Transcript CHAPTER 9: Statistical Physics
CHAPTER 9
Statistical Physics
9.1 Historical Overview 9.2 Maxwell Velocity Distribution 9.3 Equipartition Theorem 9.4 Maxwell Speed Distribution 9.5 Classical and Quantum Statistics 9.6 Fermi-Dirac Statistics 9.7 Bose-Einstein Statistics
Ludwig Boltzmann, who spent much of his life studying statistical mechanics, died in 1906 by his own hand. Paul Ehrenfest, carrying on his work, died similarly in 1933. Now it is our turn to study statistical mechanics. Perhaps it will be wise to approach the subject cautiously.
- David L. Goldstein (
States of Matter
, Mineola, New York: Dover, 1985)
9.1: Historical Overview
Statistics and probability
New mathematical methods developed to understand the Newtonian physics through the eighteenth and nineteenth centuries.
Lagrange
around 1790 and
Hamilton
around 1840. They added significantly to the computational power of Newtonian mechanics.
Pierre-Simon de Laplace
(1749-1827) Made major contributions to the theory of probability.
Historical Overview
Benjamin Thompson (Count Rumford)
Put forward the idea of heat as merely the motion of individual particles in a substance.
James Prescott Joule
Demonstrated the mechanical equivalence of heat.
James Clark Maxwell
Brought the mathematical theories of probability and statistics to bear on the physical thermodynamics problems.
Showed that distributions of an ideal gas can be used to derive the observed macroscopic phenomena.
His electromagnetic theory succeeded to the statistical view of thermodynamics.
Historical Overview
Einstein
Published a theory of Brownian motion, a theory that supported the view that atoms are real.
Bohr
Developed atomic and quantum theory.
9.2: Maxwell Velocity Distribution
There are six parameters —the position (
x
,
y
,
z
) and the velocity (
v x
,
v y
,
v z
) —per molecule to know the position and instantaneous velocity of an ideal gas.
These parameters six-dimensional
phase space
The velocity components of the molecules are more important than positions, because the energy of a gas should depend only on the velocities.
Define a
velocity distribution function
.
= the probability of finding a particle with velocity between .
where
Maxwell Velocity Distribution
Maxwell proved that the probability distribution function is proportional to exp( −½
mv
2 /
kT
).
Therefore .
where
C
is a proportionality factor and
β
≡ (
kT
) −1 . Because
v
2 =
v x
2 +
v y
2 +
v z
2 then Rewrite this as the product of three factors.
Maxwell Velocity Distribution
g
(
v x
)
dv x
is the probability that the molecule’s velocity lies between
v x x
component of a gas and
v x
+
dv x
.
if we integrate
g
(
v x
)
dv x
over all of
v x
, it equals to 1.
then The mean value of
v x
Maxwell Velocity Distribution
The mean value of
v x
2 The velocity component distributes around the peak at
v x
= 0 at
Maxwell Velocity Distribution
The results for the
x
,
y
, and
z
velocity components are identical.
The mean translational kinetic energy of a molecule: Purely statistical considerations is good evidence of the validity of this statistical approach to thermodynamics.
9.3: Equipartition Theorem
Think of oxygen molecule as two oxygen atoms connected by a massless spring.
How much rotational /vibrational energy is there and how is it related to temperature?
Equipartition Theorem
:
In equilibrium a mean energy of ½ kT per molecule is associated with each independent quadratic term in the molecule’s momentum square and position square.
Each independent phase space coordinate:
degree of freedom
Equipartition Theorem
In a monatomic ideal gas, each molecule has There are three degrees of freedom.
Mean kinetic energy is 3(1/2
kT
) = 3/2
kT
.
In a gas of
N
helium molecules, the total internal energy is The heat capacity at constant volume is
C
V = 3/2
Nk
.
For the heat capacity for 1 mole, The ideal gas constant
R
= 8.31 J/K.
The Rigid Rotator Model
For diatomic gases, consider the rigid rotator model.
The molecule rotates about either the
x
or
y
axis.
The corresponding rotational energies are ½
I x ω x
2 and ½
I y ω y
2 .
There are five degrees of freedom (three translational and two rotational).
Equipartition Theorem
In some circumstances it is better to think of atoms connected to each other by a massless spring.
The vibrational kinetic energy is ½
m
(
dr
/
dt
) 2 energy ½ kx 2 plus the potential There are seven degrees of freedom (three translational, two rotational, and two vibrational).
Molar Heat Capacity
The heat capacities of diatomic gases are temperature dependent, indicating that the different degrees of freedom are “turned on” at different temperatures.
Example of H 2
9.4: Maxwell Speed Distribution
Maxwell velocity distribution
: Where It is useful to turn this into a
speed distribution
.
F
(
v
)
dv
= the probability of finding a particle with speed between
v
and
v
+
dv
.
Maxwell Speed Distribution
Suppose some distribution of particles
f
(
x
,
y
,
z
) exists in normal three-dimensional (
x
,
y
,
z
) space.
The distance of the particles at the point (
x
,
y
,
z
) to the origin is the probability of finding a particle between .
Maxwell Speed Distribution
Radial distribution
F
(
r
).
F
(
r
)
dr
= the probability of finding a particle between
r
+
dr
.
The volume of the spherical shell is 4
πr
2
dr
. replace the coordinates
x
,
y
, and
z
with the velocity space coordinates
v x
,
v y
, and
v z
.
Maxwell speed distribution
: It is only valid in the classical limit.
Maxwell Speed Distribution
The most probable speed
v
*, the mean speed , and the root mean-square speed
v
rms are all different.
Maxwell Speed Distribution
Most probable speed (at the peak of the speed distribution): Mean speed (average of all speeds): Root-mean-square speed (associated with the mean kinetic energy): Standard deviation of the molecular speeds:
σ v
in proportion to .
9.5: Classical and Quantum Statistics
If molecules, atoms, or subatomic particles are in the liquid or solid state, the Pauli exclusion principle prevents two particles with identical wave functions from sharing the same space.
There is no restriction on particle energies in classical physics. There are only certain energy values allowed in quantum systems.
Classical Distributions
Rewrite Maxwell speed distribution in terms of energy.
For a monatomic gas the energy is all translational kinetic energy. where
Classical Distributions
Boltzmann showed that the statistical factor exp( −
βE
) is a characteristic of any classical system.
quantities other than molecular speeds may affect the energy of a given state.
Maxwell-Boltzmann factor
for classical system: The energy distribution for classical system:
n
(
E
)
dE
= the number of particles with energies between
E
+
dE
.
g
(
E
) = the density of states, is the number of states available per unit energy range.
F
MB tells the relative probability that an energy state is occupied at a given temperature.
Quantum Distributions
Characteristic of indistinguishability that makes quantum statistics different from classical statistics.
The possible configurations for distinguishable particles in either of two energy states:
State 1
AB A B
State 2
B A AB The probability of each is one-fourth (0.25).
Quantum Distributions
If the two particles are indistinguishable:
State 1
XX X
State 2
X XX The probability of each is one-third (~0.33).
Because some particles do not obey the Pauli exclusion principle, two kinds of quantum distributions are needed.
Fermions
: Particles with half-spins obey the Pauli principle.
Bosons
: Particles with zero or integer spins do not obey the Pauli principle.
Quantum Distributions
Fermi-Dirac
distribution: where
Bose-Einstein
distribution: Where Both distributions reduce to the classical Maxwell-Boltzmann distribution when
B i
exp(
βE
) is much greater than 1.
the Maxwell-Boltzmann factor
A
exp( −
βE
) is much less than 1.
Quantum Distributions
The normalization constants for the distributions depend on the physical system being considered.
Because bosons do not obey the Pauli exclusion principle, more bosons can fill lower energy states.
Three graphs coincide at high energies – the classical limit.
Maxwell-Boltzmann statistics may be used in the classical limit.
Classical and Quantum Distributions
9.6: Fermi-Dirac Statistics
E
F is called the
Fermi energy
.
When
E
=
E
F , the exponential term is 1.
F
FD = ½ In the limit as T → 0, At
T
= 0, fermions occupy the lowest energy levels.
Near
T
= 0, there is little chance that thermal agitation will kick a fermion to an energy greater than
E
F .
Fermi-Dirac Statistics
T
= 0
T
> 0 As the temperature increases from
T
= 0, the Fermi Dirac factor “smears out”.
Fermi temperature
, defined as
T
F ≡
E
F /
k
.
.
T
=
T
F
T
>>
T
F When
T
>>
T
F ,
F
FD approaches a decaying exponential.
Classical Theory of Electrical Conduction
Paul Drude (1900) showed that the current in a conductor should be linearly proportional to the applied electric field that is consistent with Ohm’s law.
Prediction of the electrical conductivity: The electrical resistivity ρ (
rho
) is
Mean free path
is Thus: .
Classical Theory of Electrical Conduction
According to the Drude model, the conductivity should be proportional to
T
−1/2 .
But for most conductors is very nearly proportional to
T
−1 .
The heat capacity of the electron gas is (9/2)
R
.
This is not consistent with experimental results.
Quantum Theory of Electrical Conduction
The allowed energies for electrons are E=p 2 /2m = h 2 k 2 /8 p 2 m Rewrite this as
E
=
r
2
E
1 The parameter
r
is the “radius” of a sphere in phase space. The volume is (4/3)
πr
3 .
The exact number of states up to radius
r
is .
Quantum Theory of Electrical Conduction
Rewrite as a function of
E
: At
T
level.
= 0, the Fermi energy is the energy of the highest occupied Total of electrons Solve for
E
F : The density of states with respect to energy in terms of
E
F : d
N
r /d
E
=
Quantum Theory of Electrical Conduction
At
T
= 0, The mean electronic energy: Internal energy of the system : Only those electrons within about
kT
of
E
F will be able to absorb thermal energy and jump to a higher state. Therefore the fraction of electrons capable of participating in this thermal process is on the order of
kT
/
E
F .
Quantum Theory of Electrical Conduction
In general, Where
α
is a constant > 1.
The exact number of electrons depends on temperature.
Heat capacity is Molar heat capacity is
Quantum Theory of Electrical Conduction
Arnold Sommerfield used correct distribution
n
(
E
) at room temperature and found a value for
α
of
π
2 / 4. With the value
T
F = 80,000 K for copper, we obtain
c
V ≈ 0.02
R
, which is consistent with the experimental value! Quantum theory has proved to be a success.
Replace mean speed in Eq (9,37) by Fermi speed u F from
E
F = ½
u
F 2 .
defined Conducting electrons are loosely bound to their atoms.
these electrons must be at the high energy level.
at room temperature the highest energy level is close to the Fermi energy.
We should use
Quantum Theory of Electrical Conduction
Drude thought that the mean free path could be no more than several tenths of a nanometer, but it was longer than his estimation.
Einstein calculated the value of ℓ copper at room temperature.
to be on the order of 40 nm in The conductivity is
9.7: Bose-Einstein Statistics
Blackbody Radiation
Intensity of the emitted radiation is Use the Bose-Einstein distribution because photons are bosons with spin 1.
For a free particle in terms of momentum: The energy of a photon is
pc
, so
Bose-Einstein Statistics
The number of allowed energy states within “radius”
r
is Where 1/8 comes from the restriction to positive values of
n i
from the fact that there are two possible photon polarizations.
and 2 comes Energy is proportional to
r
, The density of states
g
(
E
) is The Bose-Einstein factor:
Bose-Einstein Statistics
Convert from a number distribution to an energy density distribution
u
(
E
).
For all photons in the range
E
to
E
+
dE
Using
E
=
hc
and |
dE
| = (
hc
/ λ 2 )
d
λ In the SI system, multiplying by
c
/4 is required.
Liquid Helium
Has the lowest boiling point of any element (4.2 K at 1 atmosphere pressure) and has no solid phase at normal pressure. The density of liquid helium
s
a function of temperature.
Liquid Helium
The specific heat of liquid helium as a function of temperature The temperature at about 2.17 K is referred to as the
critical temperature
(
T
c ),
transition temperature
, or
lambda point
.
As the temperature is reduced from 4.2 K toward the lambda point, the liquid boils vigorously. At 2.17 K the boiling suddenly stops.
What happens at 2.17 K is a transition from the
normal phase
to the
superfluid phase
.
Liquid Helium
The rate of flow increases dramatically as the temperature is reduced because the superfluid has a low viscosity.
Creeping film
– formed when the viscosity is very low.
Liquid Helium
Liquid helium below the lambda point is part superfluid and part normal.
As the temperature approaches absolute zero, the superfluid approaches 100% superfluid.
The fraction of helium atoms in the superfluid state: Superfluid liquid helium is referred to as a
Bose-Einstein condensation
.
not subject to the Pauli exclusion principle all particles are in the same quantum state
Density of the States
The allowed energies for particles are E=p 2 /2m = h 2 k 2 /8 p 2 m The parameter
r
is the “radius” of a sphere in phase space. The volume is (4/3)
πr
3 .
The exact number of states up to radius
r
is . d
N
r /d
E
= d{1/3( p (8mL 2 /h 2 ) 3/2 )E 3/2 }/dE
Liquid Helium
Such a condensation process is not possible with fermions because fermions must “stack up” into their energy states, no more than two per energy state.
4 He isotope is a fermion and superfluid mechanism is radically different than the Bose-Einstein condensation.
For Helium:
Liquid Helium
m
is the mass of a helium atom.
The number distribution
n
(
E
) is now In a collection of
N
helium atoms the normalization condition is
+ N(E=0) + N(E=0)
Substituting
u
=
E
/
kT
,
+ N(E=0)
Liquid Helium
When we are close to the condensation we have
B
2 = 1; this result corresponds to the number of
molecules in the excited states
:
e =
Rearrange this,
=
The result is
T
The value 3.06 K is an estimate of
T c
.
Bose-Einstein Condensation in Gases
By the strong Coulomb interaction among gas particles it was difficult to obtain the low temperatures and high densities needed to produce the condensate. Finally success was achieved in 1995.
First, they used laser cooling to cool their gas of 87 Rb atoms to about 1 mK. Then they used a magnetic trap to cool the gas to about 20 nK. In their magnetic trap they drove away atoms with higher speeds and further from the center. What remained was an extremely cold, dense cloud at about 170 nK.