planet's early , potentially as far back as 4.2 billion years ago, and continues today at sites like the in the Atlantic Ocean. The reaction also generates reduced compounds like (CH₄) and through subsequent interactions with CO₂, influencing global geochemical cycles of elements such as carbon, , and fluid-mobile trace elements. Beyond , serpentinization plays a critical role in by providing energy sources (H₂) and catalysts (, awaruite) for prebiotic chemistry and , as seen in H₂-dependent pathways like the pathway. It alters the lithosphere's rheological, magnetic, and seismic properties, affecting dynamics and generation, and has implications for resources formed deep within the . Analogous processes are hypothesized on celestial bodies like Mars, Europa, and , where they may drive subsurface and .

Definition and Fundamentals

Overview of the Process

Serpentinization is a metamorphic hydration process involving the aqueous alteration of ferromagnesian minerals, primarily and , in ultramafic rocks, transforming them into serpentine-group minerals (such as , , and ), , and . This reaction fundamentally alters the and physical properties of the host rock, resulting in the formation of , a distinctive rock type characterized by its green color and fibrous textures. The process has been recognized since the through studies of Alpine ophiolites, where mineralogists first documented the pseudomorphic replacement textures indicative of hydration in ultramafic protoliths. The fundamental prerequisites for serpentinization include ultramafic protoliths like , rich in and , and the availability of aqueous fluids to drive the hydration.

Chemical Composition and Mineralogy

Serpentinization primarily affects ultramafic rocks, such as , which are mantle-derived igneous rocks dominated by ferromagnesian silicates. These rocks typically contain 40–90% with the general formula (Mg,Fe)2SiO4(\mathrm{Mg,Fe})_2\mathrm{SiO}_4, along with orthopyroxene (, MgSiO3\mathrm{MgSiO}_3) comprising 10–40% and clinopyroxene (, CaMgSi2O6\mathrm{CaMgSi}_2\mathrm{O}_6) making up 0–10%, depending on the subtype like or . Dunites represent the olivine end-member with over 90% , while feature higher orthopyroxene proportions. The primary mineralogical products of serpentinization are serpentine-group minerals, which form through hydration of the original silicates and adopt the ideal formula (Mg,Fe)3Si2O5(OH)4(\mathrm{Mg,Fe})_3\mathrm{Si}_2\mathrm{O}_5(\mathrm{OH})_4. These occur as three main polymorphs: , the low-temperature, fine-grained variety that dominates early alteration; , a fibrous form often found in veins; and , a platy, high-temperature polymorph stable under metamorphic conditions. , with composition Mg(OH)2\mathrm{Mg(OH)}_2 (or more precisely (Mg,Fe)(OH)2(\mathrm{Mg,Fe})(\mathrm{OH})_2), precipitates in Mg-rich systems, particularly from hydration, while (Mg3Si4O10(OH)2\mathrm{Mg}_3\mathrm{Si}_4\mathrm{O}_{10}(\mathrm{OH})_2) forms in pyroxene-bearing rocks where silica activity is higher. These minerals collectively replace the , often comprising over 90% of the resulting . Accessory minerals include magnetite (Fe3O4\mathrm{Fe}_3\mathrm{O}_4), which nucleates as disseminated grains or along fractures, and awaruite, a nickel-iron alloy (FeNi3\mathrm{FeNi}_3) that indicates highly reducing conditions during alteration. Sulfides such as pyrrhotite (Fe1−xS\mathrm{Fe}_{1-x}\mathrm{S}) and pentlandite also occur, derived from primary monosulfide solid solution in the mantle rocks and preserved or remobilized during fluid-rock interaction. Characteristic textures in serpentinites reflect the replacement process, with pseudomorphic mesh structures forming around relict grains, where serpentine rims enclose central cores of or residual . textures develop as a variant, featuring serpentine-filled hourglass-shaped voids in place of , often in more advanced alteration stages. Vein networks, filled with or fibers, indicate fluid infiltration pathways and crosscut the pseudomorphic fabrics. Compositional changes during serpentinization involve incorporation of , leading to a significant increase in H₂O content (up to 13 wt% in fully serpentinized rocks) and SiO₂ content that remains largely unchanged relative to the due to hydration without substantial silica loss. Iron oxidation states shift from dominantly Fe²⁺ in primary and pyroxenes to Fe³⁺ in and , facilitating the reducing environment essential for accessory phase formation.

Mechanisms and Reactions

Primary Hydration Reactions

Serpentinization primarily involves the hydration of ferromagnesian silicates in ultramafic rocks, with serving as the dominant reactant in most settings. The core reaction for Mg-rich (forsterite) is given by the equation: 2Mg2SiO4+3H2O→Mg3Si2O5(OH)4+Mg(OH)22 \mathrm{Mg_2SiO_4} + 3 \mathrm{H_2O} \rightarrow \mathrm{Mg_3Si_2O_5(OH)_4} + \mathrm{Mg(OH)_2} This produces , a serpentine polymorph, and , with a requiring 1.5 moles of per mole of . In Fe-bearing variants, such as ferroan , the reaction incorporates iron into the products, maintaining similar hydration proportions but influencing subsequent redox processes. Reactions often proceed incompletely, leaving residual cores within serpentine rims due to kinetic barriers and silica undersaturation in the fluid. Pyroxenes contribute to serpentinization through coupled reactions that typically require brucite derived from prior olivine hydration. For orthopyroxene (enstatite), the simplified reaction is: 2MgSiO3+Mg(OH)2→Mg3Si2O5(OH)42 \mathrm{MgSiO_3} + \mathrm{Mg(OH)_2} \rightarrow \mathrm{Mg_3Si_2O_5(OH)_4} This incorporates dissolved silica to form serpentine without net water consumption in the step itself. Clinopyroxene (diopside) undergoes breakdown via the simplified reaction: CaMgSi2O6+2Mg(OH)2→Mg3Si2O5(OH)4+Ca(OH)2\mathrm{CaMgSi_2O_6} + 2 \mathrm{Mg(OH)_2} \rightarrow \mathrm{Mg_3Si_2O_5(OH)_4} + \mathrm{Ca(OH)_2} yielding chrysotile serpentine and portlandite, which facilitates calcium mobility in the system. These pyroxene reactions generally occur after initial olivine alteration, promoting a sequential progression in mesh and hourglass textures observed in serpentinites. The process demands interaction with aqueous fluids, typically in oceanic settings or in continental environments, at low temperatures to initiate hydration. Fluid-rock ratios influence reaction extent, with low ratios favoring isochemical conditions and higher fluxes enhancing silica activity for progressive alteration. As reactions advance, the fluid evolves from near-neutral to strongly alkaline ( 9-11) due to proton consumption and release from formation. Laboratory simulations confirm these pathways, demonstrating reaction rates for olivine serpentinization on the order of 10^{-12} to 10^{-14} mol m^{-2} s^{-1} at 200-300°C and pressures around 500 bar, with water activity modulating kinetics—lower activity slows rates by up to two orders of magnitude. These experiments, using San Carlos olivine in NaCl-MgCl_2 solutions mimicking seawater, replicate natural mesh textures and validate the stoichiometric water consumption of approximately 1.5-2 moles per mole of olivine under controlled hydrothermal conditions.

Formation of Accessory Minerals and Rodingites

During serpentinization, incompatible elements and calcium mobilized from the hydration of primary silicates in rocks lead to the formation of secondary accessory minerals, particularly in rodingites. Rodingites originate as Ca-rich metasomatic rocks formed through the interaction of gabbroic veins or dikes within hosts, where clinopyroxene () breakdown releases Ca that is transported by alkaline, hydrous fluids. This process enriches the altered zones in CaO while depleting SiO₂, Na₂O, and K₂O, resulting in mineral assemblages dominated by (Ca₃Al₂Si₃O₁₂), (Ca₂Al₂Si₃O₁₀(OH)₂), and pumpellyite ((Ca,Mg,Fe)₄(Al,Fe)₅(SiO₄)₅(Si₂O₇)₂(OH,O)₂·2-4H₂O). These minerals precipitate as the fluids, buffered by low-silica serpentinization reactions, infiltrate and alter the protoliths at temperatures of 180–320 °C and pressures of 2–5 kbar. The formation of rodingites involves SiO₂ depletion in the surrounding serpentinite, which lowers silica activity and promotes the development of Ca-Si metasomatic halos around the altered bodies. These halos manifest as reaction zones with minerals like , , and , where SiO₂ is consumed, leading to the replacement of primary phases such as . Rodingites often appear as resistant, leucocratic nodules or boudins within ophiolitic , preserving relict from their gabbroic or basaltic origins despite the intense . Beyond rodingites, other accessory minerals form from the redistribution of elements during serpentinization. Chlorite (e.g., clinochlore, Mg₅Al(AlSi₃O₁₀)(OH)₈) arises from the alteration of amphibole in mafic-ultramafic contact zones, where Al- and Fe-rich fluids facilitate its precipitation as fan-shaped aggregates or vein fillings. Iowaite (Mg6Fe23+(OH)16Cl2⋅4H2O\mathrm{Mg_6Fe^{3+}_2(OH)_{16}Cl_2 \cdot 4H_2O}), a rare hydroxychloride, forms in Fe-rich fluid environments, often rimming olivine remnants in serpentinized dunites and exhibiting higher birefringence than brucite. Petrologically, these accessory minerals and rodingites develop primarily at contacts between (e.g., ) and ultramafic (e.g., ) rocks, where fluid flow is focused along fractures or shear zones. This setting allows for the preservation of original igneous fabrics, such as plagioclase coronas, while the creates sharp boundaries with the host . Classic examples include rodingites in the Val d'Ala area of the Italian Alps, featuring Ca-rich garnets and in ophiolitic mélanges, and those in the Coast Range , where hydrothermally altered blocks exhibit similar Ca-enrichment signatures.

Production of Hydrogen, Magnetite, and Hydrocarbons

During serpentinization, (Fe₃O₄) forms through the oxidation of ferrous iron (Fe²⁺) primarily sourced from , a key process that alters the geochemical environment of ultramafic rocks. A simplified representation of this reaction for iron-rich ( endmember) is: 3Fe2SiO4+2H2O→2Fe3O4+3SiO2+2H23 \text{Fe}_2\text{SiO}_4 + 2 \text{H}_2\text{O} \rightarrow 2 \text{Fe}_3\text{O}_4 + 3 \text{SiO}_2 + 2 \text{H}_2 This oxidation couples hydration with the release of hydrogen gas (H₂), where Fe²⁺ is oxidized to Fe³⁺ in , reducing water to H₂. The resulting often occurs as nanoscale grains, typically 10-50 nm in size, which are disseminated within serpentine matrices and contribute to the magnetic signature of serpentinites. Hydrogen production is a direct byproduct of this magnetite-forming reaction, with estimates ranging from 0.1 to 0.3 mol H₂ per kg of rock during progressive serpentinization, depending on the iron content of the parent minerals and degree of alteration. This H₂ acts as a potent reductant, enabling abiotic synthesis of organic compounds through reactions such as Fischer-Tropsch-type (FTT) processes, where H₂ reduces dissolved CO₂ or inorganic carbon to (CH₄) and higher hydrocarbons. In these systems, awaruite (Ni₃Fe), a native nickel-iron formed under highly reducing conditions, serves as an additional and reductant, enhancing the of carbon reduction. Hydrocarbon generation proceeds via multiple pathways, including the direct FTT reaction CO₂ + 4H₂ → CH₄ + 2H₂O, which favors CH₄ formation at temperatures below 150°C under alkaline conditions prevalent in serpentinizing fluids. An alternative route involves the intermediate formation of (HCOOH) through H₂ + CO₂ → HCOOH, catalyzed by or awaruite, followed by further reduction to CH₄ and traces of higher alkanes (C₂-C₄). These processes yield low concentrations of hydrocarbons, with CH₄ dominating and minor amounts of , , and detected in fluids, reflecting the reducing power of serpentinization-derived H₂. Field evidence from the , an active serpentinization site on the , demonstrates these processes in action, with vent fluids containing up to 15 mM dissolved H₂, supporting elevated CH₄ levels (up to 1-2 mM). Laboratory simulations replicate this, producing H₂ and CH₄ from olivine hydration under hydrothermal conditions mimicking oceanic settings. Recent isotopic analyses further confirm the abiotic origin of CH₄ in serpentinized systems; for instance, δ¹³C values of -30.9‰ to -28.6‰ and δD values of -383‰ to -363‰ in fluid inclusions from subduction-related eclogites align with equilibrium fractionation models for inorganic carbon reduction, excluding biotic signatures. These findings underscore the role of serpentinization in generating reduced volatiles with significant geochemical implications for carbon cycling.

Metamorphic and Thermal Aspects

Conditions of Pressure and Temperature

Serpentinization primarily occurs under low to moderate pressure conditions, ranging from 0.1 to 1 GPa, which correspond to shallow crustal depths of approximately 1 to 10 km. These pressures facilitate the hydration of ultramafic rocks without exceeding the stability limits of serpentine minerals, though higher pressures up to 6 GPa can support antigorite stability in subduction-related settings. Experimental studies demonstrate that increasing pressure from 0.3 to 2 GPa at temperatures of 400–500°C significantly enhances reaction kinetics, achieving up to 19% serpentinization extent in just 20 days at the higher end. Recent 2023 investigations into high-pressure behavior confirm that slab serpentinization remains viable up to 6 GPa and 600°C, with antigorite controlling the process in deep environments. The temperature range for serpentinization spans 0 to 500°C, with optimal conditions peaking between 200 and 400°C where reaction rates are most efficient. Below 100°C, kinetics are notably slow, limiting the extent of hydration, whereas rates become rapid at around 300°C, enabling substantial transformation in hydrothermal systems. Different serpentine polymorphs exhibit distinct stability: forms and remains stable below 300°C, while persists up to 600°C, particularly under elevated pressures. Fluid involvement is critical, requiring high (a_w > 0.8) to drive the hydration reactions effectively. Serpentinization can proceed in either isochemical systems, where the rock composition changes minimally beyond addition, or open-system , involving influx that alters element budgets such as silica and magnesium. Phase diagrams illustrate the stability fields of polymorphs, with and dominating low-pressure, low-temperature domains, transitioning to at higher pressures and temperatures. Above 500°C, destabilizes, leading to assemblages like talc-schist through and silica enrichment. These boundaries are influenced by bulk composition and chemistry, as confirmed by thermodynamic modeling and experimental calibration.

Exothermic Effects and Volume Changes

Serpentinization reactions are highly exothermic, with the hydration of and releasing approximately 40 kJ per mole of water incorporated into the lattice. This release arises primarily from the formation of strong Si-O and Mg-O bonds in minerals, as calculated from standard enthalpies of formation for reactions such as 3Mg₂SiO₄ + SiO₂ + 4H₂O → 2Mg₃Si₂O₅(OH)₄, yielding a ΔH of -180 kJ per mole of reaction (or ~45 kJ/mol H₂O). In confined or low-permeability environments, this localized heating can raise rock temperatures by up to 300°C for complete serpentinization under adiabatic conditions, though actual increases are moderated by heat dissipation through fluid flow. In hydrothermal systems like Lost City, the exothermic heat contributes to fluid temperatures reaching 40–90°C, sustaining circulation and altering the thermal structure of the . The incorporation of during serpentinization induces significant solid volume expansion of 30–50%, transforming the dense ferromagnesian minerals into lower-density hydrous phases. This expansion accompanies a substantial reduction, from approximately 3.3 g/cm³ in unaltered to 2.6 g/cm³ in fully serpentinized rock, reflecting the addition of ~12 wt% structural . The resulting volumetric strain generates internal stresses that propagate fractures, enhancing rock permeability by orders of magnitude and facilitating ongoing ingress essential for progressive alteration. Mechanically, the volume expansion leads to stress accumulation within the host rock, promoting cataclastic deformation and the development of extensional veins infilled with serpentine and . These veins often form perpendicular to the principal stress direction, as observed in oceanic peridotites where hydration-induced cracking creates networks that accommodate the ~50% solid volume increase without complete sealing. Such processes weaken the lithosphere, influencing faulting and potentially contributing to tectonic deformation at plate boundaries. Globally, serpentinization contributes a on the order of 10¹² , comparable in scale to portions of the radiogenic budget and playing a key role in oceanic and continental geodynamics. Numerical simulations coupling reaction kinetics, transport, and have elucidated these thermomechanical effects, demonstrating how exothermic heating and expansion drive propagation. Recent models incorporate phase-field approaches to simulate reaction-induced cracking, predicting pulses and sustained permeability during progressive serpentinization.

Geological Settings

Mid-Ocean Ridge Environments

Serpentinization predominantly occurs in environments at divergent plate boundaries, where abyssal peridotites from the are exposed to through tectonic processes. At slow- to ultraslow-spreading ridges, such as the , detachment faulting exhumes mantle-derived peridotites, allowing pervasive fluid-rock interactions. These peridotites, primarily harzburgites and dunites, undergo hydration as penetrates fractures formed during exhumation, leading to the formation of serpentine minerals like and . The process involves seawater infiltration at temperatures of 200–400°C, driven by the exothermic hydration of and pyroxenes, which generates hydrogen-rich fluids. In these settings, serpentinization fosters unique hydrothermal systems, exemplified by the on the at 30°N on the , where alkaline fluids (pH 9–11) precipitate tall chimneys up to 60 m high. These systems differ from typical basalt-hosted black smokers by their lower temperatures (40–90°C at vents) and reactions involving dissolved CO₂. Global from these reactions is estimated at 10¹⁰–10¹² mol/yr, indicating substantial fluid fluxes. At sites like the , recovered serpentinized harzburgites exhibit 50–80% alteration, with mesh textures and magnetite veins documenting progressive hydration. Recent analyses of drill cores from Hess Deep along the (IODP Expedition 345 samples re-evaluated in 2024) reveal alteration gradients, showing initial low-temperature (<200°C) formation transitioning to higher-temperature in deeper sections.

Subduction Zone Settings

In subduction zones, primarily occurs in the mantle wedge, where hydration of by water-rich fluids released from the subducting slab drives the formation of serpentine minerals such as and . These fluids, derived from reactions during of the downgoing and sediments, migrate upward through fractures and porous media, reacting with the overlying ultramafic mantle at depths typically ranging from 10 to 20 km. This process is facilitated by the compressional tectonic regime, which promotes fluid channeling along faults, and results in significant water incorporation into the mantle, altering its and influencing fluid budgets in convergent margins. Temperature conditions in the vary with proximity to the : in the outer forearc, cool thermal regimes below 200–300°C favor the formation of low-temperature polymorphs like , while deeper zones within the wedge support stability up to approximately 600°C. This thermal gradient reflects the cooling effect of the subducting slab, which maintains low geothermal gradients (around 20–50°C/km) in the forearc, enabling serpentinization to persist without . The extent of hydration can reach 20–40% in many zones, controlling fluid flux and potentially contributing to volume expansion that affects local stress fields. Prominent examples include the Mariana , where serpentinized harzburgites and dunites have been recovered from Conical via Ocean Drilling Program Leg 125, revealing up to 80 km landward of the trench axis and indicating fluid-mediated elemental exchange between slab and mantle. In this setting, mud volcanoes rise up to 2.5 km above the seafloor, expelling hydrated material and providing direct samples of forearc processes. Similarly, the Cascadia margin exhibits widespread forearc serpentinization, inferred from low seismic velocities and high Vp/Vs ratios indicating 30–50% hydration, with fluid expulsion at cold seeps and mud volcanoes potentially involving serpentinized components from the . Recent seismic imaging in the Sumatra-Andaman zone has revealed low Pn velocities (~7.8 km/s) and trench-parallel in the western , signifying a hydrated mantle wedge influenced by slab fluids.

Continental Margin Environments

Serpentinization also occurs at continental margins, particularly in magma-poor rifted margins where hyperextended crust exposes mantle peridotites to infiltration during continental breakup. These settings, analogous to ultraslow-spreading mid-ocean ridges, feature detachment faulting that exhumes and hydrates ultramafic rocks, producing serpentine minerals, , and . Examples include the West Iberia Margin and the , where drilled peridotites show 50–100% serpentinization degrees and associated hydrothermal alteration. This process contributes to (potentially 10^9–10^10 mol/yr globally from rifted margins) and may facilitate abiotic formation through fluid-rock interactions.

Broader Implications

Seismological and Tectonic Effects

Serpentinization significantly alters the of fault zones by reducing the frictional strength of minerals, with steady-state friction coefficients typically ranging from 0.3 to 0.6, depending on the serpentine polymorph and shear conditions. This weakening promotes aseismic slip, as evidenced by experiments showing velocity-weakening behavior and low healing rates in serpentinized gouges, which facilitate slow earthquakes and creep rather than dynamic rupture. In transform and fault settings, these properties enable stable sliding, reducing the potential for seismic energy release. The process contributes to limiting the downdip extent of megathrust seismogenic zones, often capping ruptures at depths around 40 km due to the weakening of wedge interface by serpentinization. For instance, in the 2011 Tohoku-Oki , while the rupture extended deeper than typical (up to 50-55 km), the general transition to velocity-strengthening behavior in serpentinized antigorite-dominated zones acts as a barrier to further propagation. Recent models indicate that slab influences this limit by controlling the extent of re-serpentinization, with dewatering reactions reducing fault strength downdip. Serpentinization plays a key role in by facilitating initiation through hydration-induced weakening of the , allowing passive ingress of oceanic plates. The associated volume expansion, up to 50-60% during hydration, drives normal faulting and crustal fracturing at mid-ocean ridges, enhancing permeability and exhumation of mantle peridotites. Seismically, serpentinized zones exhibit distinctive signatures, including elevated Vp/Vs ratios (1.8-2.0) due to reduced shear wave velocities in hydrated peridotites, and pronounced (up to 20-30% in Vs) from aligned fibers oriented by shear deformation. These features are imaged in mantle wedges, where low velocities and high Poisson's ratios indicate 20-100% serpentinization. Case studies highlight these effects: along the , talc-bearing serpentinites in the creeping section provide lubrication via low-friction minerals (μ ≈ 0.1-0.3), promoting aseismic strike-slip motion over 30-50 km segments. In zones, 2025 numerical models of slab dehydration demonstrate how fluid release from antigorite breakdown re-serpentinizes the interface, modulating rupture barriers and distributions.

Astrobiological and Extraterrestrial Relevance

Serpentinization plays a pivotal role in on Earth by generating (H₂) and (CH₄) that serve as sources for hyperthermophilic microbes in alkaline hydrothermal environments. At the in the , abiotic H₂ and CH₄ produced via serpentinization of ultramafic rocks support methanogenic , including Methanopyrus kandleri, which thrive at temperatures up to 122°C and utilize these reductants for hydrogenotrophic . This process creates chemosynthetic ecosystems analogous to those potentially sustaining life in subsurface or extreme settings, highlighting serpentinization's capacity to drive without . The Russell hypothesis posits that alkaline vents formed by serpentinization were key sites for the origin of life in the ocean, providing natural proton gradients, H₂ as a reductant, and compartments for prebiotic chemistry. Developed in the , this theory emphasizes how serpentinization reactions between ultramafic rocks and generate alkaline fluids (pH ~9–11) rich in H₂, , and minor organics, enabling the synthesis of simple biomolecules like and pyruvate from CO₂ without enzymes. Experimental analogs simulating these vents have demonstrated H₂-driven reduction of CO₂ to prebiotic compounds, supporting the idea that such disequilibria could have powered early autocatalytic networks. On Mars, evidence of serpentinization includes hydrated olivine in Nili Fossae, detected via orbital spectroscopy, indicating past aqueous alteration of ultramafic minerals that could have produced H₂ and CH₄. The Curiosity rover detected transient CH₄ spikes in Gale Crater in 2019, reaching ~21 parts per billion, potentially abiotically sourced from subsurface serpentinization of olivine-rich crust, though seasonal and geological origins remain debated. Analysis of the ALH 84001 meteorite reveals carbonates and organics formed via serpentinization and carbonation ~4 billion years ago, with nanoscale imaging showing abiotic synthesis of complex refractory organic matter in a low-temperature hydrothermal setting, underscoring Mars' ancient habitability potential. For , Cassini spacecraft data from 2015 indicate a subsurface ocean with 11–12, inferred from Na⁺-rich, carbonate-bearing plumes consistent with serpentinization of a rocky core. Molecular H₂ detected in these plumes (up to 1% mole fraction) points to ongoing hydrothermal serpentinization, providing reductant to power by under Enceladus-like conditions (90°C, 11, high ), as demonstrated in cultures of Methanothermococcus okinawensis. Serpentinization's extraterrestrial relevance extends to other icy moons, where it may sustain subsurface . On Europa, modeling suggests potential H₂ production from serpentinization of iron-rich silicates in the rocky mantle, balancing oxidants from surface to yield energy for microbial life in the ocean. For Titan, ancient or ongoing serpentinization at the base of its water-ammonia ocean could contribute to atmospheric hydrocarbons, including that photochemically forms the layer, though photolysis dominates current production. Experimental analogs continue to explore these processes for prebiotic chemistry, while the (JWST), operational since 2022, offers prospects for detecting serpentinization signatures in exomoon atmospheres through of H₂ or CH₄ emissions, potentially identifying habitable analogs around exoplanets by late 2025.

References

  1. https://www.nature.com/articles/ncomms16107
  2. https://www.mdpi.com/2075-1729/8/4/41
  3. https://pubs.geoscienceworld.org/gsa/geology/article/48/6/552/583188/Quantifying-the-volume-increase-and-chemical
  4. https://pmc.ncbi.nlm.nih.gov/articles/PMC4523005/
  5. https://www.usgs.gov/faqs/how-geologic-hydrogen-formed
  6. https://pubs.geoscienceworld.org/msa/elements/article/9/2/95/137949/Serpentinites-Essential-Roles-in-Geodynamics-Arc
  7. https://www-odp.tamu.edu/publications/103_SR/VOLUME/CHAPTERS/sr103_12.pdf
  8. https://www.alexstrekeisen.it/english/pluto/peridotites.php
  9. https://www.pnas.org/doi/10.1073/pnas.0405289101
  10. https://www.sciencedirect.com/science/article/pii/002449377690030X
  11. https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2021GC009989
  12. https://pubs.geoscienceworld.org/gsa/books/edited-volume/2118/chapter/116181966/Serpentinization-related-nickel-iron-and-cobalt
  13. https://rruff.geo.arizona.edu/doclib/cm/vol15/CM15_459.pdf
  14. https://rruff.info/doclib/cm/vol30/CM30_1113.pdf
  15. https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2004GC000744
  16. https://website.whoi.edu/gfd/wp-content/uploads/sites/14/2018/10/Klein_et_al_2009_58566.pdf
  17. https://www.sciencedirect.com/science/article/abs/pii/S0016703713003311
  18. https://academic.oup.com/petrology/article/48/7/1351/1531832
  19. https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2006GL025681
  20. https://www.sciencedirect.com/science/article/pii/S0016703720303215
  21. https://www.sciencedirect.com/science/article/abs/pii/S0009254117306277
  22. https://progearthplanetsci.springeropen.com/articles/10.1186/s40645-016-0115-4
  23. https://www.sciencedirect.com/science/article/abs/pii/S0024493718303086
  24. https://academic.oup.com/petrology/article/49/9/1579/1499269
  25. https://www.mdpi.com/2075-163X/9/12/728
  26. https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2020JB020619
  27. http://www-odp.tamu.edu/publications/149_SR/chap_32/c32_5.htm
  28. https://se.copernicus.org/articles/15/1143/2024/
  29. https://www.sciencedirect.com/science/article/pii/S0024493725001574
  30. https://www.sciencedirect.com/science/article/pii/0016703779901686
  31. https://pubs.geoscienceworld.org/gsa/geology/article/49/3/330/592435/The-nanogeochemistry-of-abiotic-carbonaceous
  32. https://www.frontiersin.org/journals/earth-science/articles/10.3389/feart.2021.673063/full
  33. https://www.frontiersin.org/journals/microbiology/articles/10.3389/fmicb.2023.1257597/full
  34. https://pmc.ncbi.nlm.nih.gov/articles/PMC6316048/
  35. https://www.frontiersin.org/journals/earth-science/articles/10.3389/feart.2020.00209/full
  36. https://royalsocietypublishing.org/doi/10.1098/rsta.2018.0429
  37. https://www.pnas.org/doi/10.1073/pnas.1611843113
  38. https://pmc.ncbi.nlm.nih.gov/articles/PMC9840456/
  39. https://pubs.geoscienceworld.org/gsa/geology/article/44/2/175/132075/RESEARCH-FOCUS-Serpentinization-and-the-formation
  40. https://core.ac.uk/download/pdf/30842062.pdf
  41. https://agupubs.onlinelibrary.wiley.com/doi/full/10.1002/2013GC005148
  42. https://www.sciencedirect.com/science/article/pii/S1631071303001354
  43. https://agupubs.onlinelibrary.wiley.com/doi/full/10.1002/2015GC005869
  44. https://www.sciencedirect.com/science/article/pii/S0016703722003155
  45. https://agupubs.onlinelibrary.wiley.com/doi/10.1002/2017GL072893
  46. https://www.sciencedirect.com/science/article/pii/S0009254124001402
  47. https://cdnsciencepub.com/doi/10.1139/cjes-2024-0082
  48. https://pubs.geoscienceworld.org/gsa/geology/article/31/3/267/197774/Seismic-evidence-for-widespread-serpentinized
  49. https://www.sciencedirect.com/science/article/abs/pii/S0012821X03002632
  50. https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2004GC000777
  51. https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2008GL034163
  52. https://academic.oup.com/gji/article/243/3/ggaf378/8285822
  53. https://agupubs.onlinelibrary.wiley.com/doi/full/10.1002/2016GC006598
  54. https://www.sciencedirect.com/science/article/abs/pii/S0012821X19306594
  55. https://www.nature.com/articles/srep01784
  56. https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2020JB020763
  57. https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2020GL090482
  58. https://pubs.geoscienceworld.org/gsa/geosphere/article/16/6/1408/592223/Deep-decoupling-in-subduction-zones-Observations
  59. https://www.nature.com/articles/s41598-024-78193-w
  60. https://www.nature.com/articles/s41467-020-15904-7
  61. https://eps.rutgers.edu/images/Deformation_and_surface_uplift_associated_with_serpentinization_at_mid-ocean_ridges_and_subduction_zones.pdf
  62. https://www.nature.com/articles/s41598-018-35290-x
  63. https://cdnsciencepub.com/doi/10.1139/cjes-2024-0121
  64. https://www.sciencedirect.com/science/article/abs/pii/S0012821X25000123
  65. https://academic.oup.com/femsec/article/77/3/647/518817
  66. https://onlinelibrary.wiley.com/doi/abs/10.1111/j.1472-4669.2010.00249.x
  67. https://pmc.ncbi.nlm.nih.gov/articles/PMC10581274/
  68. https://www.sciencedirect.com/science/article/abs/pii/S0019103517302762
  69. https://www.science.org/doi/10.1126/science.abg7905
  70. https://www.sciencedirect.com/science/article/abs/pii/S0016703715002239
  71. https://www.science.org/doi/10.1126/science.aai8703
  72. https://www.nature.com/articles/s41467-018-02876-y
  73. https://royalsocietypublishing.org/doi/10.1098/rsta.2018.0421
  74. https://www.frontiersin.org/journals/astronomy-and-space-sciences/articles/10.3389/fspas.2025.1544426/full
Add your contribution
Related Hubs
User Avatar
No comments yet.