Subduction initiation from a stagnant lid and global overturn: new insights from numerical models with a free surface

Fabio Crameri; Paul J. Tackley

doi:10.1186/s40645-016-0103-8

Research Article
Open Access

Subduction initiation from a stagnant lid and global overturn: new insights from numerical models with a free surface

Fabio Crameri^{1, 2, 3}Email author View ORCID ID profile and
Paul J. Tackley³

Progress in Earth and Planetary Science20163:30

https://doi.org/10.1186/s40645-016-0103-8

Received: 20 January 2016
Accepted: 19 August 2016
Published: 29 September 2016

Abstract

Subduction initiation is a key in understanding the dynamic evolution of the Earth and its fundamental difference to all other rocky planetary bodies in our solar system. Despite recent progress, the question about how a stiff, mostly stagnant planetary lid can break and become part in the global overturn of the mantle is still unresolved. Many mechanisms, externally or internally driven, are proposed in previous studies. Here, we present the results on subduction initiation obtained by dynamically self-consistent, time-dependent numerical modelling of mantle convection. We show that the stress distribution and resulting deformation of the lithosphere are strongly controlled by the top boundary formulation: A free surface enables surface topography and plate bending, increases gravitational sliding of the plates and leads to more realistic, lithosphere-scale shear zones. As a consequence, subduction initiation induced by regional mantle flow is demonstrably favoured by a free surface compared to the commonly applied, vertically fixed (i.e. free-slip) surface. In addition, we present global, three-dimensional mantle convection experiments that employ basal heating that leads to narrow mantle plumes. Narrow mantle plumes impinging on the base of the plate cause locally weak plate segments and a large topography at the lithosphere-asthenosphere boundary. Both are shown to be key to induce subduction initiation. Finally, our model self-consistently reproduces an episodic lid with a fast global overturn due to the hotter mantle developed below a former stagnant lid. We conclude that once in a stagnant-lid mode, a planet (like Venus) might preferentially evolve by temporally discrete, global overturn events rather than by a continuous recycling of lid and that this is something worth testing more rigorously in future studies.

Keywords

Subduction initiation
Plate tectonics
Mantle convection
Numerical modelling
Planetary evolution
Geodynamics

Introduction

Earth-like planets lose the heat in their interiors by mantle convection. Part of mantle convection is the cold top boundary layer: The surface boundary layer is either stagnant on top of a flowing mantle or, which seems less common, it is mobile and also part of the vertical flow into and out of the deep mantle (Bercovici 2003; Tackley 2000a,b). The observed high abundance of stagnant lid convection and the fact that mantle viscosity is strongly temperature-dependent and thus likely to produce a stagnant lid (Moresi and Solomatov 1995) indicate that the Earth might have evolved through a stagnant-lid phase in between its early magma ocean phase and its current mobile-lid phase (Sleep 2000; Stern 2007).

To understand how a system evolves from a stagnant-lid to a mobile-lid mode, we need to understand how subduction starts (Gerya 2012; van Hunen and Moyen 2012): Subduction is the main driver of the mobile surface plates on present-day Earth (Conrad and Lithgow-Bertelloni 2002; Forsyth and Uyeda 1975). Yet, subduction initiation (SI) from an initial stagnant lid is still an unresolved problem despite the many mechanisms that have been proposed to break and/or subduct an intact or laterally heterogeneous lithosphere. These mechanisms include, for example, nucleation from an existing rupture produced either by a meteorite impact (Hansen 2007), by a transform fault (Gurnis et al. 1998; Hall et al. 2003; Nikolaeva et al. 2010), by an oceanic plateau (Nair and Chacko 2008; Niu et al. 2003) or by a major episode of delamination (Toth and Gurnis 1998). Different weakening mechanisms like the addition of water or melt into the lithosphere (Dymkova and Gerya 2013; Hirth and Kohlstedt 2003), grain-size reduction (e.g. Bercovici and Ricard 2005, 2013, 2014; Karato et al. 1980, 1986; Rozel et al. 2011), void generation (Bercovici 1998; Regenauer-Lieb 1998) or shear-heating (Crameri and Kaus 2010; Lu et al. 2015; Thielmann and Kaus 2012; Yuen et al. 1978) have been proposed to be a key in subduction initiation by providing a necessary weak and localised, lithospheric-scale shear zone. Although the elastic response of the lithosphere and mantle can be ignored over long times (>1 million years), elasticity might play an important role in subduction initiation (e.g. Hall et al. 2003; Regenauer-Lieb et al. 2001; Thielmann and Kaus 2012; Toth and Gurnis 1998). Mechanisms like the interaction of thermo-chemical plumes with the lithosphere (Burov and Cloetingh 2010; Burov and Gerya 2014; Ueda et al. 2008) or small-scale convection in the sub-lithospheric mantle (Solomatov 2004) might further be able to break an intact lid. It is, however, clear that the question of how subduction might initiate and evolve to its present state remains unclear and elusive (see e.g. Gerya 2011).

Spontaneous initiation and forced initiation are the two principle mechanisms believed to discriminate the key physics involved in subduction initiation during a mobile-lid phase (e.g. on present-day Earth). Spontaneous subduction initiation, on the one hand, is driven solely by the buoyancy contrast of adjacent plates. The density excess of the cold plate compared to its surrounding acts as the primary driving force for subduction (Vlaar and Wortel 1976). The most favourable tectonic setting for spontaneous subduction initiation is a passive margin along an old continent due to its large density contrast (Cloetingh et al. 1989; Nikolaeva et al. 2010). Induced subduction initiation, on the other hand, is characterised by external forces supporting plate convergence. To finally reach self-sustaining subduction, these external forces need to act as long as the negative buoyancy of the underthrusting plate does not exceed the resisting forces for subduction (Mckenzie 1977). The most favourable tectonic setting for induced subduction initiation is therefore a pre-existing plate boundary (e.g. a transform fault or a spreading centre) during a change in plate motion direction.

Although there are many present-day observations of the cessation of subduction zones due to the collision of the trench with, e.g. positively buoyant continents, oceanic plateaus, magmatic arcs or ridges (e.g. Isacks and Molnar 1969), there is less evidence of recent subduction initiation. A few subduction zones are believed to have initiated during the Cenozoic (Gurnis et al. 2004): Apart from the South Sandwich subduction zone, which might have initiated due to a subduction polarity reversal (Crameri and Tackley 2014), they have all appeared in the intra-oceanic setting of the Pacific basin.

Of all the rocky planets of our solar system, a mobile lid is operating only on the Earth. While Mercury has an immobile lithosphere that is heavily marked by mostly old impact craters and volcanic activity, these markers have been modified by the atmosphere and surface fluids (water or melts) on Mars. Below its dense atmosphere, Venus also reveals a heavily cratered lithosphere that is dated by crater statistics to be 500–750 Ma old (McKinnon et al. 1997; Schaber et al. 1992). A global resurfacing event is believed to have happened on Venus during that time, after which the planet formed and retained its stagnant lid. On the long term, Venus’ dynamic evolution is believed to be characterised by the episodic style of plate tectonics, where long-lasting stagnant-lid periods are interrupted by short, dramatic periods of global overturns (Armann and Tackley 2012; Moresi and Solomatov 1998; Reese et al. 1999). The difference between Venus and Earth is believed to be caused the absence of water (Venus’ surface is dry, e.g. Kaula 1999) and the impact of the dense atmosphere (Venus’ surface is hot), which for example reduces the tendency to localise lithosphere-scale thermal shear faults (Crameri and Kaus 2010) or increases healing rates of damaged zones in the lithosphere (Landuyt and Bercovici 2009). Other mechanisms like damage rheology and its feedback with grain size are further discussed to explain a planet’s tendency to develop a mobile-lid style of plate tectonics (e.g. Foley et al. 2012).

In the following, we present new insights on breaking a stagnant lid by (i) small-scale convection in combination with a free surface and by (ii) global mantle convection in combination with either a lateral gradient in mantle temperature or narrow plumes impinging on the base of the lithosphere. Finally, a self-consistent global overturn is produced using numerical modelling on a three-dimensional sphere.

Methods/Experimental

For this numerical modelling study, we use two different model setups. The first is a simplistic regional model in 2D Cartesian geometry that is reproduced from a previous study by Solomatov (2004) and intended to characterise subduction initiation by small-scale convection. The second is a global model in either 2D Cartesian or 3D spherical geometry. It is used to study subduction initiation and the episodic-lid style of plate tectonics within the framework of global mantle convection.

The physical model in both cases consists of an incompressible mantle, applying the Boussinesq approximation. The corresponding non-dimensional equations for conservation of mass, momentum and energy are thus

$$ \vec{\nabla} \cdot \vec{v} = 0 $$

(1)

$$ \vec{\nabla} \cdot {\sigma_{ij}} - \vec{\nabla} p = RaT\,{\hat{\vec{e}}_{z}} $$

(2)

$$ \frac{{\partial T}}{{\partial t}} = {\nabla^{2}}T - \vec{v} \cdot \vec{\nabla} T + H $$

(3)

where v is the velocity, σ _ij is the deviatoric stress tensor, p is the pressure, Ra is the temperature-based Rayleigh number, T is the temperature, ${\hat {\vec {e}}_{z}}$ is the vertical unit vector, t is the time and H is the non-dimensional internal heating rate.

Regional model

The first, regional model setup is used to investigate the ability of small-scale convection to initiate subduction (see “Subduction initiation by small-scale convection” section). The model is similar to the one used and explained by Solomatov (2004). His model is reproduced and compared to additional models that are extended by employing a free surface instead of the usual free-slip surface. The models are run in 2D Cartesian domains with a 4:1 aspect ratio and are purely internally heated and cooled from above. The model boundaries are reflective on the sides and free slip at the bottom and the top, while some models use a sticky-air layer to approximate a free surface (Crameri et al. 2012a; Matsumoto and Tomoda 1983; Schmeling et al. 2008). The models start with a fully intact stagnant lid and use a slightly cooler initial mantle temperature than what is expected for a quasi steady state to which the models then self-consistently evolve to.

The viscosity is defined by a simple exponential law (using the Frank-Kamenetskii approximation to reduce the resulting viscosity contrast) as

$$ \eta \left({T} \right) = b\exp \left({ - \theta T} \right) $$

(4)

where b is a constant, θ is the Frank-Kamenetskii parameter (given in Table 1) and T is the temperature. The viscosity variation is limited to 10 orders of magnitude by the limits η _min and η _max (see Table 3). The heating-based Rayleigh number, R a _H,0=0.1, defined at the surface for this regional model is

$$ Ra_{H,0} = \frac{\rho^{2}g\alpha HD^{5}}{kb\kappa} $$

(5)

Table 1

Parameters used in this study

		Regional model		Global model
		Non-dimensional	Dimensional	Non-dimensional	Dimensional
Parameter	Symbol	value	value	value	value	Units
Mantle depth	D	1	600	1	2890	km
Reference viscosity	η ₀	1	6.92×10²⁷	1	10²³	Pa s
Surface Ra number	R a _H,0	0.1	-			-
Internal Ra number	R a _T,0			10⁶	-	-
Frank-Kamenetskii parameter	θ	60	-			-
Stress exponent	n	1	-			-
Gravitational acceleration	g	-	9.81	-	9.81	ms ⁻²
Thermal conductivity	k	-	3	-	3	Wm ⁻¹ K ⁻¹
Thermal diffusivity	κ	1	10⁻⁶	1	10⁻⁶	m ² s ⁻¹
Thermal expansivity	α	-	3×10⁻⁵	-	3×10⁻⁵	K ⁻¹
Temperature gradient	Δ T	-	2500	-	2500	K
Reference density	ρ ₀	-	3300	-	3300	kg m ⁻³
Heat capacity	C p ₀	-	1200	-	1200	Jkg ⁻¹ K ⁻¹
Internal heating rate	H	1	6.31×10⁻¹²	20	5.44×10⁻¹²	Wkg ⁻¹
Constant yield stress	σ _y,const	variable ^b	variable ^b	variable ^b	variable ^b	MPa
Yield stress gradient	Δ σ _y	variable ^b	variable ^b	variable ^b	variable ^b	-
Friction coefficient	μ			0.09 ^a	-	-
Cohesion	C			100	6.34×10⁵	Pa
Activation energy	E _act			11.55	240	kJmol ⁻¹
Activation volume	V _act			4.0	8.8878×10⁻⁷	m ³mol
Upper viscosity cutoff	η _max	10² η ₀	6.92×10²⁹	10⁵ η ₀	10²⁸	Pa s
Lower viscosity cutoff	η _min	10⁻⁸ η ₀	6.92×10¹⁹	10⁻⁴ η ₀	10¹⁹	Pa s
Sticky-air layer: ^c
Thickness	d _st	0.05	30	0.05	145	km
Viscosity	η _st	10⁻⁸ η ₀	6.92×10¹⁹	10⁻² η ₀	10²¹	Pa s
C-condition ^d	C _Stokes	1.5×10⁻⁷	-	0.175	-	-

^aIndicated is standard setup; parameter variation is mentioned separately

^bFor actual values, see Tables 2 and 3

^cIf applied

^dIndicates suitable free-surface approximation with sticky-air approach if C _Stokes≪1 (Crameri et al. 2012a)

where ρ is the density, g is the gravitational acceleration, α is the thermal expansion coefficient, D is the depth of the convective layer and k and κ are the coefficients of thermal conductivity and diffusion, respectively. The effective yield stress for the regional model, which can be depth-dependent, is defined by

$$ {\sigma_{y}} = {\sigma_{y,\text{const}}} + \Delta {\sigma_{y}} \cdot d $$

(6)

where σ _y,const is a depth-constant yield stress, Δ σ _y is the yield stress gradient and d is the vertical coordinate. The three different yield stress envelopes applied here are presented in Fig. 1 and the specific experimental setup is further explained in Table 2.

Fig. 1
Applied yield stress profiles in regional models. Yield stress envelopes for the different experiments with either depth-constant (Δ σ _y=0), depth-dependent (σ _y,const=∞) or composite (σ _y,const≠∞, Δ σ _y≠0) yield stresses. The transition between brittle (i.e. depth-dependent) and ductile (i.e. depth-constant) yielding is set to occur in the middle of the plate, at 50 km depth

Table 2

Regional model setups

			Constant		Yield stress
			yield stress		gradient	Mean
	Top	Resolution	(σ _y,const)		(Δ σ _y)	plate strength
Tag	boundary	(n x×n y)	[non-dim]	[MPa]	[non-dim]	[MPa]	Regime
lid01	Free-slip	256×64	∞	∞	∞	-	Stagnant
lid02	Free	256×64	∞	∞	∞	-	Stagnant
lidA1	Free-slip	256×64	0.0003	4.4	0	4.4	Mobile
lidA1crit	Free-slip	256×64	0.00035	5.1	0	5.1	Stagnant
lidA2	Free-slip	256×64	0.0004	5.8	0	5.8	Stagnant
lidA3	Free-slip	256×64	0.0005	7.3	0	7.3	Stagnant
lidA4	Free	256×64	0.0003	4.4	0	4.4	Mobile
lidA5	Free	256×64	0.0004	5.8	0	5.8	Mobile
lidA5crit	Free	256×64	0.00045	6.6	0	6.6	Stagnant
lidA6	Free	256×64	0.0005	7.3	0	7.3	Stagnant
lidB1	Free-slip	256×64	0	0	0.003	4.9	Mobile
lidB2	Free-slip	256×64	0	0	0.004	6.5	Stagnant
lidB3	Free-slip	256×64	0	0	0.005	8.1	Stagnant
lidB4	Free-slip	256×64	0	0	0.006	9.7	Stagnant
lidB5	Free	256×64	0	0	0.003	4.9	Mobile
lidB6	Free	256×64	0	0	0.004	6.5	Mobile
lidB7	Free	256×64	0	0	0.005	8.1	Mobile
lidB8	Free	256×64	0	0	0.006	9.7	Stagnant
lidC1	Free-slip	256×64	0.0005	7.3	0.0045	5.5	Mobile
lidC1crit	Free-slip	256×64	0.00055	8.0	0.00495	6.0	Stagnant
lidC2	Free-slip	256×64	0.0006	8.7	0.0054	6.5	Stagnant
lidC3	Free-slip	256×64	0.0007	10.2	0.0063	7.6	Stagnant
lidC4	Free	256×64	0.0005	7.3	0.0045	5.5	Mobile
lidC5	Free	256×64	0.0006	8.7	0.0054	6.5	Mobile
lidC5crit	Free	256×64	0.00065	9.5	0.00585	7.1	Mobile
lidC6	Free	256×64	0.0007	10.2	0.0063	7.6	Stagnant

See “ Regional model” section for more explanations

Dimensionalization

The model described in this section is dimensionalized using the thickness D of the modelled layer for the length scale, D ²/κ for the timescale and ρ H D ²/κ for the temperature scale. The depth of the convective layer D=600 km is estimated from the vertical extent of a small-scale convective cell, which is on the order of 500–1000 km (Solomatov 2004). The thermal diffusivity is given by κ=k/ρ C p ₀, ρ is the density, H=6.31×10⁻¹² W/kg is the internal heating rate and C p ₀ is the heat capacity.

Global model

A second, global model setup is chosen to study subduction initiation on the global scale. It is intended to analyse the findings of the regional model in a more complete, global framework and to produce time-dependent 3D, global mantle convection including hot mantle plumes in a dynamically self-consistent way. To account for the dynamical effect of narrow mantle plumes (e.g. Davies 1994; Morgan 1972), which predominantly form at the CMB and sample the lowermost lower mantle (Cagney et al. 2016), it is important to cover the whole mantle depth. The experiments are, therefore, calculated in a larger domain than the previous regional studies and that comprises the whole mantle depth: They are either in 2D Cartesian or in a 3D full spherical shell geometry. The model assumes the Boussinesq approximation and the rheology is strongly temperature- and pressure-dependent:

$$ \eta \left({T,p} \right) = {\eta_{A}} \cdot \text{exp}\left[ {\frac{{{E_{\text{act}}} + p{V_{\text{act}}}}}{RT}} \right] $$

(7)

where η is the viscosity, p is the pressure, R=8.314 Jmol ⁻¹ K ⁻¹ is the gas constant, T is the temperature, E _act=240 kJ/mol is the activation energy, V _act=8.89·10⁻⁷ m ³mol is the activation volume and the pre-exponential constant η _A is set such that η is the reference viscosity (η ₀) at T=1600 K and p=0 Pa. A temperature-based Rayleigh number of R a _T,0=10⁶ is used for the global models and given by

$$ Ra_{T,0} = \frac{\rho g\alpha\Delta T D^{3}}{\eta_{0}\kappa} $$

(8)

where Δ T is the temperature scale, and the model can be heated both internally and from below (see Table 3). Additionally, plastic yielding is included using a Drucker-Prager yield criterion with the pressure-dependent yield stress σ _y,brittle based on Byerlee’s law

Table 3

Global model setups

				Constant
		Top		yield stress ^a	Friction
	Box	boundary	Resolution	(σ _y,const)	coefficient	Heating
Tag	geometry	condition	(n x×n y×n z × n b)	[MPa]	(μ)	mode
g l o b a l1	Cartesian	Free-slip	2048×1×256	21.7	0.005	Purely internal
g l o b a l2	Cartesian	Free	2048×1×256	21.7	0.005	Purely internal
g l o b a l3	Spherical	Free-slip	128×384×64 × 2	190^b	0.09	Internal & bottom ^c
g l o b a l4	Spherical	Free	128×384×64 × 2	190^b	0.09	Internal & bottom ^c

^aIn addition to a brittle, depth-dependent yield stress (see “Global model” section for more details)

^bGiven is the surface value that increases with depth according to σ _y,ductile=σ _y,const+Δ σ _y·d, where Δ σ _y=0.025 and d is the non-dimensional depth ranging from 0 (top) to 1 (bottom)

^cUsing an isothermal bottom boundary with a non-dimensional temperature of T _bot=1.0

$$ \sigma_{y,\text{brittle}} = C+p\mu $$

(9)

with specified friction coefficient μ and cohesion C. A few models presented here additionally use a maximum, ductile yield stress given by

$$ {\sigma_{y,\text{ductile}}}=\sigma_{y,\text{const}}+\Delta\sigma_{y}\cdot d $$

(10)

where σ _y,const is the surface value of the ductile yield stress, Δ σ _y is the ductile yield stress gradient and d is the non-dimensional depth ranging from 0 (top) to 1 (bottom). The effective yield stress for the global model is then given by

$$ {\sigma_{y}} = \min \left[ {{\sigma_{y,\text{brittle}}},{\sigma_{y,\text{ductile}}}} \right] $$

(11)

Finally, the viscosity variation is limited to 9 orders of magnitude by applying an upper and a lower cutoff of η _max=10⁵ η ₀ and η _min=10⁻⁴ η ₀ (see Table 1).

A low-viscosity asthenosphere is accounted for in the 3D global model setup using two methods: a depth-dependent viscosity increase controlled by V _act and, if applied, a “melting viscosity reduction” (MVR) controlled by a simple solidus function (see Tackley 2000b for a more detailed description).

The outer boundary is isothermal (300 K) and mechanically a free surface. The bottom (core-mantle) boundary is free slip and has either zero heat flux or is isothermal (see Table 3). In Cartesian geometry, the side boundaries are periodic.

Numerical model

All experiments presented here are calculated by the code STAGYY (Tackley 2008), which is based on a finite-volume discretization and a multigrid flow solver. Non-diffusive tracers track the different compositions (regular mantle and sticky air) if applied. To allow for a free evolution of surface topography, a sticky-air layer is used (Matsumoto and Tomoda 1983; Schmeling et al. 2008), which is a good approach for simulating a free surface in an Eulerian grid. It consists of low viscosity “air” of (nearly) zero density that decouples the surface of the lithosphere from the top of the model domain. For a good free-surface treatment, this air layer has to (a) be sufficiently thick and (b) have sufficiently low viscosity (Crameri et al. 2012a). Using the actual viscosity of air or water is computationally unfeasible, but the application of the test conditions (e.g. C _Stokes≪1) provided by Crameri et al. (2012a) show that the sticky-air viscosity assumed here is sufficiently low in combination with the layer thickness to properly allow changes in topography that are driven by mantle convection (see Table 1 for sticky-air parameters including their C _Stokes values). The effective surface topography is tracked using the composition tracers (i.e. searching the interface between air and rock), which allows for subgrid resolution. In the case of a fixed, free-slip top boundary, a traction-derived surface topography is calculated, which is, however, only a valid approximation, if the resulting topography fulfils several criteria (see Crameri et al. 2012a). Finally, our sticky-air models have been tested rigorously earlier in terms of both surface topography (Crameri et al. 2012a) and plate tectonic characteristics (Crameri and Tackley 2015).

The numerical data in this study is processed and visualised using either STAGLAB (www.fabiocrameri.ch/software) or VISIT (Childs et al. 2012).

Plume-tracking software

For this study, a plume-tracking algorithm implemented in STAGLAB is used (see Fig. 10) in order to track hot upwellings that are connected to the hot boundary layer at the base of the convecting mantle similar to the one used in Labrosse (2002).

A temperature at a given location is marked as an anomaly, if it exceeds a certain threshold (f _hot) in the range between the horizontally averaged temperature (T _mean) and the maximum temperature (T _max) at a given depth level (z) according to

$$ {T_{A,\text{hot}}}\left(z \right) = {T_{\text{mean}}}\left(z \right) + {f_{\text{hot}}}\left[ {{T_{\text{max}}}\left(z \right) - {T_{\text{mean}}}\left(z \right)} \right] $$

(12)

where a threshold of f _hot=1 (or f _hot=0) defines anomalies that are 100 % (or 0 %) hotter than the horizontal average in the possible range between mean and maximum temperature.

Once all hot anomalies are located, they are checked on their connection to the bottom boundary layer by a classical image processing procedure, searching for connected pixels in a matrix (e.g. Kovesi 2000). In this study, anomalously hot features are tracked in order to visualise active upwellings and their specific threshold value is given in the respective figure captions.

Results

Here, we test first the ability of small-scale convection to initiate subduction with the two different top boundary conditions and, second, the importance of basal heating and an initial stagnant-lid phase on the mode of plate tectonics in global models of mantle convection.

Subduction initiation by small-scale convection

A lithosphere below a free surface can be expected to develop a different stress pattern (e.g. through slight convection-induced bending) than a lithosphere that is vertically fixed at its top (Thielmann et al. 2015). We, therefore, compare the behaviour of an intact, stagnant lid that is either vertically fixed or can freely evolve in the vertical direction. Solomatov (2004) provides a numerical study of such a setup (using a vertically-fixed, free-slip top boundary) that investigates the ability of stresses exerted by sub-lithospheric small-scale convection to break a stagnant lid. Some of these models are reproduced and compared to additional models with a free surface.

No yield stress

Deformation in Earth’s mantle is mainly controlled by its temperature- and pressure-dependent rheology. Yet, it is now an established fact that a temperature- and pressure-dependent rheology alone leads to a flowing mantle with a stagnant lid on its top (Nataf and Richter 1982; Ratcliff et al. 1997; Solomatov 1995; Stengel et al. 1982). The cold, stagnant top boundary layer is thereby too strong to be broken apart by the stresses exerted via the coupling to the convecting, low-viscosity mantle underneath: Subduction does not initiate. The convective stresses are thereby focussed at the uppermost part of the lid, its coldest and thus strongest part (see Fig. 2 a and Additional file 1: Figure S1.1). A non-Newtonian weakening mechanism like brittle or ductile yielding has previously been shown to be the key mechanism to prevent a stagnant lid and to allow for subduction (Tackley 2000a).

Fig. 2
Radial parameter profiles of regional models. Radial profiles of experiments with a no yielding, b depth-dependent yielding, c depth-constant yielding and d composite yielding with a transition at 50 km depth. Shown in each subplot are temperature (*left*), viscosity (*middle*) and second invariant of stress (*right*) for both regional models with either a free-slip surface (*grey*) or a free surface (*orange*)

For the study on subduction initiation by small-scale convection enabled by plastic yielding, we therefore present three suites of a simple regional model with either a simple depth-constant yield stress, a depth-dependent yield stress or a more realistic, composite yield stress by superimposing the two previous formulations (see Fig. 1).

Depth-constant yield stress

Solomatov (2004) employed experiments with varying plate strength that tested different constant (i.e. depth-independent) yield stresses. In one set of experiments, the lithosphere weakened solely by employing a (non-dimensional) depth-independent yield stress σ _y,const. He found that small-scale convection is able to initiate subduction in weak plates with σ _y,const=0.0003 (4.4 MPa) but not in “strong” plates with σ _y,const=0.0004 (5.8 MPa). This result is confirmed by our models shown in Fig. 3 a–c.

Interestingly, subduction of a “strong” plate with σ _y,const=0.0004 (5.8 MPa) can be initiated using the same model setup plus a free surface (Fig. 3 e). The time it takes for subduction to initiate is longer than in the case with a lower σ _y,const, where subduction occurs more readily (Fig. 3 d). An even stronger plate with σ _y,const=0.0005 (7.3 MPa), however, can resist stresses exerted by small-scale convection even with a free surface and does not result in subduction initiation (Fig. 3 f).

Depth-dependent yield stress

In a second suite of experiments, we consider a Byerlee-type, depth-dependent yield stress, again according to Solomatov (2004). The minimum variation of the Δ σ _y parameter between two different experiments is as low as possible to still be resolved spatially: The vertical resolution at lithospheric depths is around 10 km, which still resolves a change of the yield stress gradient (Δ σ _y) of ±0.001 at around 100 km depth (i.e. at the lithosphere-asthenosphere boundary) in the parameter range chosen (see Fig. 1). This is important to consider because the numerical grid slightly differs between the two models due to the missing/presence of the sticky-air layer.

Similarly to the depth-constant yield stress experiments, this comparison indicates that a free surface favours subduction initiation in comparison to a vertically fixed (free-slip) surface (see Table 2 and Additional file 1: Figures S1.3 and S1.4). Experiments with a vertically fixed surface develop subduction only until a yield stress gradient of Δ σ _y=0.0003 but not for higher values. Higher values of up to Δ σ _y=0.0005, however, still yield subduction in the free surface experiments. A yield stress gradient of Δ σ _y=0.0006 finally prevents subduction caused by small-scale convection in both models.

Composite yield stress

The third suite of experiments shown in Fig. 4 with the regional model applies a more Earth-like composite yield stress, with a brittle, depth-dependent yield stress in the upper part and a ductile, depth-constant part in the lower part of the lithosphere. The cross-over between brittle and ductile yielding is set such that it occurs approximately in the middle of the lithosphere, which is here set at 50 km depth.

Again, subduction occurs more readily when the vertically fixed surface is replaced by a free surface (Fig. 4 e): The maximum ductile yield stress that still allows subduction to occur is σ _y,const=0.0005 (7.3 MPa) and σ _y,const=0.00065 (9.5 MPa) for the free-slip and the free surface model, respectively. Limiting the strength of the lithosphere at shallow depth therefore allows for a 64 % stronger lower part that still entirely yields and subsequently subducts.

Free slip versus free surface

Modelling of mantle convection becomes more realistic when the top surface of the mantle is treated as a free surface instead of being vertically fixed (i.e. free slip): A free surface allows for natural plate bending (Crameri et al. 2012b). The plate bending in turn causes a characteristic lithospheric stress pattern resulting in two thin (instead of one thick) horizontal layers of high stress (Crameri 2013; Thielmann et al. 2015).

In our high-resolution regional models, we find that another striking difference between free-slip and free surface models exists. Both fixed and a free surface model setups lead to lithosphere-scale shear zones that, given a suitable flow rheology, eventually trigger subduction initiation. The most striking difference lies, however, within these shear zones: While a vertically fixed surface leads to broad, diffuse shear zones (Fig. 5 d), multiple criss-crossing, narrow shear zones next to each other characterise models with a free surface (Fig. 5 i). This striking difference can be attributed to the deformation in the uppermost parts of the plate. If the surface is fixed, vertical deformation at shallow depth has to be translated entirely into horizontal deformation due to mass conservation. A vertically, or near-vertically dipping shear zone (e.g. at 45°) therefore always involves a significant amount of horizontal strain, which causes the localised deformation to widen horizontally.

Fig. 5
Free-slip versus free surface steady-state stagnant lid. Small-scale convection experiments l i d C2 with a free-slip surface (*left hand side column*) and l i d C5 with a free surface (*right hand side column*) both employing a composite yield stress with a yield stress gradient of Δ σ _y=0.0054 and a dimensional, constant yield stress of σ _y,const=8.7 MPa. a Surface topography of the free-slip top boundary model that is calculated from the normal stress occurring at the vertically fixed, top domain boundary and f the actual topography that occurs in the model with the free top boundary. b, g Effective viscosity and the 700 K contour (*black line*), c, h second invariant of the strain rate, d, i second invariant of stress and e, j horizontal velocity are shown for both models, where *green colours* indicate flow in clockwise direction. If applied, the sticky-air layer is removed visually and replaced with a hatched grey area. Very high values are clipped in regions where they exceed a certain maximum value (*black areas*). *White arrows* and *grey streamlines* indicate the flow direction and pattern

The free surface, on the contrary, enables a lithosphere-scale shear zone to maintain its strain direction throughout the plate interior to the plate surface by creating actual topography there. Since a single fault is rarely able to accommodate the total horizontal deformation of the plate, a characteristic crisscrossing pattern of aligned and mirrored shear zones dipping at around 45° forms as is visible in Fig. 5 g, i. This feature occurs throughout all the free-surface experiments considered here independent of applied yielding formulation, their time-dependent evolution or the numerical resolution (see Additional file 1: Figures S1.5 and S1.6). Additional figures and a movie show this in more detail (see Additional file 1: Figures S1.2 and S1.3, and the ). Small-scale horst and graben-like structures are thereby the topographic result of multiple normal or reverse faults situated next to each other in regions of extension or compression, respectively (Fig. 5 f). In contrast to the broad, diffuse shear zones in the free-slip surface models, straight and localised deformation zones occurring in models with a free surface are more efficient to take up tectonic stresses and allow the shear zones to reach deeper. A shear zone that reaches the bottom of the lithosphere is a prerequisite for subduction initiation as has been pointed out by Fowler and O’Brien (2003). A model with a free surface might therefore favour subduction initiation as discussed below (see Fig. 6).

Fig. 6
Time evolution of plastic-zone depth. Maximum depth of brittle yielding over time shown for the critical experiments a, b l i d A2 and l i d A5 with depth-constant yield stress, c, d l i d B3 and l i d B7 with depth-dependent yield stress and e, f l i d C2 and l i d C5 with a composite yield stress, where there is no subduction with the free-slip surface (*top row*) but subduction with the free surface (*bottom row*). The depth of the thermal lithosphere (sampled at T=700 K and marked by a *black line* in Fig. 5 b, g) is indicated by the dark grey band, whereby its thickness indicates the range between the minimum and the maximum depth found at the given point in time. A sudden drop of the graph to deep levels (>200 km) indicates the initiation of subduction

Additional file 2: Movie of the experiment “lidC5” showing the temporal evolution of the regional model for (a) topography, (b) viscosity, the second invariant of (c) the stress and (d) the strain-rate tensor, (e) horizontal velocity and (f) the dominating deformation mechanism. (MOV 7114 kb)

Another mechanism to cause deeper brittle yielding might be the slight time-dependent bending of the plates while floating on a weaker, convecting mantle. The time-dependent mantle up- and downwellings induce a time-dependent vertical forcing on the plate floating above, which causes topography at the lithosphere-asthenosphere boundary (LAB). In the model where the top surface is vertically fixed, this deflection at the base of the plate is accommodated by plate-internal deformation. Releasing the plate surface from its vertical fixity, however, causes the plate to deflect in its entirety: positive and negative surface deflections matching the LAB topography occur above mantle up- and downwellings, respectively (Fig. 5 f). The strong plate-internal deformation occurring in the model with a vertically fixed surface is reduced when applying a free surface and accommodated by vertical deflection of the whole plate: The plate is bending.

While the convective stresses in the free-slip surface model cause internal deformation and convert to rather shallow accumulation of lithospheric stresses, they cause plate bending in the free surface model, which in turn increases shallow but also deep lithospheric stresses. Although the thermal thickness of the lid is similar for both upper boundary conditions, the high stress pattern in the case of the composite yield stress experiments reaches deeper in the case of a free surface (Fig. 5 c, h). Figure 2 shows the radial profiles of the root-mean-square (RMS) values of temperature, viscosity and the second invariant of the stress tensor for all models. The different stress distribution—solely caused by the free surface—is significant in all experiments, even though temperature and viscosity profiles are similar.

Plate bending favours another important tectonic mechanism: The lateral gradient in vertical plate deflection (i.e. tilting) causes a gravitation-induced, horizontal sliding of the plate segments. The plate segments, separated by the narrow weak zones of high deformation, tend to flow from the high pressure above mantle upwellings to the low pressure above mantle downwellings (Fig. 5 e, j). The tilting of the plate segments together with the resulting gravitational sliding cause regionally high lithospheric stresses (in between tilted segments) that lead to increased and deeper yielding in the case with a free surface. In the models with a fixed surface, mantle up- and downwellings cause lateral pressure gradients inside the plate that lead to horizontal flow similar to the gravitational sliding mentioned above. However, the plate segments are, due to the fixed top, not tilted and this does therefore not cause any additional stress.

The maximum depth of yielding can be taken as an indicator for lithosphere-scale shear zones. Figure 6 shows the maximum depth of brittle and/or ductile yielding during the temporal evolution of the models. The maximum depth of yielding increases shortly after the model’s initial state and during onset of convection in the mantle, while the plate thickness slowly decreases over time due to slight heating up of the model and subsequent erosion at the base of the plate. The different time-dependent fluctuation of the maximum yielding depth between free-slip and free surface models is mostly caused by the different top boundary conditions (and their implications) rather than variations in mantle flow, as the time-dependent evolution of the flow below the plate is similar for both model setups. Although the yielding occurs then throughout most of the thermal lithosphere in the free-slip model at around 3.8 Ga (see Fig. 6 a), it does not exceed its maximum thickness: subduction does not initiate. The maximum depth of yielding exceeds, however, the depth of the thermal lithosphere in the free-surface model and subduction initiates (Fig. 6 b). The same occurrence can be observed in the models applying a depth-dependent (Fig. 6 c, d) or a composite yield stress (Fig. 6 e, f). These experiments therefore show that subduction initiates once the model produces plastic failure down to the lithosphere-asthenosphere boundary.

The above results consider only small-scale convection, which is only one feature in a long list of possible triggers for subduction initiation in global models as the ones presented subsequently.

Subduction initiation by large-scale convection

Although global-scale models lack the spatial resolution of regional models, they do, in contrast, account for additional triggers of lithosphere-scale failure. Global-scale convective cells and narrow plumes rising from the core-mantle boundary (CMB) impinging the base of the lithosphere are just two of these mechanism that we focus on in the following sections.

Global stagnant-lid convection

In our global models, we apply both a stronger plate (than in the regional models) and a high plate-mantle viscosity contrast in order to prevent double-sided subduction and instead enable realistic, single-sided subduction (Crameri et al. 2012b). Necessitating a strong plate, single-sided subduction is therefore harder to initiate. Global-scale flow that produces wide mantle flow cells (i.e. >400 km) might, however, induce significantly higher lithospheric stresses and thus facilitate subduction initiation (e.g. Wong and Solomatov 2015). The global models presented in this section can, in contrast to the regional models above, where flow cells in the mantle are relatively narrow (e.g. <400 km), account for the effect of wider convection cells.

The purpose of our global 2D models is to reproduce the findings of our regional models regarding lithospheric deformation features. Figure 7 presents such an experiment with the free surface, while Additional file 1: Figure S1.7 presents the corresponding experiment with the free-slip surface. Here, we slightly increase the strength of the plate with a friction coefficient of μ=0.005 and a maximum yield stress of σ _y,const=21.7 MPa. We can indeed find the lithospheric criss-cross shear pattern again in the models where the surface evolves freely but not in the models where the surface is fixed vertically. Moreover, lithosphere-scale failure occurs early in the model evolution, even though these global models apply a slightly higher yield stress than the regional models. This supports previous findings (e.g. Wong and Solomatov 2015) that global mantle flow with larger flow cells adds a significant amount of additional forcing to the lid at the surface. The exact amount of the additional forcing has to be, however, carefully investigated in a future study.

Fig. 7
Free surface steady-state stagnant-lid in the 2-D global models. Lithosphere-scale yielding induced by global-scale convection of experiment g l o b a l2 with a free surface. The model employs a composite yield stress with a yield stress gradient of Δ σ _y=0.005 and a dimensional, constant yield stress of σ _y,const=21.7 MPa. Shown are a effective topography, b effective viscosity, c second invariant of the stress, and d second invariant of strain rate. The sticky-air layer is removed visually and replaced with a hatched grey area. Very high values are clipped in regions where they exceed a certain maximum value (*black areas*). *White arrows* and *grey streamlines* indicate the flow direction and pattern

Narrow hot mantle plumes

In general, models with realistic (e.g. based on laboratory measurements) friction coefficient and/or yield stress fail to break an intact stagnant lid. Even models that produce on-going single-sided subduction are, up to this point, not able to initiate subduction once in a stagnant-lid mode (e.g. Crameri et al. 2012b). The global 3D model presented in this section additionally includes narrow hot mantle plumes together with an even stronger plate that is, however, still relatively weak compared to laboratory estimates (see “Discussion” section for an extended discussion) using a friction coefficient of μ=0.09 and a maximum yield stress of σ _y,const=190.0 MPa. The experiment presented here with the free-slip surface (i.e. g l o b a l3) therefore remains in stagnant-lid convection even after a long time of more than 6 Ga (bottom row of Figure 8 and Additional file 1: Figure S1.8). However, the corresponding experiment that additionally features a free surface (i.e. g l o b a l4) spontaneously initiates subduction after starting in stagnant-lid mode (top row Figs. 8 and 9). An additional movie file shows this in more detail (see ). The mantle plumes are caused by the combined heating from the bottom (i.e. from the CMB) as well as from within. The isothermal CMB thereby favours the development of narrow plumes that are able to locally weaken the lithosphere and hence to facilitate subduction initiation as was previously suggested by Ueda et al. (2008) and Burov and Cloetingh (2010). This model additionally applies a depth-constant, ductile yield stress in combination with the depth-dependent yield stress (see Table 3). This helps to critically weaken the base of the plate and increases the impact that mantle plumes have on the cold plate.

Fig. 8
Temporal evolution of both global, 3D spherical models with different top boundary conditions. The free-slip model (g l o b a l3) remains in stagnant-lid mode (*top row*), while the free surface model (g l o b a l4) produces subduction initiation and a subsequent global overturn event (*bottom row*). Cold plates are indicated by viscosity isosurfaces (*grey*) and hot mantle plumes by a temperature isosurface (*red*). Presented snapshots are taken at t _E3=5.29 Ga, t _E4−5=5.66 Ga and t _E7=6.49 Ga or t _E5−6=6.09 Ga. An additional movie file shows the free surface model in more detail (see Additional file 3)

Fig. 9
Time snapshots of SI by global mantle flow. Temporal evolution of subduction initiation in a global, 3-D spherical experiment (g l o b a l4) showing the cold plates by viscosity isosurfaces (*grey*) and mantle plumes by a temperature isosurface (*red*). Individual snapshots highlight the different phases characterised by a onset of hot mantle plumes, b local lithospheric thinning, c-d development of strong LAB-topography through shallow horizontal mantle flow and an additional plume pulse, e-f plate failure, and finally g-h buoyancy-driven subduction

Additional file 3: Movie of the experiment “global4” showing the temporal evolution of the global, fully spherical, 3D model with the hot temperature isosurface (red) and stiff viscosity isosurfaces (grey). (MOV 22192 kb)

Figure 9 illustrates the time evolution in multiple snapshots at the location of the initial subduction initiation inside the 3D spherical model. This event can be attributed to the following five phases. Phase 1: Local lithospheric thinning by plumes is characterised by narrow rising plumes impinging the base of the fully intact, stagnant lid. The additional heat at the lithosphere-asthenosphere boundary (LAB) from the hot upwellings causes the lithosphere to locally weaken and to thin out (Fig. 9 b). Phase 2: Large LAB topography develops by the continued local thinning caused by mantle plumes and the associated thickening nearby caused by the return flow of the hot upwelling. The return flow consists of a laterally limited horizontal component (connecting up- and downwelling) and a downward component. Both are causing significant topography in the base of the lithosphere (Fig. 9 c). Phase 3: An additional plume pulse by a reactivation of the upwelling causes a broad patch of hot material spreading at the base of the thinned lid. This further weakens the already thin plate and causes a decoupling of the thick part of the lithosphere from its thinned surroundings (Fig. 9 d). Phase 4: Plate failure is caused by the sinking of the thickened plate portion. The sinking of the plate can be related (i) to its negative buoyancy, (ii) to the adjacent, hot and failing part of the plate and (iii) to the support of the already existing downward return flow of the plume-driven convective cell (Fig. 9 e, f). Phase 5: Subduction finally takes place and the sinking slab rearranges the mantle flow in its surroundings: The typical poloidal flow in the mantle wedge and in the back-slab region and the toroidal flow around the slab edges form (Fig. 9 g).

The observation of these five phases indicates that the occurrence of LAB topography (phase 2) and the heating caused by hot mantle upwellings (phases 1 and 3) are here key to produce subduction initiation from a stagnant lid.

Global overturn event

Once a stagnant lid spontaneously initiates subduction, it can evolve either by an ongoing mobile lid or by an episodic lid that is characterised by temporally separated events with intermediate stagnant-lid phases (Tackley 2000a,b). In the latter case, a single episode of lithosphere recycling is termed a “global overturn”, which is believed to be the dominant mechanism in Venus’ dynamic evolution (e.g. Armann and Tackley 2012; Reese et al. 1999). Here, we present and discuss a global, fully spherical model that produces, for the first time, such a global overturn event.

The time evolution of the model with both internal and basal heating is presented in Fig. 10. This experiment starts from a globe-covering, intact lid that has no lateral heterogeneities (like plate thickness variations or slabs). Due to heating at the CMB, several point-like, hot upwellings (i.e. mantle plumes) form and cause locally round locations of weakening at the base of the lithosphere (t _E1). This weakening is enforced at later stages of the evolution and the former point-like plumes start to merge (hence reducing their total number) and deform to more elongated, sheet-like structures at time t _E2. The flow in the upper mantle is mainly dominated by these upwellings at this stage. The hot upwellings usually form thereby the centre of one of the several convection cells. At time t _E3, subduction has initiated at one spherical weak patch in the lithosphere that is close to but not exactly above one of the strongest hot anomalies. Single-sided subduction forms a horseshoe-shaped trench that kinks into one double-horseshoe-shaped structure and splits into a separately evolving subduction zone at time t _E4. The two subduction zones subsequently propagate throughout the model forming more complex and wider structures until a nearly intact belt of subduction is covering the globe (t _E5). Mantle flow is now dominated by the sinking portions of the plates. A few anomalously hot upwellings supported by the CMB still remain. Subduction stops again, shortly after the recycling of most of the former stagnant lid at time t _E6.

After spontaneously starting subduction from a stagnant lid, the model evolves with a mobile lid until the oldest and hence coldest and strongest portions (i.e. the former stagnant lid) are recycled into the mantle. Subduction acts quickly and so does not allow the newly created plate portions to cool down sufficiently to become sufficiently negative buoyant. These portions cannot therefore continue to subduct and the systems falls back into stagnant lid mode. This global overturn event operates around 1.2 Ga.

For such an event to happen, high plate velocities caused by a fast sinking of the slabs are needed. This can be enforced by having a small viscosity increase with depth (see Crameri et al. 2012b) or more generally by a lower viscosity mantle. The first is not the cause in this study, since other models presented here do not show a global overturn event although they have the same amount of viscosity increase with depth. The latter, a generally lower mantle viscosity, is, however, enforced by having a stagnant lid in the beginning. This is due to the fact that stagnant-lid convection is not as efficient at cooling the mantle than mobile-lid convection and thus heats up the mantle. We show that once in a stagnant-lid mode, a planet thus might preferentially evolve by temporally discrete global overturn events rather than by a continuous recycling of lid. This has strong relevance to Earth’s sister planet Venus, as it currently has no mobile lid, but is believed to recycle its surface episodically in such spectacular global-overturn events (e.g. Armann and Tackley 2012). The initial difference, however, that caused a stagnant-lid on Venus and a mobile lid on Earth might be explained by the absence of liquid water on Venus’ surface (Kaula 1999) and the impact of the hot, dense Venusian atmosphere, which can inhibit localisation of lithosphere-scale thermal shear faults (Crameri and Kaus 2010) or foster healing through increased grain-growth (Landuyt and Bercovici 2009).

Discussion

The goal of this study is to explore the initiation of Earth-like subduction using a modelling approach that is as simplified as possible while still retaining key first-order physical characteristics. We consider these key characteristics to be a strongly temperature-dependent, visco-plastic rheology and a free surface. Hence, the two model setups presented here are not intended to be exact replicas of an Earth-like rocky planet, and the simplifications may cause some disagreements with nature. We therefore evaluate model features below.

Model features that are not in good agreement with natural observations are the plate thickness in the global models, which is larger than realistic due to a low effective Rayleigh number, and the relatively low maximum yield strength of σ _y<7 MPa obtained here for the initiation of subduction by small-scale convection in the regional models: Even with a free surface, the latter is still around two orders of magnitude lower than the σ _y∼800 MPa expected for the strong core of the lithosphere based on laboratory rock measurements (Goetze and Evans 1979; Kohlstedt et al. 1995). Similarly small is the friction coefficient μ∼0.1 that mainly controls the lithospheric strength in the global models, when compared to estimates from lithospheric flexure and seismicity caused by oceanic islands, μ>0.25 (Zhong and Watts 2013), and to laboratory rock measurements, μ∼0.5−0.8. It should be noted, though, that subduction initiation preferentially occurs at the weakest places of the lithosphere and that the models presented here do not have preexisting weak zones in contrast to nature. The plate as modelled here therefore has to be weak in its entirety. The occurrence of subduction initiation in our models both with and without localised upwellings (that locally weaken the lithosphere) implies, however, the importance of small- and large-scale convection to produce lithospheric stresses close to what is needed for nature-like lithosphere-scale failure.

In contrast, there are model features that have been improved to agree well with observations. Given the resolution applied in the regional models, lithosphere-scale shear zones are modelled more realistically with a free surface than with a fixed surface. This indicates that a free surface in subduction-initiation modelling is important.

Previous self-consistent spherical 3D models of plate tectonics with a free-slip surface and a lower viscosity contrast between cold plates and hot mantle have had no problem to spontaneously initiate subduction (e.g. Foley and Becker 2009; Nakagawa et al. 2010; Rolf and Tackley 2011; Tackley 2000a,b; van Heck and Tackley 2008). However, compared to the global models presented here, they all lack realistic single-sided subduction—a key feature of global mantle convection observed on Earth. The global model presented in this study, in contrast, develops nature-like subduction and is able to produce an episodic lid self-consistently even with a realistically high viscosity contrast (see Crameri and Tackley 2015).

Nevertheless, subduction initiation is still challenging even with the model presented here. There are, however, simplifying assumptions made here, which may hamper subduction initiation and might thus explain the current discrepancy between models and nature as listed below: Low effective Rayleigh number: The relatively low effective Rayleigh number as applied in the global model inhibits the occurrence of convection on a smaller scale. One consequence is a thicker and hence stronger lithosphere that resists failure and subduction initiation more readily. No elasticity: Both models presented here apply a simplified visco-plastic rheology, with no elasticity. Elasticity, however, might be important in the lithosphere as elastic bending operates on shorter time periods than the viscous bending considered in this study (e.g. Zhong 2002). Moreover, elasticity might increase lithospheric stress at deep levels (Beuchert and Podladchikov 2010; Thielmann et al. 2015). Although it might reduce the risk of lithospheric shear localisation at first due to the reduction of the total deformation work, it might additionally favour subduction initiation later on by releasing the stored elastic work into deformation when a lithospheric shear zone has established (Thielmann and Kaus 2012). No continental lithosphere: Both our models assume a compositionally homogeneous lithosphere (i.e. no continents). Continental lithosphere, however, might focus lithospheric stresses and hence foster subduction initiation (Rolf and Tackley 2011). No lithospheric weakening mechanisms: There is a long list of potential weakening mechanisms that are believed to support lithosphere-scale failure (as listed in the “Introduction” section). None of them are taken into account for the modelling presented here. Doing so would, however, further facilitate lithosphere-scale failure and subsequent subduction initiation.

An individual, systematic testing of the mentioned physical complexities in dynamically self-consistent, time-dependent global models seems therefore crucial and should be the focus of future studies.

Conclusions

The regional models presented here confirm that a relatively low yield stress of σ _y<7 MPa is needed to allow for subduction to initiate due to lithospheric stresses induced by sub-lithospheric small-scale convection. In this study, we show that subduction initiation by small-scale convection is, however, favoured by a free surface as compared to a vertically fixed, free-slip surface. A free rock-air interface causes surface down- and uplifts, enables plate bending and increases the horizontal, gravitational sliding of plate portions from high-pressure regions above mantle upwellings to low-pressure regions above mantle downwellings. A freely evolving rock-air interface further allows for more realistic, linear and narrow lithosphere-scale shear zones. These shear zones penetrate through the whole plate by vertically offsetting rigid blocks at the surface and so lead to the characteristic criss-cross pattern. The combination of all of these features caused by a free surface finally increases the tendency for subduction to occur spontaneously out of an initial stagnant lid that is applied to the forcing of small-scale convection.

In addition to the regional models, we present data from two global-scale models with whole-mantle convection. These global models indicate that both a free surface and narrow hot plumes caused by basal heating at the core-mantle boundary indeed facilitate subduction initiation. On the one hand, a global-scale model enables wide convection cells that increase lithospheric stresses and facilitate lithospheric failure. The mantle plumes impinge, on the other hand, at the base of the lithosphere create locally hot and weak patches, which cause a significant topography of the lithosphere-asthenosphere interface. This can lead to the removal of large pieces of lithospheric material by horizontal asthenospheric flow, which in turn might cause lithosphere-scale failure and subsequently subduction initiation.

Such a subduction initiation is then shown to be able to cause an episodic overturn of the planet. A stagnant-lid phase causes, thereby, the mantle to heat up due to lack of cooling-efficient subduction. When subduction is initiated in such a hot state, subduction operates much faster due to the hotter and thus weaker mantle. A fast global resurfacing event is the result, which consumes the old and cold lithosphere until it is stopped by the resulting, globally spanning young and still buoyant surface. In conclusion, this indicates that once in a stagnant-lid mode, an Earth-like planet preferentially evolves by continuing in the episodic-lid rather than the mobile-lid mode of plate tectonics. However, this has to be tested with additional experiments spanning a wider parameter range.

Abbreviations

CMB:: Core-mantle boundary

LAB:: Lithosphere-asthenosphere boundary

SI:: Subduction initiation

Declarations

Funding

This work was supported by the Research Council of Norway through its Centres of Excellence funding scheme, project number 223272. This work was further supported by a grant from the Swiss National Supercomputing Centre (CSCS) under project ID s272. Some calculations were additionally performed on ETH’s Brutus high-performance computing cluster. Further methodical details and the raw numerical data can be requested from the author (www.fabiocrameri.ch).

Authors’ contributions

FC and PJT collaborated on developing the idea and designing the study. FC carried out and analysed the experiments. PJT wrote the code StagYY. FC and PJT collaborated with the writing and read and approved the final manuscript.

Competing interests

The authors declared that they have no competing interests.

Open Access This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made.

Authors’ Affiliations

(1)

Centre for Earth Evolution and Dynamics, University of Oslo, postbox 1028 Blindern, Oslo, 0315, Norway

(2)

Department of Earth Sciences, University College London, Gower Street, London, WC1E 6BT, UK

(3)

Department of Earth Sciences, ETH Zurich, Sonneggstrasse 5, Zurich, 8092, Switzerland

References

Armann, M, Tackley PJ (2012) Simulating the thermochemical magmatic and tectonic evolution of Venus’s mantle and lithosphere: two-dimensional models. J Geophys Res 117(E12): 12003.View ArticleGoogle Scholar
Bercovici, D (1998) Generation of plate tectonics from lithosphere-mantle flow and void-volatile self-lubrication. Earth Planet Sci Lett 154(1–4): 139–151.View ArticleGoogle Scholar
Bercovici, D (2003) The generation of plate tectonics from mantle convection. Earth Planet Sci Lett 205(3–4): 107–121.View ArticleGoogle Scholar
Bercovici, D, Ricard Y (2005) Tectonic plate generation and two-phase damage: void growth versus grain size reduction. J Geophys Res 110(B3): 03401.View ArticleGoogle Scholar
Bercovici, D, Ricard Y (2013) Generation of plate tectonics with two-phase grain-damage and pinning: source–sink model and toroidal flow. Earth Planet Sci Lett 365(0): 275–288.View ArticleGoogle Scholar
Bercovici, D, Ricard Y (2014) Plate tectonics, damage and inheritance. Nature 508(7497): 513–516.View ArticleGoogle Scholar
Beuchert, MJ, Podladchikov YY (2010) Viscoelastic mantle convection and lithospheric stresses. Geophys J Int 183(1): 35–63.View ArticleGoogle Scholar
Burov, E, Cloetingh S (2010) Plume-like upper mantle instabilities drive subduction initiation. Geophys Res Lett 37(3): 03309.View ArticleGoogle Scholar
Burov, E, Gerya T (2014) Asymmetric three-dimensional topography over mantle plumes. Nature 513(7516): 85–89.View ArticleGoogle Scholar
Cagney, N, Crameri F, Newsome WH, Lithgow-Bertelloni C, Cotel A, Hart SR, Whitehead JA (2016) Constraining the source of mantle plumes. Earth Planet Sci Lett 435: 55–63.View ArticleGoogle Scholar
Childs, H, Brugger E, Whitlock B, Meredith J, Ahern S, Pugmire D, Biagas K, Miller M, Harrison C, Weber GH, Krishnan H, Fogal T, Sanderson A, Garth C, Bethel EW, Camp D, Rübel O, Durant M, Favre JM, Navrátil P (2012) VisIt: an end-user tool for visualizing and analyzing very large data In: High Performance Visualization–Enabling Extreme-Scale Scientific Insight, 357–372.. Taylor and Francis, Boca Raton.Google Scholar
Cloetingh, S, Wortel R, Vlaar NJ (1989) On the initiation of subduction zones. Pure Appl Geophys 129(1–2): 7–25.View ArticleGoogle Scholar
Conrad, CP, Lithgow-Bertelloni C (2002) How mantle slabs drive plate tectonics. Science 298(5591): 207–209.View ArticleGoogle Scholar
Crameri, F, Kaus BJP (2010) Parameters that control lithospheric-scale thermal localization on terrestrial planets. Geophys Res Lett 37(9): 09308.View ArticleGoogle Scholar
Crameri, F, Schmeling H, Golabek GJ, Duretz T, Orendt R, Buiter SJH, May DA, Kaus BJP, Gerya TV, Tackley PJ (2012a) A comparison of numerical surface topography calculations in geodynamic modelling: an evaluation of the ‘sticky air’ method. Geophys J Int 189(1): 38–54.View ArticleGoogle Scholar
Crameri, F, Tackley PJ, Meilick I, Gerya TV, Kaus BJP (2012b) A free plate surface and weak oceanic crust produce single-sided subduction on Earth. Geophys Res Lett 39(3): 03306.View ArticleGoogle Scholar
Crameri, F (2013) The interaction between subduction-related mantle currents and surface topography. PhD thesis. ETH Zurich.Google Scholar
Crameri, F, Tackley PJ (2014) Spontaneous development of arcuate single-sided subduction in global 3-D mantle convection models with a free surface. J Geophys Res Solid Earth 119(7): 5921–5942.View ArticleGoogle Scholar
Crameri, F, Tackley PJ (2015) Parameters controlling dynamically self-consistent plate tectonics and single-sided subduction in global models of mantle convection. J Geophys Res Solid Earth 120(5): 3680–3706.View ArticleGoogle Scholar
Davies, GF (1994) Thermomechanical erosion of the lithosphere by mantle plumes. J Geophys Res 99(88): 15709–15722.View ArticleGoogle Scholar
Dymkova, D, Gerya T (2013) Porous fluid flow enables oceanic subduction initiation on Earth. Geophys Res Lett 40(21): 5671–5676.View ArticleGoogle Scholar
Foley, BJ, Becker TW (2009) Generation of plate-like behavior and mantle heterogeneity from a spherical, viscoplastic convection model. Geochem Geophys Geosyst 10(8): 08001.View ArticleGoogle Scholar
Foley, BJ, Bercovici D, Landuyt W (2012) The conditions for plate tectonics on super-Earths: inferences from convection models with damage. Earth Planet Sci Lett331–332(0): 281–290.View ArticleGoogle Scholar
Forsyth, D, Uyeda S (1975) On the relative importance of the driving forces of plate motion*. Geophys J R Astron Soc 43(1): 163–200.View ArticleGoogle Scholar
Fowler, A, O’Brien S (2003) Lithospheric failure on Venus. Proc Roy Soc Lond Math Phys Sci 459(2039): 2663–2704.View ArticleGoogle Scholar
Gerya, T (2011) Future directions in subduction modeling. J Geodyn 52(5): 344–378.View ArticleGoogle Scholar
Gerya, T (2012) Origin and models of oceanic transform faults. Tectonophysics522-523(0): 34–54.View ArticleGoogle Scholar
Goetze, C, Evans B (1979) Stress and temperature in the bending lithosphere as constrained by experimental rock mechanics. Geophys J Int 59: 463–478.View ArticleGoogle Scholar
Gurnis, M, Hall C, Lavier L (2004) Evolving force balance during incipient subduction. Geochem Geophys Geosyst 5(7): 07001.View ArticleGoogle Scholar
Gurnis, M, Müller RD, Moresi L (1998) Cretaceous vertical motion of Australia and the Australian Antarctic discordance. Science 279(5356): 1499–1504.View ArticleGoogle Scholar
Hall, CE, Gurnis M, Sdrolias M, Lavier LL, Müller RD (2003) Catastrophic initiation of subduction following forced convergence across fracture zones. Earth Planet Sci Lett 212(1–2): 15–30.View ArticleGoogle Scholar
Hansen, VL (2007) Subduction origin on early Earth: a hypothesis. Geology 35(12): 1059–1062.View ArticleGoogle Scholar
Hirth, G, Kohlstedt D (2003) Rheology of the upper mantle and the mantle wedge: a view from the experimentalists In: Geophys. Monogr. Ser, 83–105.. AGU, Washington, DC. http://dx.doi.org/10.1029/138GM06.Google Scholar
Isacks, B, Molnar P (1969) Mantle earthquake mechanisms and the sinking of the lithosphere. Nature 223(5211): 1121–1124.View ArticleGoogle Scholar
Karato, S-I, Toriumi M, Fujii T (1980) Dynamic recrystallization of olivine single crystals during high-temperature creep. Geophys Res Lett 7(9): 649–652.View ArticleGoogle Scholar
Karato, S-I, Paterson MS, FitzGerald JD (1986) Rheology of synthetic olivine aggregates: influence of grain size and water. J Geophys Res 91(B8): 8151–8176.View ArticleGoogle Scholar
Kaula, WM (1999) Constraints on Venus evolution from radiogenic argon. Icarus 139(1): 32–39.View ArticleGoogle Scholar
Kohlstedt, DL, Evans B, Mackwell SJ (1995) Strength of the lithosphere: constraints imposed by laboratory experiments. J Geophys Res 100(B9): 17587–17602.View ArticleGoogle Scholar
Kovesi, PD (2000) Matlab and octave functions for computer vision and image processing. Online: http://www.peterkovesi.com/matlabfns/. Accessed 25 Aug 2016.
Labrosse, S (2002) Hotspots, mantle plumes and core heat loss. Earth Planet Sci Lett 199(12): 147–156.View ArticleGoogle Scholar
Landuyt, W, Bercovici D (2009) Variations in planetary convection via the effect of climate on damage. Earth Planet Sci Lett 277(1–2): 29–37.View ArticleGoogle Scholar
Lu, G, Kaus BJP, Zhao L, Zheng T (2015) Self-consistent subduction initiation induced by mantle flow. Terra Nova27: 130–138. ISSN:1365-3121, http://dx.doi.org/10.1111/ter.12140.View ArticleGoogle Scholar
Matsumoto, T, Tomoda Y (1983) Numerical simulation of the initiation of subduction at the fracture zone. J Phys Earth 31(3): 183–194.View ArticleGoogle Scholar
Mckenzie, DP (1977) The Initiation of Trenches: A finite amplitude instability In: Island Arcs, Deep Sea Trenches and Back-Arc Basins, 57–61.. American Geophysical Union, Washington, DC. ISSN:9781118665756, http://dx.doi.org/10.1029/ME001p0057.View ArticleGoogle Scholar
McKinnon, WB, Zahnle KJ, Ivanov BA, Melosh HJ (1997) Cratering on Venus: Models and observations. In: Bougher SW, Hunten DM, Philips RJ (eds)Venus II: Geology, geophysics, atmosphere, and solar wind environment, 969.. University of Arizona Press, Tucson.Google Scholar
Moresi, L, Solomatov VS (1995) Numerical investigation of 2D convection with extremely large viscosity variations. Phys Fluids 7(9): 2154–2162.View ArticleGoogle Scholar
Moresi, L, Solomatov VS (1998) Mantle convection with a brittle lithosphere: thoughts on the global tectonic styles of the Earth and Venus. Geophys J Int 133(3): 669–682.View ArticleGoogle Scholar
Morgan, WJ (1972) Deep mantle convection plumes and plate motions. AAPG Bull 56(2): 203–217.Google Scholar
Nair, R, Chacko T (2008) Role of oceanic plateaus in the initiation of subduction and origin of continental crust. Geology 36(7): 583–586.View ArticleGoogle Scholar
Nakagawa, T, Tackley PJ, Deschamps F, Connolly JAD (2010) The influence of MORB and harzburgite composition on thermo-chemical mantle convection in a 3-D spherical shell with self-consistently calculated mineral physics. Earth Planet Sci Lett 296(3–4): 403–412.View ArticleGoogle Scholar
Nataf, HC, Richter FM (1982) Convection experiments in fluids with highly temperature-dependent viscosity and the thermal evolution of the planets. Phys Earth Planet Inter 29(3–4): 320–329.View ArticleGoogle Scholar
Nikolaeva, K, Gerya TV, Marques FO (2010) Subduction initiation at passive margins: numerical modeling. J Geophys Res 115(B3): 03406.View ArticleGoogle Scholar
Niu, Y, O’Hara MJ, Pearce JA (2003) Initiation of subduction zones as a consequence of lateral compositional buoyancy contrast within the lithosphere: a petrological perspective. J Petrol 44(5): 851–866.View ArticleGoogle Scholar
Ratcliff, JT, Tackley PJ, Schubert G, Zebib A (1997) Transitions in thermal convection with strongly variable viscosity. Phys Earth Planet Inter 102(3–4): 201–212.View ArticleGoogle Scholar
Reese, CC, Solomatov VS, Moresi L-N (1999) Non-Newtonian stagnant lid convection and magmatic resurfacing on Venus. Icarus 139(1): 67–80.View ArticleGoogle Scholar
Regenauer-Lieb, K (1998) Dilatant plasticity applied to Alpine collision: ductile void growth in the intraplate area beneath the Eifel volcanic field. J Geodyn 27(1): 1–21.View ArticleGoogle Scholar
Regenauer-Lieb, K, Yuen DA, Branlund J (2001) The initiation of subduction: criticality by addition of water?Science 294(5542): 578–580.View ArticleGoogle Scholar
Rolf, T, Tackley PJ (2011) Focussing of stress by continents in 3D spherical mantle convection with self-consistent plate tectonics. Geophys Res Lett 38(18): 18301.View ArticleGoogle Scholar
Rozel, A, Ricard Y, Bercovici D (2011) A thermodynamically self-consistent damage equation for grain size evolution during dynamic recrystallization. Geophys J Int 184(2): 719–728.View ArticleGoogle Scholar
Schaber, GG, Strom RG, Moore HJ, Soderblom LA, Kirk RL, Chadwick DJ, Dawson DD, Gaddis LR, Boyce JM, Russell J (1992) Geology and distribution of impact craters on Venus: what are they telling us?J Geophys Res 97(E8): 13257–13301.View ArticleGoogle Scholar
Schmeling, H, Babeyko AY, Enns A, Faccenna C, Funiciello F, Gerya T, Golabek GJ, Grigull S, Kaus BJP, Morra G, Schmalholz SM, van Hunen J (2008) A benchmark comparison of spontaneous subduction models—towards a free surface. Phys Earth Planet Inter 171(1–4): 198–223.View ArticleGoogle Scholar
Sleep, NH (2000) Evolution of the mode of convection within terrestrial planets. J Geophys Res 105(E7): 17563–17578.View ArticleGoogle Scholar
Solomatov, VS (1995) Scaling of temperature- and stress-dependent viscosity convection. Phys Fluids 7: 266.View ArticleGoogle Scholar
Solomatov, VS (2004) Initiation of subduction by small-scale convection. J Geophys Res 109(B1): 01412.View ArticleGoogle Scholar
Stengel, KC, Oliver DS, Booker JR (1982) Onset of convection in a variable-viscosity fluid. J Fluid Mech 120: 411–431.View ArticleGoogle Scholar
Stern, RJ (2007) When and how did plate tectonics begin? Theoretical and empirical considerations. Chinese Sci Bull 52 52(5): 578–591.View ArticleGoogle Scholar
Tackley, PJ (2000a) Self-consistent generation of tectonic plates in time-dependent, three-dimensional mantle convection simulations—Part 1: pseudo-plastic yielding. Geochem Geophys Geosyst 1(8): 1–45.Google Scholar
Tackley, PJ (2000b) Self-consistent generation of tectonic plates in time-dependent, three-dimensional mantle convection simulations—Part 2: strain weakening and asthenosphere. Geochem Geophys Geosyst 1: 1–45.Google Scholar
Tackley, PJ (2008) Modelling compressible mantle convection with large viscosity contrasts in a three-dimensional spherical shell using the yin-yang grid. Phys Earth Planet Inter 171(1–4): 7–18.View ArticleGoogle Scholar
Thielmann, M, Kaus BJP (2012) Shear heating induced lithospheric-scale localization: does it result in subduction?Earth Planet Sci Lett359/360(0): 1–13.View ArticleGoogle Scholar
Thielmann, M, Kaus BJP, Popov AA (2015) Lithospheric stresses in Rayleigh–Bénard convection: effects of a free surface and a viscoelastic Maxwell rheology. Geophys J Int 203(3): 2200–2219.View ArticleGoogle Scholar
Toth, J, Gurnis M (1998) Dynamics of subduction initiation at preexisting fault zones. J Geophys Res 103(B8): 18053–18067.View ArticleGoogle Scholar
Ueda, K, Gerya T, Sobolev SV (2008) Subduction initiation by thermal-chemical plumes: numerical studies. Phys Earth Planet Inter 171(1–4): 296–312.View ArticleGoogle Scholar
van Heck, HJ, Tackley PJ (2008) Planforms of self-consistently generated plates in 3D spherical geometry. Geophys Res Lett 35(19): 19312.View ArticleGoogle Scholar
van Hunen, J, Moyen J-F (2012) Archean subduction: fact or fiction?Annu Rev Earth Planet Sci 40(1): 195–219.View ArticleGoogle Scholar
Vlaar, NJ, Wortel MJR (1976) Lithospheric aging, instability and subduction. Tectonophysics 32(3–4): 331–351.View ArticleGoogle Scholar
Yuen, DA, Fleitout L, Schubert G, Froidevaux C (1978) Shear deformation zones along major transform faults and subducting slabs. Geophys J R Astron Soc 54(1): 93–119.View ArticleGoogle Scholar
Wong, T, Solomatov V (2015) Towards scaling laws for subduction initiation on terrestrial planets: constraints from two-dimensional steady-state convection simulations. Progress Earth Planetary Sci 2(1): 18.View ArticleGoogle Scholar
Zhong, S (2002) Effects of lithosphere on the long-wavelength gravity anomalies and their implications for the formation of the Tharsis rise on Mars. J Geophys Res 107(E7): 8–1–8-13.View ArticleGoogle Scholar
Zhong, S, Watts A. B (2013) Lithospheric deformation induced by loading of the Hawaiian Islands and its implications for mantle rheology. J Geophys Res Solid Earth 118(11): 2013–010408.View ArticleGoogle Scholar