Earth Structure

obvious from space that Earth has two fundamentally different physiographic features: oceans (71%) and continents (29%) global topography from: crust

Earth’s Plates

MORB Genesis

Submarine Pillow Basalt Formation

Volumes of Igneous Rocks on Earth

Convergent Margin Magma Genesis

Forms of Energy Energy: commonly defined as the capacity to do work (i.e. by system on its surroundings); comes in many forms Work: defined as the product of a force (F) times times a displacement acting over a distance (d) in the direction parallel to the force work = Force x distance Example: Pressure-Volume work in volcanic systems. Pressure = Force/Area; Volume=Area x distance; PV =( F/A)(A*d) = F*d = w

Forms of Energy Kinetic energy: associated with the motion of a body; a body with mass (m) moving with velocity (v) has kinetic energy »E (k) = 1/2 mass * velocity 2 Potential energy: energy of position; is considered potential in the sense that it can be converted or transformed into kinetic energy. Can be equated with the amount of work required to move a body from one position to another within a potential field (e.g. Earth’s gravitational field). »E (p) = mass * g * Z where g = acceleration of gravity at the surface (9.8 m/s 2 ) and Z is the elevation measured from some reference datum

Forms of Energy (con’t.) Chemical energy: energy bound up within chemical bonds; can be released through chemical reactions Thermal energy: related to the kinetic energy of the atomic particles within a body (solid, liquid, or gas). Motion of particles increases with higher temperature. Heat is transferred thermal energy that results because of a difference in temperature between bodies. Heat flows from higher T to lower T and will always result in the temperatures becoming equal at equilibrium.

Heat Flow on Earth An increment of heat,  q, transferred into a body produces a Proportional incremental rise in temperature,  T, given by  q = Cp *  T where Cp is called the molar heat capacity of J/mol-degree at constant pressure; similar to specific heat, which is based on mass (J/g-degree). 1 calorie = J and is equivalent to the energy necessary to raise 1 gram of of water 1 degree centigrade. Specific heat of water is 1 cal/g°C, where rocks are ~0.3 cal/g°C.

Heat Transfer Mechanisms Radiation: involves emission of EM energy from the surface of hot body into the transparent cooler surroundings. Not important in cool rocks, but increasingly important at T’s >1200°C Advection: involves flow of a liquid through openings in a rock whose T is different from the fluid (mass flux). Important near Earth’s surface due to fractured nature of crust. Conduction: transfer of kinetic energy by atomic vibration. Cannot occur in a vacuum. For a given volume, heat is conducted away faster if the enclosing surface area is larger. Convection: movement of material having contrasting T’s from one place to another. T differences give rise to density differences. In a gravitational field, higher density (generally colder) materials sink.

Magmatic Examples of Heat Transfer Thermal Gradient   T between adjacent hotter and cooler masses Heat Flux = rate at which heat is conducted over time from a unit surface area Heat Flux = Thermal Conductivity *  T Thermal Conductivity = K; rocks have very low values and thus deep heat has been retained!

Convection Examples

Rayleigh-Bernard Convection

Convection in the Mantle

convection in the mantle models observed heat flow warmer: near ridges colder: over cratons from: from:

From: "Dynamic models of Tectonic Plates and Convection" (1994) by S. Zhong and M. Gurnis

note continuity of blue slab to depths on order of 670 km blue is high velocity (fast) …interpreted as slab from: examples from western Pacific

example from western US all from:

Earth’s Geothermal Gradient Approximate Pressure (GPa=10 kbar) Average Heat Flux is 0.09 watt/meter 2 Geothermal gradient =  /  z  C/km in orogenic belts; Cannot remain constant w/depth At 200 km would be 4000°C ~7°C/km in trenches Viscosity, which measures resistance to flow, of mantle rocks is times tar at 24°C !

Earth’s Energy Budget Solar radiation: 50,000 times greater than all other energy sources; primarily affects the atmosphere and oceans, but can cause changes in the solid earth through momentum transfer from the outer fluid envelope to the interior Radioactive decay: 238 U, 235 U, 232 Th, 40 K, and 87 Rb all have t 1/2 that >10 9 years and thus continue to produce significant heat in the interior; this may equal 50 to 100% of the total heat production for the Earth. Extinct short-lived radioactive elements such as 26 Al were important during the very early Earth. Tidal Heating: Earth-Sun-Moon interaction; much smaller than radioactive decay Primordial Heat: Also known as accretionary heat; conversion of kinetic energy of accumulating planetismals to heat. Core Formation: Initial heating from short-lived radioisotopes and accretionary heat caused widespread interior melting (Magma Ocean) and additional heat was released when Fe sank toward the center and formed the core

Rates of Heat Production and Half-lives

Heat Production through Earth History

Gravity, Pressure, and the Geobaric Gradient Geobaric gradient defined similarly to geothermal gradient:  P/  z; in the interior this is related to the overburden of the overlying rocks and is referred to as lithostatic pressure gradient. SI unit of pressure is the pascal, Pa and 1 bar (~1 atmosphere) = 10 5 Pa Pressure = Force / Area and Force = mass * acceleration P = F/A = (m*g)/A and  (density) =  mass/volume

Earth Interior Pressures P =  Vg/A =  gz, if we integrate from the surface to some depth z and take positive downward we get  P/  z =  g Rock densities range from 2.7 (crust) to 3.3 g/cm 3 (mantle) 270 bar/km for the crust and 330 bar/km for the mantle At the base of the crust, say at 30 km depth, the lithostatic pressure would be 8100 bars = 8.1 kbar = 0.81 GPa

Changing States of Geologic Systems System: a part of the universe set aside for study or discussion Surroundings: the remainder of the universe State: particular conditions defining the energy state of the system

Definitions of Equilibrium