An Etymological Dictionary of Astronomy and Astrophysics
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The energy radiated from an object in the form of → electromagnetic waves as a result of its → temperature. Thermal radiation ranges in → wavelength from the longest → infrared radiation through the → visible light spectrum to the shortest → ultraviolet rays. In opposition, → non-thermal radiation is caused by energetic particles.

→ thermal; → radiation.

Stresses induced in a material because of rapid temperature change or a → thermal gradient .

→ thermal; → shock.

A → transient → rise in → temperature above the normal level in a medium.

→ thermal; → spike.

In star formation models, the gas pressure that counters the collapsing pull of gravity.

→ thermal; → support.

1) The process by which a system reaches → thermal equilibrium. Thermalization results from energy exchange between the components constituting the system and their exchange with the outside medium. In a gas at a given temperature, molecules move with different velocities. The gas temperature corresponds to the mean velocity of the molecules, but individual molecules may deviate largely from the mean velocity. Some move very fast others slowly and change velocity upon collisions. Collisions reduce the energy of fast moving molecules and increase that of slow ones. In the process of thermalization → matter and → radiation are in constant interaction such that their → temperatures become identical. The process goes on until energy distribution reaches → equilibrium. The system is said to be → thermalized.
2) The condition where in an → atomic or → molecular → transition the → Boltzmann factor for the two → levels of transition takes on the value it would have in → thermodynamic equilibrium.

Verbal noun of → thermalize.

To bring neutrons into → thermal equilibrium with their surroundings; to produce → thermal neutrons.

From → thermal + → -ize.

Yekgarmâyidan, literally "equal warming," from yek-, → one, + garmâyidan, infinitive from garmâ, → thermo-.

A collisionally excited spectral line formed in high density condition well above the → critical density. At such densities the → excitation temperature is at (or very near) the → kinetic temperature of the gas. At low densities, below the critical density, the excitation temperature will be only slightly above the radiation temperature and the emission line will be practically invisible.

Thermalized, p.p. of → thermalize; → line.

In evolutionary models of → post-asymptotic giant branch stars, the occurrence of the helium shell burning when the star has reached the → white dwarf cooling track. This leads to the possibility of a violent → helium shell flash and expansion on a time-scale of ≤ 10 years. The rapid expansion and prompt change in surface composition observed in → Sakurai's Object are thought to be due to such a very late thermal pulse.

→ very; → late; → thermal; → pulse.