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Transcript
How to Make Starlight (part 1)
Chapter 7
Origin of light



Light (electromagnetic radiation) is
just a changing electric and
magnetic field.
Changing electric field (e.g., due to
acceleration of an electron)
generates electromagnetic radiation.
We discuss two major mechanisms:


Blackbody Radiation
Spectral Line Emission
Heat and Temperature
•Temperature refers to the degree of
agitation, or the speed with which
the particles move (T~v2).
•All atoms are vibrating unless at
absolute zero temperature (T = 0 K
= -459.7 F).
•Water freezes at 273 K and boils at
373 K.
•Heat refers to the amount of energy
stored in a body as agitation among
its particles and depends on density
as well as temperature.
Blackbody Spectrum
It is the spectrum that a
"perfect emitter" or a
"perfect absorber"
(roughly a very thick or
solid object) would
radiate. A black object is
the closest approximation
to a perfect absorber.
The Difference Between Black and
White




“White” light – contains all the frequencies of the
visible part of the spectrum.
White paint – diffusely scatters all frequencies of
the visible part of the spectrum equally.
Black paint – absorbs all frequencies of the
visible part of the spectrum equally.
“Blackbody” – emits and absorbs radiation over a
specific set of frequencies.
Discussion Question
Why does NASA paint spacecraft white?
80%
Absorption
Absorption Spectrum
of Black Paint
40%
Visible
Infrared
Absorption Spectrum
of White Paint
0%
Frequency
Hotter objects emit photons with a
higher average energy.

Wien’s Law
• The peak of the blackbody emission
spectrum is given by
max
2.9 10

nm
T(Kelvin)
6
Blackbody Radiation
The graph below shows the blackbody spectra of
three different stars. Which of the stars is at
the highest temperature?
1) Star A
2) Star B
3) Star C
Energy
per
Second
A
B
C
Wavelength
Hotter objects emit more total
radiation per unit surface area.
Cold
Hot
Stefan-Boltzmann Law:
Emitted power per square meter = σ T4
σ = 5.7 x 10-8 W/(m2K4)
You are gradually heating up a rock in
an oven to an extremely high
temperature. As it heats up, the rock
emits nearly perfect theoretical
blackbody radiation – meaning that it
1)
2)
3)
4)
is
is
is
is
brightest when hottest.
bluer when hotter.
both
neither
L=A T4
Campfires
Campfires are blue on the bottom, orange in the
middle, and red on top.
Which parts of the fire are the hottest? the coolest?
As atoms get hotter, they wiggle faster and collide to each
other harder ---> more light they emit and more wiggle per
second = frequency goes up = wavelength goes down. Thus
bluer.
Thus, as temperature goes up light gets stronger and gets
blue.
Blackbody Radiation (a.k.a.
Thermal Radiation)
• Every object with a temperature
greater than absolute zero emits
blackbody radiation.
• Hotter objects emit more total
radiation per unit surface area.
• Hotter objects emit photons with a
higher average energy.
How to Make Light (Part 2)

Structure of atoms

Energy levels and transitions

Emission and absorption lines

Light scattering
Atoms
Atoms are made of
electrons, protons, and
neutrons.
A Planetary Model of the Atom
The bounding force: the
attractive Coulomb
(electrical) force between
the positively charged
nucleus and the negatively
charged electrons.
Energy Levels
Electrons can be in
different orbits of certain
energies, called energy
levels.
Different atoms have
different energy levels, set
by quantum physics.
Quantum means discrete!
Excitation of Atoms
To change its energy levels,
an electron must either
absorb or emit a photon that
has the same amount of energy
as the difference between the
energy levels
E = h --- Larger energy
difference means higher
frequency.
Different jumps in energy
levels means different
frequencies of light absorbed.
Spectral Line Emission
If a photon of exactly
the right energy is
absorbed by an
electron in an atom,
the electron will gain
the energy of the
photon and jump to an
outer, higher energy
orbit.
A photon of the same energy is emitted when the
electron falls back down to its original orbit.
Spectral Line Emission
Collisions (like in a
hot gas) can also
provide electrons
with enough
energy to change
energy levels.
A photon of the same energy is emitted
when the electron falls back down to its
original orbit.
Energy Levels of a Hydrogen Atom
Different allowed
“orbits” or energy
levels in a hydrogen
atom.
Emission line spectrum
Absorption line spectrum
Spectral Lines of Some Elements
Argon
Helium
Mercury
Sodium
Neon
Spectral lines are like a cosmic barcode system for elements.
Atoms of different elements have unique
spectral lines because each element

has atoms of a unique color

has a unique set of neutrons

has a unique set of electron orbits

has unique photons
The Solar Spectrum
There are similar absorption lines in the other regions of
the electromagnetic spectrum. Each line exactly
corresponds to chemical elements in the stars.
Sources of spectral lines
Emission nebula
Reflection nebula
An Object’s Spectrum
Encoded in an object’s spectrum
is information about the emitter/absorber.
This is how we learn what the Universe
is made of!
Variability
(change with time)
There are three basic aspects of
the light from an object that
we can study from the Earth.
Intensity
(spatial distribution of the light)
Spectra
(composition of the object
and the object’s velocity)