Introduction to Geochemistry
Introduction to Geochemistry Introduction to Geochemistry
How do we know? ! Red shift • Spectral lines emitted by distant galaxies (actually supernovae in galaxies) are shifted to the red by the Doppler Effect • 1929: Edwin Hubble measured redshifts of light from 18 galaxies in the Virgo cluster… calculated recessional velocities • Found that recessional velocity increases with distance • Doppler equation !/!’ = 1 + "/c Where !’ = wavelength of spectral line emitted by moving source ! = wavelength of same line emitted by stationary source c = speed of light " = recessional velocity
- Page 1 and 2: Introduction to Geochemistry ! Geoc
- Page 3: Origin of the Universe ! “Big Ban
- Page 7 and 8: Cosmic microwave radiation ! Discov
- Page 9 and 10: Wilkinson Microwave Anisotropy Prob
- Page 11 and 12: NASA's Spitzer Space Telescope •
- Page 13 and 14: ! Eagle Nebula - NGC 6611 - 6,500 l
- Page 16 and 17: Stellar Life Cycle ! Birth • Cont
- Page 19 and 20: Nearby Starforming Region: Orion Ne
- Page 21 and 22: Cosmic Abundances of the Elements U
- Page 23 and 24: Nucleosynthesis in the Sun & smalle
- Page 25 and 26: He Fusion in Red Giants ! Triple al
- Page 27 and 28: Fusion of Elements Heavier than Ni
How do we know?<br />
! Red shift<br />
• Spectral lines emitted by distant galaxies (actually supernovae in<br />
galaxies) are shifted <strong>to</strong> the red by the Doppler Effect<br />
• 1929: Edwin Hubble measured redshifts of light from 18 galaxies<br />
in the Virgo cluster… calculated recessional velocities<br />
• Found that recessional velocity increases with distance<br />
• Doppler equation<br />
!/!’ = 1 + "/c<br />
Where !’ = wavelength of spectral line emitted by moving source<br />
! = wavelength of same line emitted by stationary source<br />
c = speed of light<br />
" = recessional velocity
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