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Radiation

Radiation.

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Radiation

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  1. Radiation Thermal energy emitted by matter as a result of vibrational and rotational movements of molecules, atoms and electrons. The energy is transported by electromagnetic waves (or photons). Radiation requires no medium for its propagation, therefore, can take place also in vacuum. All matters emit radiation as long as they have a finite (greater than absolute zero) temperature. The rate at which radiation energy is emitted is usually quantified by the modified Stefan-Bolzmann law: where the emissivity, e , is a property of the surface characterizing how effectively the surface radiates compared to a "blackbody" (0<e<1 ). E=q/A (W/m2) is the surface emissive power. s is the Stefan-Boltzmann constant (s=5.67x10-8 W/(m2K4)). Tb is the absolute temperature of the surface (in Kelvin).

  2. Radiation (cont.) Blackbody: is an ideal surface which emits the maximum possible thermal radiation at a given temperature. Irradiation (G): All incoming radiation that is incident on the surface. It can then be transmitted, absorbed or reflected from the surface. G = Gtrans + Gabs + Gref = t G + aG + rG Where t, a and r represent transmissivity, absorptivity and reflectivity, respectively. t + a + r =1

  3. Radiation (cont. 2) Ga=aG Absorbed irradiation

  4. Radiation (cont. 3) Electromagnetic radiation spectrum Thermal radiation spectrum range: 0.1 to 100 mm It includes some ultraviolet (UV) radiation and all visible (0.4-0.76 mm) and infrared radiation (IR).

  5. Radiation (cont. 3) Question: Can microwave-oven heating process be considered one kind of heat transfer mode? Strictly speaking, it is not. It heats up food through microwave radiation, not thermal radiation. However, when microwave energy (with very high frequency) interacts with water molecules inside the food, it generates heat inside the food. Therefore, it can be modeled as some forms of heat generation but not relate to any modes of heat transfer.

  6. Radiation (cont. 4) The Planck Distribution The Planck law describes theoretical spectral distribution for the emissive power of a black body. It can be written as where C1=3.742x108 (W.mm4/m2) and C2=1.439x104 (mm.K) are two constants. The planck distribution is shown in the following figure as a function of wavelength for different body temperatures.

  7. Spectral blackbody emissive power

  8. Planck Distribution • At given wavelength, the emissive power increases with increasing temperature • As the temperature increases,more emissive energy appear at shorter wavelengths • For low temperature (>800 K), all radiant energy falls in the infrared region and is not visible to the human eyes. That is why only very high temperature objects, such as molten iron, can glow. • Sun can be approximated as a blackbody at 5800 K

  9. Solar Irradiation

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