Upload
roscoe
View
64
Download
0
Embed Size (px)
DESCRIPTION
5. The Nature of Light. Light travels in vacuum at 3.0 . 10 8 m/s Light is one form of electromagnetic radiation Continuous radiation: Based on temperature Wien ’ s Law & the Stefan-Boltzmann Law Light has both wave & particle properties Each element has unique spectral lines - PowerPoint PPT Presentation
Citation preview
5. The Nature of Light• Light travels in vacuum at 3.0 . 108 m/s• Light is one form of electromagnetic radiation• Continuous radiation: Based on temperature• Wien’s Law & the Stefan-Boltzmann Law• Light has both wave & particle properties• Each element has unique spectral lines• Atoms: A nucleus surrounded by electrons• Spectral lines: Electrons change energy levels• Spectral lines shift wavelength due to motion
Does Light Travel Infinitely Fast?• Some ancient common experiences
– Lightning & thunder• At minimum, light travels faster than easily
measured• At maximum, light might travel infinitely fast
– Galileo’s experiments• Human reflexes are much too slow• Human pulse is much too long
• Olaus Rømer 1676– Inconsistencies in occultations of Jupiter’s moons
• Earlier than expected with Jupiter closer than average• Later than expected with Jupiter farther than average
EMR Travels At Finite Speed
Occultation
Occultation
Light Moves in Vacuum 3.0 . 108 m/s• Light travels at constant speed in vacuum
– Recognized by Einstein as highest possible speed– Independent of the speed of any observer– That speed is…c…and is… “celeritas”
c = 3.0 . 105 km/sc = 3.0 . 108 m/sc = 3.0 . 1010 cm/s
• Light travels different speeds in different media– Air slows light a little Low density
• Light bends/refracts a little as it enters the atmosphere
– Glass slows light a lot High density• Light bends/refracts a lot as it enters a telescope
lens
“Light” is Electromagnetic Radiation• “Light” is one form of electromagnetic radiation
– Electric & magnetic components are sine waves• Electric & magnetic components identical wavelengths• Electric & magnetic components perfectly synchronized
• Various regions electromagnetic radiation– R Radio Longest λ’s Low energies– I Infrared– V Visible “Light” Medium
energies– U Ultraviolet– X X-ray– G Gamma-ray Shortest λ’s High energies
EMR: Electric & Magnetic Waves
• Wave properties– Electric vector vibrates in a sine wave form
vibrates in a single plane– Magnetic vector vibrates in a sine wave form
vibrates perpendicular to e– vectorvibrates synchronized w/e– vector
Refraction of Sunlight By a PrismThe “Celebrated Phenomenon of Colours”
Red light isrefracted least
Blue light isrefracted most
Prisms Do Not Add Color to Light
• Newton’s prism experiments– Isolate one color from sunlight using one prism– Pass that color through a second prism
• No color is added
The Electromagnetic Spectrum
Emission & Absorption Spectra• Emission spectra Bright = Hot
Looking directly at a hot high-density object– Continuous Hot high-density objects
• Hot stars with no intervening interstellar gas clouds– Bright-line Hot low-density objects
• Hot interstellar gas clouds between any star & the Earth
• Absorption spectra Dark = ColdNot looking directly at a hot high-density object– Dark-line Cool low-density objects
• Cool interstellar gas clouds
Continuous and Line SpectraAbsorption from a coollow density object
Emission from a hot Emission from a hothigh density object low density object
=+
The Blackbody Concept• Blackbody: An ideal concept
– Absorbs 100% of all wavelengths of incident EMR• All X-rays, visible light, radio waves…• Experience shows that this is impossible
– Emits all absorbed energy as blackbody radiation• Radiation based exclusively on Kelvin temperature• Experience shows that this actually happens
• Wien’s Law– Wavelength at which the most energy is produced
• Stefan-Boltzmann Law– Total energy is proportional to T4
Blackbody Curve: The Ideal
“White” stars
Our Sun
“Red” stars
Blackbody Curve: The Sun
Wien’s Law• Blackbody radiation curves have one peak
– This wavelength emits the most energy– This wavelength depends on Kelvin temperature
lmax = Wavelength of maximum emission(meters)
T = Temperature (kelvins)
• lmax is inversely proportional to Kelvin temp.– Higher temperature Shorter wavelength
The Stefan-Boltzmann Law• Blackbody radiation curves show energy flux
– This energy flux depends on Kelvin temperature
F = Energy flux (joules . m–2 . sec–1 )s = Constant = 5.67 . 10–8 W . m–2 .
K–4
TK = Temperature (kelvins)
• Energy is directly proportional to TK4
– Raising TK by a factor of 10 raises energy by 10,000
The Wave-Particle Nature of EMR• EMR behavior depends on the experiment
– Wave experiment: EMR behaves like a wave• Young’s double-slit experiment
– Particle experiment: EMR behaves like a particle• EMR as photons
– A quantum amount of EMR energy– Energy = Planck’s Constant . Frequency
• The photoelectric effect– Electron emission requires some minimum energy
• Possible only if photons actually exist
Each Element Has a Unique Spectrum• Every material has a unique spectral signature
– Unique set of spectral lines• When hot, the spectral lines are bright• When cool, the spectral lines are dark
– Each spectral line has a unique l Spectroscopy– Each spectral line emits a unique amount of energy
• Kirchhoff’s Laws– Hot opaque objects: Continuous spectra
• Classical blackbody radiation– Hot transparent objects: Bright-line spectra
• Hot interstellar gas clouds with no continuous background– Cool transparent objects: Dark-line spectra
• Cool interstellar gas clouds with a continuous background
The Periodic Table of the Elements
Spectra: The Hydrogen Family
Spectra: The Helium Family
Spectra: The Beryllium Family
Spectra: The Boron Family
Spectra: The Carbon Family
Spectra: The Nitrogen Family
Spectra: The Oxygen Family
Spectra: The Fluorine Family
The Bohr Model of the Atom• A central nucleus
– One or more protons Atomic number• Determines the chemical properties (elements)
– Zero or more neutrons Mass number• Determines the nuclear properties (isotopes)
• Electron orbitals surround the nucleus– Neutral atoms: Number of p+ = Number of e–
– Ionized atoms: Number of p+ ≠ Number of e–
• Cations: One or more e– lost Net positive charge
• Anions: One or more e– gained Net negative charge
Bohr Model of the Hydrogen Atom
Electron orbitals are not to scale
Hydrogen Electron Transitions
Electrons Jump Energy Levels• Electrons jumping energy levels produce lines
– Hydrogen atom is the simplest of all• Lyman series: Ultraviolet
spectrum• Balmer series: Visible
spectrum• Paschen series: Infrared
spectrum– All other atoms & elements are more complicated
• More considerations about spectral lines– Each line has a different amount of energy
• Energy = Planck’s constant . Frequency– Each line has a different probability of jumping
• More jumps More energy emitted Brighter lines
Spectra: Hydrogen Energy Levels
The Doppler Effect• Effect Wavelength shift due to relative motion
– Source & viewer moving closer Blue shift• Spectral lines shifted toward blue end of the spectrum
– The spectral lines do not actually appear blue ! ! !– Source & viewer moving farther Red shift
• Spectral lines shifted toward red end of the spectrum– The spectral lines do not actually appear red ! ! !
• Cause Relative motion of source & observer– Source & viewer moving closer
• Waves compressed Shorter wavelength Blue shift– Source & viewer moving farther
• Waves stretched Longer wavelength Red shift
Doppler Shift: Stretching Waves
Compressed wavelengths Stretched wavelengthsHigher frequencies Lower frequenciesShift toward blue Shift toward red
• Light in vacuum at constant speed– 3.0 . 108 m . sec–2
• Light in other media moves slower– Related generally to media density
• Light is one form of EMR– Gamma rays– X-rays– Ultraviolet– Visible– Infrared– Microwave / Radio
• Emission & absorption spectra– Continuous Hot high
density– Bright line Hot low
density– Dark line Cool low
density• Blackbody concept
– Absorbs 100% of all wavelengths– Emits 100% at specific wavelengths
• Wien’s Law– Wavelength of maximum energy
• Stefan-Boltzmann Law– Total energy produced
• Wave-particle duality of all EMR– Behavior depends on experiment– Photoelectric effect
• Unique sets of spectral lines– Kirchhoff’s three laws
• Bohr’s mode of hydrogen– Nucleus with orbitals– Neutral & ionized atoms– Electron energy jumps produce lines
• Doppler effect– Relative convergence: Blue shift– Relative divergence: Red shift
Important Concepts