Date post: | 14-Dec-2015 |
Category: |
Documents |
Upload: | osvaldo-hiscock |
View: | 213 times |
Download: | 0 times |
Grain size-dependent viscosity convection
Slava SolomatovWashington University in St. Louis
Acknowledgements: Rifa El-Khozondar
Boulder CO, June 23
Outline
• Mantle rheology
• What controls the grain size?
• How does grain size affect mantle convection?
Simple example (from Solomatov, 1996)
RT
Qd exp2∝η ⎟⎟
⎠
⎞⎜⎜⎝
⎛−∝RT
Qtd gr
3exp3/1
RT
QQt gr 3/2exp3/2 −
∝η
660 km
ColdHot (but can have higher viscosity if Qgr > 1.5Q)
Simple example (from Solomatov, 1996)
RT
Qd exp2∝η ⎟⎟
⎠
⎞⎜⎜⎝
⎛−∝RT
Qtd gr
3exp3/1
RT
QQt gr 3/2exp3/2 −
∝η
660 km
ColdHot (but can have higher viscosity if Qgr > 1.5Q)
Qeff
Possible explanations
• Mantle has more U, Th and K than geochemistry suggests (by as much as 50%)
• Viscous bending controls plate velocity (Christensen and others)
Possible explanations
• Mantle has more U, Th and K than geochemistry suggests (by as much as 50%)
• Viscous bending controls plate velocity (Christensen and others)
• Decreasing convective layering (Peltier and others)
Possible explanations
• Mantle has more U, Th and K than geochemistry suggests (by as much as 50%)
• Viscous bending controls plate velocity (Christensen and others)
• Decreasing convective layering (Peltier and others)
• Larger heat flux from the core than we used to believe
Assumptions
• Lower mantle is in the grain size sensitive creep regime (seismically isotropic = diffusion creep/superplasticity).
• Slab buoyancy is mainly balanced by viscous resistance in the lower mantle (so that plate velocity is controlled by lower mantle viscosity).
Hall and Parmentier (2003) included grain size evolution as well as grain size reduction in a numerical convection model.
Models of mantle reservoirs(from Tackley, 2000)
Layeredmantle
Primitive blobs
Primitivepiles
Well stirred except forprimitive/enrichedbottom
Recycled lithosphere+crust
Deep primitivelayer
The absence of spinel-perovskite transition is an issue for Mars and Mercury – grains (and viscosity) keep growing without recrystallization (to ~1, maybe 10 cm).
Mars and Mercury
Conclusion
Grain size is important for mantle convection:
• Planetary evolution• Plumes• Sublithospheric small-scale instabilities• Chemical mixing
(well, it’s not the size that matters but how muchit changes)