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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.

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

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

• 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.

• 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.

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

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

• 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.

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

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

• 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.

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

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

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

• 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.

• 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.

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