“thermal radiation”的概念、定义、翻译、参考文献-科学参考

thermal radiation

Astronomy

Electromagnetic radiation that arises from the thermal energy of an object. It takes two main forms: black-body radiation, and thermal free–free radiation. All objects emit thermal radiation by virtue of their temperature; for many astronomical objects, such thermal radiation will be very similar to black-body radiation. In free–free radiation, the thermal energy of electrons is converted into radiation as they are accelerated past ions. This accounts for much of the radio emission from hot nebulae. See also non-thermal radiation.

Chemical Engineering

The energy emitted by all bodies above absolute zero temperature due to the excitation by molecular vibration. Energy is transmitted between bodies without heating the space in between unless the medium is capable of absorbing energy. The Stefan–Boltzmann constant, σ, is used in thermal radiation calculations in which the rate of heat loss from a black body is:
$q = ε σ A (T_{1}^{4} - T_{2}^{4})$

where ε is the emissivity, σ the Stefan–Boltzmann constant, A is the area, and T is the absolute temperature. The SI units are J s⁻¹.

单词	thermal radiation
释义	thermal radiation Astronomy Electromagnetic radiation that arises from the thermal energy of an object. It takes two main forms: black-body radiation, and thermal free–free radiation. All objects emit thermal radiation by virtue of their temperature; for many astronomical objects, such thermal radiation will be very similar to black-body radiation. In free–free radiation, the thermal energy of electrons is converted into radiation as they are accelerated past ions. This accounts for much of the radio emission from hot nebulae. See also non-thermal radiation. Chemical Engineering The energy emitted by all bodies above absolute zero temperature due to the excitation by molecular vibration. Energy is transmitted between bodies without heating the space in between unless the medium is capable of absorbing energy. The Stefan–Boltzmann constant, σ, is used in thermal radiation calculations in which the rate of heat loss from a black body is: $q = ε σ A (T_{1}^{4} - T_{2}^{4})$ where ε is the emissivity, σ the Stefan–Boltzmann constant, A is the area, and T is the absolute temperature. The SI units are J s⁻¹.
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