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The 49 pages that link to Thermal equilibrium, each with the reason it gives.

• TemperatureRelated: Equal temperatures mark the absence of net heat flow.

• Heat transferCompared with: It marks the condition reached when temperature differences no longer drive net transfer.

• Big Bang nucleosynthesisRelated: Early reaction rates initially kept particle populations close to thermal equilibrium.

• Thermodynamic equilibriumBroader topic: It is the thermal condition required for full thermodynamic equilibrium.

• Thermal radiationRelated: Equilibrium underlies the standard laws for ideal thermal radiation.

• Black-body radiationNarrower topic: Black-body radiation is the equilibrium radiation field associated with a body's temperature.

• Kinetic theory of gasesRelated: Equilibrium gives the stable statistical state described by the theory.

• Heat capacityRelated: Temperature change, the denominator of heat capacity, is defined through thermal states.

• Effective temperatureNarrower topic: It is the condition under which ordinary thermodynamic temperature has a consistent equilibrium meaning.

• Gravitational collapseCompared with: A collapsing object may gain heat without reaching thermal equilibrium.

• CalorimetryRelated: Equilibration establishes the final temperature needed for a heat balance.

• Thermal massRelated: Thermal mass exchanges heat with surroundings until temperatures approach equilibrium.

• Thermodynamic stateRelated: It is one component of full thermodynamic equilibrium, not a complete state criterion.

• BaryogenesisCompared with: Baryogenesis requires conditions that evade equilibrium, where generated asymmetries would otherwise be erased.

• Equipartition theoremRelated: The theorem predicts averages only under equilibrium conditions.

• ThermometerRelated: A contact thermometer approaches the measured object’s temperature through thermal equilibration.

• Thermal inertiaCompared with: Equilibrium is a final state; thermal inertia governs the pace of reaching it.

• Isothermal processRelated: Maintaining constant temperature often requires contact with a heat reservoir.

• Maxwell–Boltzmann distributionRelated: The distribution describes particle speeds or energies in this equilibrium state.

• Exothermic reactionCompared with: An exothermic reaction drives heat transfer until its surroundings approach thermal equilibrium.

• Population inversionCompared with: A system with ordinary positive temperature has fewer particles in higher energy levels.

• Ultraviolet catastropheRelated: Blackbody spectra are defined for radiation in equilibrium with matter at a temperature.

• Kirchhoff's law of thermal radiationNarrower topic: The law applies when matter and radiation share a common equilibrium temperature.

• Baryon asymmetryCompared with: Equilibrium erases generated asymmetries, so baryogenesis requires conditions that depart from it.

• Carryover cookingNarrower topic: Carryover cooking ends as temperature differences within the food diminish.

• Infrared thermographyRelated: Temperature is a property of matter, while a thermal camera observes radiation leaving it.

• Optical pumpingCompared with: Optical pumping drives populations away from this equilibrium distribution.

• Fluctuation–dissipation theoremRelated: The theorem’s standard relations require equilibrium before perturbation.

• Countercurrent heat exchangeRelated: The exchanger's streams approach equilibrium as they exchange heat.

• Zeroth law of thermodynamicsBroader topic: The law's relation is defined by this state.

• Absolute temperatureRelated: Absolute temperature quantifies the shared thermal state in equilibrium.

• Maxwell–Boltzmann statisticsRelated: The distribution describes particles after equilibration at a common temperature.

• Electroweak baryogenesisCompared with: Baryogenesis requires departure from equilibrium, which a sufficiently strong first-order transition could provide.

• Primordial nucleosynthesisRelated: Early equilibrium governed particle abundances before expansion disrupted weak interactions.

• Sakharov conditionsCompared with: Departure from equilibrium prevents reactions from simply erasing the generated asymmetry.

• Isolated systemRelated: An isolated system can approach equilibrium through internal energy redistribution.

• PhotoevaporationRelated: Heating and cooling rates set the temperature that drives or suppresses gas escape.

• Bose–Einstein distributionRelated: The formula describes occupations after equilibration at a common temperature.

• Boltzmann brainRelated: The hypothesis considers observers arising in a universe that has reached equilibrium.

• Brightness temperatureRelated: A blackbody-like spectrum can make brightness temperature correspond to a source’s physical temperature.

• Newton's law of coolingRelated: The modeled object approaches this state with its surroundings.

• Active matterCompared with: Persistent motion and energy consumption prevent active systems from settling into this state.

• Black bodyRelated: Black-body spectra describe radiation in thermal equilibrium with matter.

• Microscopic reversibilityRelated: The principle presumes equilibrium conditions rather than externally driven molecular traffic.

• Meghnad SahaRelated: The equation assumes matter in a star is close to thermal equilibrium.

• Temperature measurementRelated: Contact measurements require enough heat exchange for sensor and target to equilibrate.

• Lepton epochNarrower topic: The epoch’s particle abundances were governed by thermal equilibrium until interactions became too weak.

• Debye T³ lawRelated: The law describes heat capacity for phonons in thermal equilibrium.

• High-energy-density plasmaCompared with: Experiments can produce nonequilibrium plasmas whose electrons and ions differ in temperature.