Astr. 101 Notes 4

Astr. 101 Notes 4 - -light flux from Sun-luminosity (total...

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-light flux from Sun-luminosity (total energy, over all colors, in all directions), flux (energy through a specific surface area, luminosity/4pier^2); Stephan Boltzman Law 1879 (flux from a blackbody is F=sigmaT^4 -Sun’s spectral lines-German optician Josef von Fraunhofer, 1814, magnified sunlight broken into colors by a prism and discovered dark lines -spectroscopes-refraction (Snell’s Law-change in angle depends on wavelength = color) and diffraction (angle for waves to add depends on wavelength = color) -chemical fingerprints-mid 1850s Gustav Kirchhoff and Robert Bunsen discovered emission lines in lab -types of spectra-1860s Kirchoff’s laws -continuous spectrum-blackbody emits light at all wavelengths -absorption line spectrum-atoms in gas cloud absorb light of certain specific wavelengths, producing dark lines in spectrum -emission line spectrum-atoms in gas cloud remit something -atomic structure-1910 Ernest Rutherford, physicist from New Zealand, beamed helium nuclei through a thin gold foil and discovered matter is mostly empty space -Bohr Model (electron “orbits”)-1913 Neils Bohr, found a simple relationship b/w electrons in a hydrogen atom and the colors of the hydrogen spectrum, if electrons were restricted to specific “orbits” and thus energies -modern view (electron clouds)-quantum mechanics, developed in 1920s, explains why electrons can only
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This note was uploaded on 05/13/2011 for the course ASTR 101 taught by Professor Christiansen during the Spring '08 term at UNC.

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Astr. 101 Notes 4 - -light flux from Sun-luminosity (total...

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