CAITLIN CAMPBELL Spectral Lines

Spectrometer Instrument used to measure properties of light of the electromagnetic spectrum Enters through optical fiber, spectrometer refracts incoming light splitting into component wavelengths and records intensity with a detector Oceans Optics USB-4000 Spectrometer 350 nm to 1050 nm

Hydrogen Spectrum Balmer Series nm nm Transitions to n=2

Red Laser Helium Neon Laser nm

Mercury lamp nm (blue) nm (green) pair at nm and nm (yellow-orange)

Blackbody Radiation Spectrum depends only on bodys temperature Shifts with increasing/decreasing temperature Have a maximum wavelength of emission related to their temperature Maximum about 655 nm so temperature about 4424 K Weins Displacement Law

Flashlight (Tungsten)

Natural Sunlight

Suns temperature about 5800 K so using Weins Displacement Law maximum wavelength should be about 500 nm

Fraunhofer Lines Dark lines in solar spectrum are due to absorption by elements in the atmosphere nm Hydrogen nm Magnesium or Iron / nm Potassium 759 nm Oxygen Line spectrum corresponds to the emission of photons from transitions from a higher state to a lower state of energy Atmosphere absorbs frequencies associated to the spectral lines of the elements it is formed of

Monitor Use RGB pixels Additive color model Eyes read as one color Used in electronic systems like computers and televisions

RGB Pixels Red nm Green nm Blue nm

Blue Green

Uncertainties Noise from overhead light and other sources in room Age of lamps Spectrometer has 1 nm uncertainty approximately

Summary Elements spectral lines are like fingerprints

THANK YOU! Questions?