ASTRO 105 1st Edition Lecture 5Current LectureStefan – Boltzmann Law F=σT4 F=flux=watts/meter2T=temp (k) Flux α temp4Planck’s LawE photon = energy of a photon (joules) E photon = hc/λh= Planck’s constant6.63x10-34c = speed of light 3x108 m/sλ= wavelength of a photon (m)Spectra - When heat a pure element, produce light- Colors=wavelength=frequency - Once we know color, we know composition - Hot material emission spectra (only certain colors)- Cold material absorption spectra (dark bands)Spectroscopy - Analysis of lighto What colors are emitted or absorbed These notes represent a detailed interpretation of the professor’s lecture. GradeBuddy is best used as a supplement to your own notes, not as a substitute.Modern Theory of the Atom compliments of Niels Bohr (around 1920)- Energy is conserved - Photons have energy - Electron loses energy (drops down) = photon Carries energy away - Spectra only particular wavelengths- Electron has much larger waves than the proton - Electron can exist at only certain energy levels (also known as orbits Bohr’s Law1 = R( 1 – 1λ n2 n2 ) λ= wavelength of the photonR= Rydberg constant=1.1 x 107 1/mn= smaller orbit #N= larger orbit # Doppler Shif- Blue shift light source towards us - Red shift light source away from
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