PHYS 183 Lecture Notes - Lecture 12: Stellar Atmosphere, Photosphere, Orion Nebula
Document Summary
Phys 183 the milky way inside and out tracy webb. Each kind of atom has a unique set of energy levels. Each transition corresponds to a unique frequency, wavelength & energy. Electrons falling will emit certain amounts of energy which will emit certain amounts of light corresponding to a specific colour based on wavelength or frequency these are called chemical fingerprints they are different for every single element. Downward transitions give us emission lines electrons lose energy as they fall closer to the nucleus (similar to gravitational potential energy) Upward transitions give us absorption lines electrons gain energy as they move farther from nucleus: photons with exact energies are absorbed. Absorption and emission spectra are the opposite of each for the same element. Properties of thermal radiation: hotter objects emit more energy they are brighter, hotter objects emit photons with a higher average energy they are bluer. As you increase the energy of an object, it gets brighter & bluer.
