Successfully reported this slideshow.
We use your LinkedIn profile and activity data to personalize ads and to show you more relevant ads. You can change your ad preferences anytime.

Optional spectra slides

516 views

Published on

Published in: Education
  • Be the first to comment

  • Be the first to like this

Optional spectra slides

  1. 1. Spectra<br />
  2. 2. Newton – split sunlight<br />Actually sunlight is not continuous – there are missing wavelengths<br />-- Fraunhofer lines – explanation will relate to the info in this chapter<br />
  3. 3. Chemists split light by using prisms or diffraction gratings<br />You can look at the spectral lines of fluorescent light bulbs by using a “CD” – the lines on the CD are comparable to a diffraction grating<br />
  4. 4. Flame tests aand spectra tubes<br />
  5. 5. Pg 136<br />Spectra<br />White light – continuous spectrum<br />Heated matter also continuous<br />1879<br />http://members.misty.com/don/bulb1.html#vvg<br />
  6. 6. Spectra of gaseous atoms – not continuous<br />Light from fluorescent bulb reflected<br />Off CD - NOT conintuous<br />Mercury vapor<br />uncoated<br />Buying light bulbs<br />
  7. 7. Color related to temperatureFluorescent bulbs – color rated by temp<br />3000K Kitchen/bath<br />4200 K cool white<br />5000K sunshine<br />6500 K Daylight<br />Higher temp – more blue – more balanced<br />Lower temperatures, less blue – more “yellowish”<br />GE black light 368 nm<br />
  8. 8.
  9. 9. Hydrogen spectra lines<br />Light separated by prism or <br />Diffraction grating<br />
  10. 10. Explanation of these spectral lines<br />H atom – <br />1 p 1e<br />Review Ch 2 sec 2, Atom video (WOC)<br />Thomson’s electron, Rutherford nuclear model<br />Bohr model of H atom – to explain spectra<br />Proton surrounded by electron<br />Electron revolve around proton <br />At specific distances <br />With specific energies<br />Can move from energy level to energy level<br />
  11. 11. Bohr MODEL<br />Thomson<br />Absorption<br />Emission<br />QM<br />Explanation of H spectral lines<br />

×