Stellar Astrophysics: The Interaction of Light and Matter
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1 Stellar Astrophysics: The Interaction of Light and Matter
2 The Photoelectric Effect Methods of electron emission Thermionic emission: Application of heat allows electrons to gain enough energy to escape Secondary emission: The electron gains enough energy by transfer from another high-speed particle that strikes the material from outside Field emission: A strong external electric field pulls the electron out of the material Photoelectric effect: Incident light (electromagnetic radiation) shining on the material transfers energy to the electrons, allowing them to escape
3 The Photoelectric Effect Electromagnetic radiation interacts with electrons within metals and gives the electrons increased kinetic energy Light can give electrons enough extra kinetic energy to allow them to escape The ejected electrons are called photoelectrons The minimum extra kinetic energy which allows escape is called the work function φ of the material
4 Experimental Setup Minimum voltage for which I = 0 is called stopping potential V 0
5 Experimental Results The kinetic energies of the photoelectrons are independent of the light intensity The maximum kinetic energy of the photoelectrons, for a given emitting material, depends only on the frequency of the light The smaller the work function φ of the emitter material, the smaller is the threshold frequency of the light that can eject photoelectrons
6 Experimental Results When the photoelectrons are produced, however, their number is proportional to the intensity of light The photoelectrons are emitted almost instantly following illumination of the photocathode, independent of the intensity of the light
7 Einstein s Theory Einstein suggested that the electromagnetic radiation field is quantized into particles called photons Each photon has the energy quantum Albert Einstein ( ) E photon = h ν = h c λ where ν is the photon frequency and h is Planck s constant The photon travels at the speed of light in a vacuum, and its wavelength is given by c λ = ν
8 Einstein s Theory Conservation of energy yields h ν = φ + K electron Explicitly, the energy of the most energetic electrons is K max = h ν φ The retarding potentials measured in the photoelectric effect are the opposing potentials needed to stop the most energetic electrons e V 0 = K max
9 Quantum Interpretation The kinetic energy of the electron does not depend on the light intensity at all, but only on the light frequency and the work function of the material K max = e V 0 = h ν φ Einstein in 1905 predicted that the stopping potential was linearly proportional to the light frequency, with a slope h, the same constant found by Planck
10 The Compton Effect A photon impinging on a material will scatter from an atomic electron For high photon energies, we can neglect the binding energy and treat the collision as an elastic collision between the photon and electron For the photon energy we can write Arthur Compton ( ) E photon = h ν = h c λ = p c
11 The Compton Effect Scattering of photons off loosely bound atomic electron Conservation laws h ν i + m e c 2 = h ν f + ( p 2 e c 2 + (m e c 2 ) 2 ) 1/2 h / λ i = h / λ f cos θ + p e cos φ h / λ f sin θ = p e sin φ
12 The Compton Effect The scattering off the electron yields a change in wavelength of the scattered photon which is known as the Compton Effect Δ λ = λ f λ h I = ( 1 cos θ ) m e c = λ C ( 1 cos θ ) with Compton wavelength λ C = nm The radiation pressure discussed previously is caused by the Compton Effect
13 Line Spectra Chemical elements were observed to produce unique wavelengths of light when burned or excited in an electrical discharge Emitted light is passed through a diffraction grating with thousands of lines per cm and diffracted according to its wavelength λ by the equation d sinθ = n λ with n = 0, 1, 2, where d is the distance between grating lines
14 Balmer Series In 1885, Johann Balmer found an empirical formula for wavelengths of the visible hydrogen line spectrum 1 λ = R 1 H 4 1 n 2 Johann Balmer ( ) where n = 3,4,5 and R H = m -1 Rydberg constant
15 De Broglie Waves Prince Louis V. de Broglie suggested that massive particles should have wave properties similar to electromagnetic radiation He was guided by the relations for photons h ν = p c = p λ ν Similarly for photons, the wavelength and momentum are related λ = h / p The wavelength of the particle, deduced from its momentum, is called the de Broglie wavelength Louis de Broglie ( )
16 The Classical Atomic Model Let s consider atoms as a planetary model The force of attraction on the electron by the nucleus and Newton s second law give 1 4 π ε 0 e 2 r 2 = µ υ 2 r where υ is the tangential velocity of the electron and the reduced mass m µ = e m p m e + m p Can estimate υ, taking r = m υ m/s < 0.01 c
17 The Classical Atomic Model The total energy of the atom can be written as the sum of kinetic and potential energy E = K + U = 1 e π ε 0 r 4 π ε 0 e 2 r = 1 8 π ε 0 e 2 r
18 Problems with the Planetary Model From classical E&M, an accelerated electric charge radiates energy (electromagnetic radiation) So the total energy must decrease radius r must decrease Electron crashes into the nucleus in ~ 10-9 s!?
19 The Bohr Model of the Hydrogen Atom Bohr s assumptions Stationary states in which orbiting electrons do not radiate energy exist in atoms Emission/absorption of energy occurs along with atomic transition between two stationary states Δ E = E 1 - E 2 = h ν Classical laws of physics do not apply to transitions between stationary states The angular momentum of the atom in a stationary state is a multiple of h/2π L = n h 2 π n ћ n = principle quantum number Niels Bohr ( )
20 Bohr s Quantization Condition The electron is a standing wave in an orbit around the proton This standing wave will have nodes and be an integral number of wavelengths 2 π r = n λ = n The angular momentum becomes h p L = r p = n h 2 π = n ћ
21 Bohr Radius From L = n h 2 π n ћ and K = 8 π ε = 0 r e 2 µ υ 2 2 The radius of the hydrogen atom for stationary states is r n = = n 2 a 0 4 π ε 0 n 2 ћ 2 µ e 2 where the Bohr radius is a 0 = 4 π ε 0 ћ 2 µ e 2 = x 10 quantized orbit (position) The smallest radius of the hydrogen atom occurs when n = 1 This radius gives its lowest energy state (called the ground state of the atom) 10 m
22 The Hydrogen Atom The energies of the stationary states (with E 0 = 13.6 ev) e 2 e 2 E E n = = = 0 8 π ε 0 r n 8 π ε 0 a 0 n2 Emission of light occurs when the atom in an excited state decays to a lower energy state (n u n l ) h ν = E h E l where ν is the frequency of the photon n 2 1 λ ν E h E l 1 1 = = = R H n 2 c h c l n h 2 and R H the Rydberg constant
23 Transitions in the Hydrogen Atom Lyman series (invisible) The atom exists in the excited state for a short time before making a transition to a lower energy state with emission of a photon. At ordinary temperatures, almost all hydrogen atoms exist in n = 1 state. Absorption therefore gives the Lyman series. Balmer series (visible) When sunlight passes through the atmosphere, hydrogen atoms in water vapor absorb wavelengths of the Balmer series giving dark lines in the absorption spectrum.
24 Limitations of the Bohr Model The Bohr model was a great step for the new quantum theory, but it had its limitations. Works only for single-electron atoms Could not account for the intensities or the fine structure of the spectral lines Could not explain the binding of atoms into molecules
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