07-Spectra2 - 7. Spectra II - PreLab Name: Section: Date:...

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7. Spectra II - PreLab Name: Section: Date: Blackbody Radiation Every substance emits light. Our bodies glow in infrared colors. This is why you can see human bodies through walls with IR goggles. The hotter the object, the higher the energy the emitted photons will have. A star like the sun is about 6000K, which peaks in greenish-blue visible light. Hotter stars peak in the Ultra-Violet, and the most energetic (hottest) objects in the universe emit X-rays and gamma rays. Objects around the temperatures on Earth emit mostly infrared radiation. Even though objects tend to peak in a certain color, they still emit light at other colors too. Here is a spectrum of an object with various temperatures. The overall shapes of these spectra are called blackbody curves . Any object will produce a spectrum that looks roughly like the ones shown here. The real spectrum of a substance or object will contain other peaks and valleys, but follow the same overall trend. This overall trend is called the continuum . From the previous lab you may remember the law relating the wavelength (remember that’s just like color) of the peak of the spectrum to the temperature of the object. The law is (Wien's law), it states. .. (Brightest Color Light Emitted) = .29/(Temperature in Kelvin)
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07-Spectra2 - 7. Spectra II - PreLab Name: Section: Date:...

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