The thermal history of Earth involves the study of the cooling history of Earth's interior. It is a sub-field of geophysics. The study of the thermal evolution of Earth's interior is uncertain and controversial in all aspects, from the interpretation of petrologic observations used to infer the temperature of the interior, to the fluid dynamics responsible for heat loss, to material properties that determine the efficiency of heat transport.
Overview Observations that can be used to infer the temperature of Earth's interior range from the oldest rocks on Earth to modern seismic images of the inner core size. Ancient volcanic rocks can be associated with a depth and temperature of melting through their geochemical composition. Using this technique and some geological inferences about the conditions under which the rock is preserved, the temperature of the mantle can be inferred. The mantle itself is fully convective, so that the temperature in the mantle is basically constant with depth outside the top and bottom thermal boundary layers. This is not quite true because the temperature in any convective body under pressure must increase along an adiabat, but the adiabatic temperature gradient is usually much smaller than the temperature jumps at the boundaries. Therefore, the mantle is usually associated with a single or potential temperature that refers to the mid-mantle temperature extrapolated along the adiabat to the surface. The potential temperature of the mantle is estimated to be about 1350 C today. There is an analogous potential temperature of the core but since there are no samples from the core its present-day temperature relies on extrapolating the temperature along an adiabat from the inner core boundary, where the iron solidus is somewhat constrained.
Thermodynamics The simplest mathematical formulation of the thermal history of Earth's interior involves the time evolution of the mid-mantle and mid-core temperatures. To derive these equations one must first write the energy balance for the mantle and the core separately. They are,
Q surf = Q sec,man + Q rad + Q cmb {\displaystyle Q_{\text{surf}}=Q_{\text{sec,man}}+Q_{\text{rad}}+Q_{\text{cmb}}}
for the mantle, and
Q cmb = Q sec,core + Q L + Q G {\displaystyle Q_{\text{cmb}}=Q_{\text{sec,core}}+Q_{\text{L}}+Q_{\text{G}}}
for the core. Q surf {\displaystyle Q_{\text{surf}}} is the surface heat flow [W] at the surface of the Earth (and mantle), Q sec,man = M man c man d T man / d t {\displaystyle Q_{\text{sec,man}}=M_{\text{man}}c_{\text{man}}dT_{\text{man}}/dt} is the secular cooling heat from the mantle, and M man {\displaystyle M_{\text{man}}} , c man {\displaystyle c_{\text{man}}} , and T man {\displaystyle T_{\text{man}}} are the mass, specific heat, and temperature of the mantle. Q rad {\displaystyle Q_{\text{rad}}} is the radiogenic heat production in the mantle and Q cmb {\displaystyle Q_{\text{cmb}}} is the heat flow from the core mantle boundary. Q sec,core = M core c core d T core / d t {\displaystyle Q_{\text{sec,core}}=M_{\text{core}}c_{\text{core}}dT_{\text{core}}/dt} is the secular cooling heat from the core, and Q L {\displaystyle Q_{\text{L}}} and Q G {\displaystyle Q_{\text{G}}} are the latent and gravitational heat flow from the inner core boundary due to the solidification of iron. Solving for d T man / d t {\displaystyle dT_{\text{man}}/dt} and d T core / d t {\displaystyle dT_{\text{core}}/dt} gives,
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