Thermal Equilibrium
(a) A state in which there is no net flow of heat. If two bodies are in thermal equilibrium, then they have the same temperature. (see also Equilibrium) ...
Thermal Equilibrium - The condition in which a body or a portion of a body gains energy (by generating it or absorbing it) at the same rate at which energy is transported away from it ...
isothermal equilibrium The state of an atmosphere at rest, uninfluenced by any external agency, in which the conduction of heat from one part to another has, after a sufficient length of time, ...
Thermal Equilibrium: (1) The idea that any energy radiated away from an object (e.g. a star) is replaced by energy generation so that the temperatures remain constant.
Maxwell-Boltzmann distribution (Plasma Physics and Fusion Energy Glossary) Distribution function of particle velocities (or energies) corresponding to a system in thermal equilibrium with a temperature value of T.
The gas molecules in a canister of gas are distributed homogeneously and isotropically because they are in thermal equilibrium: gas throughout the canister has had enough time to interact to dissipate inhomogeneities and anisotropies.
Blackbody radiation is produced after a group of particles and photons have come into thermal equilibrium with each other, with every reaction between the particles balanced by the reverse reaction, so that the system as a whole has stopped changing.
WEAKLY INTERACTING MASSIVE PARTICLES (WIMPs) - Broad class of particles that were once in thermal equilibrium with the early universe but were "cold," i.e., moving non-relativistically at the time of structure formation.
Before recombination matter and energy are strongly coupled by scattering - the density is high enough to approach thermal equilibrium. The epoch of recombination may also be called the epoch of decoupling.
The condition follows from the assumption that light is emitted and absorbed by atoms independently, and that the thermal equilibrium is preserved by interaction with atoms.
When two systems are at the same temperature, they are in thermal equilibrium and no heat transfer will occur.
The intensity of light illuminating the object is known (from its distance to the Sun), and one assumes that most of its surface is in thermal equilibrium (usually not a bad assumption for an airless body).
In quantum mechanics, the black hole emits Hawking radiation, and so can come to thermal equilibrium with a gas of radiation.
Thick mirrors also take longer to reach thermal equilibrium each night, reducing the achievable resolution and adding to seeing effects. Modern primaries, however, can be made very thin. Those for the Gemini telescopes are only 20-cm thick.
For a celestial body (such as a star or cloud of interstellar gas) which is in thermal equilibrium, the continuum emission approximates a blackbody spectrum, with a peak in emission at a wavelength determined by the object's temperature.
However, due to the equation for thermal equilibrium (below), it should only be about 80 K. This extra heat is generated due to its gas slowly separating.
black-body radiation The characteristic way in which the intensity of radiation emitted by a hot object in thermal equilibrium depends on frequency.
Our next major subdivision of the Radiation Era covers the period when all "heavy" elementary particles"that is, all the way down in mass to protons, neutrons, and their constituent quarks"were in thermal equilibrium with the radiation.
Albert Einstein Particle statistics determines the statistical distribution of identical identical particles bosons over the energy states in thermal equilibrium....
are now used to describe the behaviors of any assembly of "boson ...
is flowing out from the Sun and it is not cooling off, energy must be generated somewhere inside the Sun. Since the Sun is not heating up that energy generation rate must be equal to the Sun's luminosity. This is the concept of thermal equilibrium.
Less energy is released when heavier elements are undergoing fusion, so the star needs to burn that material at a greater rate to produce enough energy to sustain the structure of the star (to maintain stuff like Hydrostatic and Thermal Equilibrium).
 See also: Energy, Temperature, Field, Second, Element
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