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9.24.07 Astronomy Notes

9.24.07 Astronomy Notes - state and when it drops back down...

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9.24.2007 – Astronomy Why are there no green stars? - When we get the same amount of all the colors, we see white Color progression of stars: R O Y-W W B-W B Spectroscopy - Continuous (blackbody). Kirchhoff’s Laws 1. For a continuous spectrum: luminous solid or liquid, hot opaque gas 2. Emission line spectrum: hot or heated transparent gas 3. Absorption line spectrum: backlit cool transparent gas Astronomical applications: - Compositions - Temperature Atomic Structure Bohr Model: - Proton/neutron nucleus, electrons in orbits - In excited state, electron is farther from protons - Wave-particle duality - Constructive/destructive interference explain stable orbits o If circumference of orbit is integer multiple of electron wavelength, it can be stable If an electron in the ground state absorbs a photon at the right wavelength, it will jump to the first
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Unformatted text preview: state, and when it drops back down it will release the photon at a specific wavelength It can also go to the second excited state, which could result in two different spectra E ~ frequency (nu) For light, the constant of proportionality = Planck’s constant (h) Jumps in energy are organized into series: JUST FOR HYDROGEN-Lyman series (ultraviolent) – jumps from ground state. o 122 nm, 103, 97.3, 95, 93.8 (shorter wavelengths, higher frequency, higher energy)-Balmer series (visible) – things already in the first excited state o 656 nm, 486, 434, 410-Paschen series (infrared) – second excited state? o 1875 nm, 1282, 1094...
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