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Metamorphism changes mineral assemblage and texture under changed pressure, temperature, fluid and deformation conditions without requiring bulk melting.
ModelEarth & cosmos · Chemistry · BiologyWeathering, soil formation and chemical exportMechanical weathering changes fragment size; chemical weathering transforms or dissolves minerals through reactions such as hydrolysis and oxidation.
ModelEarth & cosmos · ChemistryGeochemical partition coefficientsA distribution coefficient relates one species' concentrations in two specified coexisting phases.
ModelEarth & cosmos · ChemistryBatch melting and fractional crystallization modelsIn homogeneous constant-D batch melting, mass balance and equilibrium give melt enrichment Cℓ/C₀=1/[D+F(1−D)].
ModelEarth & cosmosSediment entrainment, transport and depositionStreams carry bed load, suspended material and dissolved solutes through different processes.
ModelEarth & cosmosAquifer storage, permeability and rechargePorosity measures pore-space fraction, while hydraulic permeability/conductivity concerns connected flow under stated fluid conditions.
ModelEarth & cosmos · ChemistryGroundwater chemistry and transport contextGroundwater exchanges dissolved species with aquifer minerals and surfaces.
ModelEarth & cosmosGlacier mass balance and ice motionGlacier accumulation and ablation determine a mass budget; an equilibrium line separates zones in the specified surface-balance picture.
ModelEarth & cosmosGlacial erosion and depositional evidenceMoving ice can abrade and pluck bedrock, while transported debris can be deposited directly as till or sorted by meltwater.
ModelEarth & cosmosGlobal and relative sea-level changeRelative sea level is water level measured against local land.
ModelEarth & cosmosAtmospheric and oceanic hydrostatic balanceWhen vertical acceleration is negligible, the vertical pressure gradient balances gravity: ∂p/∂z=−ρg for upward z.
ApproximationEarth & cosmosGeostrophic flow and Rossby-number scopeFor sufficiently slowly varying large-scale flow away from strong friction, horizontal pressure-gradient and Coriolis accelerations can approximately balance.
ApproximationEarth & cosmosDry adiabatic motion and potential temperatureFor an ideal dry gas with constant heat capacities, potential temperature θ=T(p₀/p)^(Rd/cp) is conserved in reversible adiabatic parcel motion.
ModelEarth & cosmosHumidity, condensation and cloudsWater-vapour amount and relative humidity are distinct; relative humidity compares vapour pressure with a specified saturation value at the current temperature.
ModelEarth & cosmosOcean density, stratification and mixingSeawater density depends on temperature, salinity and pressure.
ModelEarth & cosmosWind stress and Ekman transportIn the steady idealized surface Ekman layer, vertically integrated mass transport is ME=τ×ẑ/f.
ApproximationEarth & cosmosWind-driven gyres and vorticity constraintsSpatially varying wind stress can cause Ekman convergence/divergence and force interior ocean circulation.
ModelEarth & cosmos · Chemistry · BiologyMarine carbonate speciation and exchangeDissolved inorganic carbon includes aqueous CO₂/carbonic-acid convention, bicarbonate and carbonate.
ModelEarth & cosmosPalaeoclimate proxy and chronology inferenceNatural archives such as ice, sediments, corals and tree rings record properties related to past environments.
MethodEarth & cosmosLTE excitation and ionization populationsFor a classical gas in local thermodynamic equilibrium, level ratios within one ionization stage obey N_b/N_a=(g_b/g_a)exp[−(E_b−E_a)/(k_BT)].
ModelEarth & cosmosEquivalent width and spectral-line saturationAn absorption line's wavelength equivalent width is W_λ=∫[1−F_λ/F_{λ,c}]dλ, using the local continuum.
MethodEarth & cosmosDistances and lookback time in FLRW cosmologyIn an expanding FLRW model with present scale factor one, the line-of-sight comoving distance is D_C=c∫₀ᶻ dz′/H(z′), and the lookback time is t_L=∫₀ᶻ dz′/[(1+z′)H(z′)].
ModelEarth & cosmosAngular and luminosity distance observablesFor transparent geometrical photon propagation in FLRW cosmology, angular diameter distance is D_A=D_M/(1+z), and luminosity distance is D_L=(1+z)D_M=(1+z)²D_A.
ModelEarth & cosmosPulsation periods and stellar densityRadial stellar pulsation has a characteristic gravitational/acoustic period scale proportional to √[R³/(GM)].
ModelEarth & cosmosPlanetary equilibrium temperature modelA spherical planet intercepts stellar power over its projected disk and emits thermal power over its surface.
ModelEarth & cosmosJeans parameter and thermal escapeAt an exobase radius r_ex and temperature T_ex, λ=GMm/(r_ex k_BT_ex) compares a species' binding energy with thermal energy.
ModelEarth & cosmosNewtonian tidal gradients and disruption scaleTides arise from gravitational acceleration differences across an extended body.
ModelEarth & cosmosNearly circular galactic disk orbitsIn a smooth stationary axisymmetric potential, expanding about a stable circular guiding radius R_g gives small radial oscillations at epicyclic frequency κ and vertical oscillations at ν.
ModelEarth & cosmosLocal gravitational stability of a gas diskFor a razor-thin rotating ideal fluid disk, local axisymmetric tightly wound perturbations have dispersion ω²=κ²−2πGΣ|k|+c_s²k².
ModelEarth & cosmosClosed-box galactic enrichment modelIn a well-mixed closed gas-plus-star system with initially zero metallicity, instantaneous recycling and constant yield p per mass locked in long-lived stars, gas metallicity follows Z=p ln(1/μ), where μ=M_gas/M_total.
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