“luminosity”的概念、定义、翻译、参考文献-科学参考

luminosity

Physics

1. Luminous intensity in a particular direction; the apparent brightness of an image.

2. The brightness of a star defined as the total energy radiated in unit time. It is related to the surface area (A) and the effective temperature (T_e; the temperature of a black body having the same radius as the star and radiating the same amount of energy per unit area in one second) by a form of Stefan’s law, i.e.

$L = A σ T_{e}^{4}$

where σ‎ is the Stefan constant and L is the luminosity.

Astronomy

The amount of radiation a star emits, corrected for interstellar absorption. It is expressed in watts, or in terms of the luminosity of the Sun (L_☉), defined by the IAU as 3.828 × 10²⁶ watts. Luminosity is related to the absolute bolometric magnitude (see absolute magnitude) of the star, M_bol, by the equation
$M_{bol} - 4.72 = - 2.5 \log (L / L_{⊙}) .$
The luminosities of stars range from over 10⁵L_☉ for the brightest supergiants to less than 10⁻⁵L_☉ for feeble red dwarfs. For X-ray sources it is usual to define luminosity not bolometrically but in particular passbands.

Space Exploration

The amount of light emitted by a star, measured in magnitudes. The apparent brightness of an object decreases in proportion to the square of its distance from the observer. The luminosity of a star or other body can be expressed in relation to that of the Sun.

单词	luminosity
释义	luminosity Physics 1. Luminous intensity in a particular direction; the apparent brightness of an image. 2. The brightness of a star defined as the total energy radiated in unit time. It is related to the surface area (A) and the effective temperature (T_e; the temperature of a black body having the same radius as the star and radiating the same amount of energy per unit area in one second) by a form of Stefan’s law, i.e. $L = A σ T_{e}^{4}$ where σ‎ is the Stefan constant and L is the luminosity. Astronomy The amount of radiation a star emits, corrected for interstellar absorption. It is expressed in watts, or in terms of the luminosity of the Sun (L_☉), defined by the IAU as 3.828 × 10²⁶ watts. Luminosity is related to the absolute bolometric magnitude (see absolute magnitude) of the star, M_bol, by the equation $M_{bol} - 4.72 = - 2.5 \log (L / L_{⊙}) .$ The luminosities of stars range from over 10⁵L_☉ for the brightest supergiants to less than 10⁻⁵L_☉ for feeble red dwarfs. For X-ray sources it is usual to define luminosity not bolometrically but in particular passbands. Space Exploration The amount of light emitted by a star, measured in magnitudes. The apparent brightness of an object decreases in proportion to the square of its distance from the observer. The luminosity of a star or other body can be expressed in relation to that of the Sun.
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