characteristic that is related to a star's temperature is effective temperature.
characteristic that is related to a star's temperature is effective temperature.
characteristic that is related to a star's temperature?
effective temperature
section::::characteristics.:temperature.









































the surface temperature of a main sequence star is determined by the rate of energy production of its core and by its radius, and is often estimated from the star's color index. the temperature is normally given in terms of an effective temperature, which is the temperature of an idealized black body that radiates its energy at the same luminosity per surface area as the star. note that the effective temperature is only a representative of the surface, as the temperature increases toward the core. the temperature in the core region of a star is several million kelvins.
star
for typical three-dimensional metals, the temperature-dependence of the electrical resistivity "ρ(t)" due to the scattering of electrons by acoustic phonons changes from a high-temperature regime in which "ρ ∝ t" to a low-temperature regime in which "ρ ∝ t" at a characteristic temperature known as the debye temperature. for low density electron systems, however, the fermi surface can be substantially smaller than the size of the brillouin zone, and only a small fraction of acoustic phonons can scatter off electrons. this results in a new characteristic temperature known as the bloch–grüneisen temperature that is lower than the debye temperature. the bloch–grüneisen temperature is defined as "2ħvk/k", where "ħ" is the planck constant, "v" is the velocity of sound, "ħk" is the fermi momentum, and "k" is the boltzmann constant.
bloch–grüneisen temperature