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This chapter explores the continuous spectrum emitted by hot, dense objects such as the Sun, planets, and moons, known as the thermal spectrum. This spectrum, which consists of the basic colors of the rainbow (ROYGBIV), occurs when white light is refracted. Additionally, it discusses emission spectra, produced by atoms and molecules in hot gases, and absorption spectra, which result from gases removing specific wavelengths of light. These concepts are crucial for understanding radiation and energy transitions in astrophysical contexts, as first noted by William Wollaston in 1802.
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Chapter 4: Learning Goal 1 Zach Saragin MichelinaRestaino
Continuous Spectrum • Cont. Spect. are found from hot, dense objects, eg, sun, planets, moons • Also called the Thermal Spectrum b/c Electromagnetic Radiation • It’s the basic ray of colors, roygbiv • It occurs when the white light is refracted with no other complications
Emission Spectrum • When atoms and molecules travel through a hot gas and then emit extra light at certain wavelengths • Given off by nebulas, comets, and certain star types
Absorption Spectra Absorptions lines occur when gases remove (absorb) wavelengths of light. These gases are naturally present in the outer layer of Earths atmosphere, scientists can also create these lines in a lab. the fraction of incidental radiation absorbed by the material over a range of frequencies. Radiation is more likely to be absorbed at frequencies that match the energy difference between two quantum mechanical states of the molecules. First Noticed by William Wollaston in 1802.
Outer layer is cooler, absorbs Photons photons ThenYouSeeThis Photosphere
