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Statistical Thermodynamics
K.S .Rao for B.Sc III Sem Physics
Contents
1. Introduction
2. Distribution of Molecular States
3. Interacting Systems – Gibbs Ensemble
4. Classical Statistical Mechanics
1. Introduction
Mechanics : Study of position, velocity, force and
energy
Classical Mechanics (Molecular Mechanics)
• Molecules (or molecular segments) are treated as rigid object
(point, sphere, cube,...)
• Newton’s law of motion
Quantum Mechanics
• Molecules are composed of electrons, nuclei, ...
• Schrodinger’s equation Wave function
1. Introduction
Methodology of Thermodynamics and Statistical Mechanics
Thermodynamics
• study of the relationships between macroscopic properties
– Volume, pressure, compressibility, …
Statistical Mechanics (Statistical Thermodynamics)
• how the various macroscopic properties arise as a consequence of the microscopic nature of
the system
– Position and momenta of individual molecules (mechanical variables)
Statistical Thermodynamics (or Statistical Mechanics) is a link between microscopic
properties and bulk (macroscopic) properties
Methods of QM
Methods of MM
A particular
microscopic model
can be usedr
U
P T V
Statistical
Mechanics
Pure mechanical variablesThermodynamic Variables
1.Introduction
Equilibrium Macroscopic Properties
Properties are consequence of average of individual
molecules
Properties are invariant with time Time average
Mechanical
Properties of
Individual
Molecules
position, velocity
energy, ...
Thermodynamic
Properties
temperature, pressure
internal energy, enthalpy,...
average
over molecules
average
over time
statistical
thermodynamics
2 3 4
1. Introduction
Description of States
Macrostates : T, P, V, … (fewer variables)
Microstates : position, momentum of each particles (~1023 variables)
Fundamental methodology of statistical mechanics
Probabilistic approach : statistical average
• Most probable value
Is it reasonable ?
• As N approaches very large number, then fluctuations are negligible
• “Central Limit Theorem” (from statistics)
• Deviation ~1/N0.5
2. Distribution of Molecular States
Statistical Distribution
n : number of occurrences
b : a property
b
ni
1 2 3 4 5 6
if we know “distribution”
we can calculate the average
value of the property b
2. Distribution of Molecular States
Normalized Distribution Function
Probability Distribution Function
b
Pi
b1 b5b4b3b2 b6
i
ii
i
ii
iiiiii
bP
bn
bn
n
bnbP
1)(
)(
)()()(
i
ii
i
ii
PbFbF
Pbb
)()(
Finding probability (distribution) function is
the main task in statistical thermodynamics
2. Distribution of Molecular States
Quantum theory says ,
Each molecules can have only discrete values of energies
Evidence
Black-body radiation
Planck distribution
Heat capacities
Atomic and molecular spectra
Wave-Particle duality
Energy
Levels
2. Distribution of Molecular States
Configuration ....
At any instance, there may be no molecules at e0 , n1
molecules at e1 , n2 molecules at e2 , …
{n0 , n1 , n2 …} configuration
e0
e2
e1
e3
e4
e5
{ 3,2,2,1,0,0}
2. Distribution of Molecular States
Weight ....
Each configurations can be achieved in different ways
Example1 : {3,0} configuration 1
Example2 : {2,1} configuration 3
e0
e1
e0
e1 e
0
e1 e
0
e1
2. Distribution of Molecular States
Calculation of Weight ....
Weight (W) : number of ways that a configuration can be achieved in
different ways
General formula for the weight of {n0 , n1 , n2 …} configuration
i
in
N
nnn
NW
!
!
!...!!
!
321
Example1
{1,0,3,5,10,1} of 20 objects
W = 9.31E8
Example 2
{0,1,5,0,8,0,3,2,1} of 20 objects
W = 4.19 E10
Principles of Equal a Priori Probability
All distributions of energy are equally probable
If E = 5 and N = 5 then
0
1
2
3
4
5
0
1
2
3
4
5
0
1
2
3
4
5
All configurations have equal probability, but
possible number of way (weight) is different.
A Dominating Configuration
For large number of molecules and large number of energy
levels, there is a dominating configuration.
The weight of the dominating configuration is much more
larger than the other configurations.
Configurations
Wi
{ni}
Dominating Configuration
0
1
2
3
4
5
0
1
2
3
4
5
0
1
2
3
4
5
W = 1 (5!/5!) W = 20 (5!/3!) W = 5 (5!/4!)
Difference in W becomes larger when N is increased !
In molecular systems (N~1023) considering the
most dominant configuration is enough for average
How to find most dominant
configuration ?
The Boltzmann Distribution
Task : Find the dominant configuration for given N and
total energy E
Method : Find maximum value of W which satisfies,
i
ii
i
i
nE
nN
e 0
0
i
ii
i
i
dn
dn
e
Stirling's approximation
A useful formula when dealing with factorials of
large numbers.
NNNN ln!ln
i
i
i
i
ii
i
i
i
i
nnNN
nnnNNN
nNnnn
NW
lnln
lnln
!ln!ln!...!!
!lnln
321
Method of Undetermined
Multipliers
Maximum weight , W
Recall the method to find min, max of a function…
Method of undetermined multiplier :
Constraints should be multiplied by a constant and
added to the main variation equation.
0ln
0ln
idn
W
Wd
Method of Undetermined
Multipliers
0ln
lnln
i
ii
i
i
ii
i
i
i
i
i
dndn
W
dndndndn
WWd
e
e
0ln
i
idn
We
undetermined multipliers
Method of Undetermined
Multipliers
j i
jj
ii
ii
n
nn
n
NN
n
W
nnNNW
)ln(lnln
lnlnln
1ln1
lnln
N
n
N
NNN
n
N
n
NN
iii
j
i
i
j
j
jj
i
j
j i
jjn
n
n
nnn
n
n
n
nn1ln
1ln
)ln(
N
nNn
n
W ii
i
ln)1(ln)1(lnln
Method of Undetermined
Multipliers
0ln ii
N
ne ie
N
ni e
j
j j
j
j
j
ee
eNenN
e
e
1
j
ii
j
i
e
e
N
nP
e
e Boltzmann Distribution(Probability function for
energy distribution)
Normalization Condition
The Molecular Partition Function
Boltzmann Distribution
Molecular Partition Function
Degeneracies : Same energy value but different states (gj-
fold degenerate)
q
e
e
e
N
np
i
j
i
j
ii
e
e
e
j
jeqe
jlevels
jjegq
e
How to obtain the value of beta ?
Assumption :
T 0 then q 1
T infinity then q infinity
The molecular partition function gives an indication of the
average number of states that are thermally accessible to a
molecule at T.
kT/1
2. Interacting Systems
– Gibbs Ensemble
Solution to Schrodinger equation (Eigen-value problem)
Wave function
Allowed energy levels : En
Using the molecular partition function, we can calculate
average values of property at given QUANTUM STATE.
Quantum states are changing so rapidly that the observed
dynamic properties are actually time average over
quantum states.
i
i
i
EUm
h 2
2
2
8
Fluctuation with Time
time
states
Although we know most probable distribution of energies of individual
molecules at given N and E (previous section – molecular partition
function) it is almost impossible to get time average for interacting
molecules
Thermodynamic Properties
Entire set of possible quantum states
Thermodynamic internal energy
,...,...,, 111 i
,...,...,,, 321 iEEEE
i
ii tEU
1lim
Difficulties
Fluctuations are very small
Fluctuations occur too rapidly
We have to use alternative, abstract approach.
Ensemble average method (proposed by Gibbs)
Alternative Procedure
Canonical Ensemble
Proposed by J. W. Gibbs (1839-1903)
Alternative procedure to obtain average
Ensemble : Infinite number of mental replica
of system of interestLarge reservoir (constant T)
All the ensemble members have the same (n, V, T)
Energy can be exchanged but
particles cannot
Number of Systems : N
N ∞
Two Postulate
E1 E2 E3 E4 E5
time
Fist Postulate
The long time average of a mechanical variable M is
equal to the ensemble average in the limit N ∞
Second Postulate (Ergodic Hypothesis)
The systems of ensemble are distributed uniformly for (n,V,T) system
Single isolated system spend equal amount of time
Averaging Method
Probability of observing particular quantum state i
Ensemble average of a dynamic property
Time average and ensemble average
i
i
ii
n
nP ~
~
i
i
iPEE
i
i
in
ii PEtEU
limlim
How to find Most Probable
Distribution ?
Calculation of Probability in an Ensemble
Weight
Most probable distribution = configuration with maximum weight
Task : find the dominating configuration for given N and E
• Find maximum W which satisfies
W
i
in
N
nnn
N
!~!
~
!...~!~!~!
~
321
i
iit
i
i
nEE
nN
~
~~
0~
0~
i
ii
i
i
ndE
nd
Canonical Partition Function
Similar method (Section 2) can be used to get most
probable distribution
j
E
E
ii
j
i
e
e
N
nP
Q
e
e
e
N
nP
i
j
i E
j
E
E
ii
j
E jeQ
Canonical Partition Function
How to obtain beta ?
– Another interpretation
rev
i
ii
i
i
i
ii
i
ii
i
rev
N
ii
i
ii
dqTdSdPPdPQdPPdPE
wPdVdVV
EPdEP
ln1
)lnln(1
i
ii
i i
iiii dEPdPEPEddU )(
pdVTdSwqdU revrev
The only function that links heat (path integral) and
state property is TEMPERATURE.
kT/1
Properties from Canonical Partition
Function
Internal Energy
VNVN
qsi
E
i
VN
qsi
E
ii
i
i
QU
eEQ
eEQ
PEEU
i
i
,,
)(,
)(
ln1
1
Properties from Canonical Partition
Function
Pressure
N
ii
iiiNi
iiNi
V
EP
wdVPdxFdE
dxFdVPw
)(
)(
dx
dViF
V
idE iE
Small Adiabatic expansion of system
V
QP
eV
E
QV
Q
eV
E
QeP
QP
PPP
i
E
N
i
N
i
E
N
i
i
E
i
i
i
i
ii
ln
ln1
ln
11
P
,
i
Thermodynamic Properties from
Canonical Partition Function
ijNVTi
i
NT
NTNV
NV
NV
N
QkT
V
QQkTG
QkTA
V
Q
T
QkTH
T
QQkS
T
QkTU
,,
,
,,
,
,
ln
)ln
ln(ln
ln
)ln
ln()
ln
ln(
)ln
ln(ln
)ln
ln(
Grand Canonical Ensemble
Ensemble approach for open system
Useful for open systems and mixtures
Walls are replaced by permeable walls
Large reservoir (constant T )
All the ensemble members have the same (V, T, i )
Energy and particles can be exchanged
Number of Systems : N
N ∞
Grand Canonical Ensemble
Similar approach as Canonical Ensemble
We cannot use second postulate because systems are not isolated
After equilibrium is reached, we place walls around ensemble and treat
each members the same method used in canonical ensemble
After
equilibrium
T,V, T,V,N1
T,V,N2
T,V,N3
T,V,N4
T,V,N5
Each members are (T,V,N) systems
Apply canonical ensemble methods for each member
Grand Canonical Ensemble
Weight and Constraint
W
Nj
j
Nj
j
Nn
Nn
,
,
)!(
!)(
Nj
jt
Nj
jjt
Nj
j
NNnN
NVENnE
Nn
,
,
,
)(
),()(
)(N
Number of ensemble members
Number of molecules after
fixed wall has been placed
Method of undetermined multiplier
with , ,g
NVNE
j eeeNn j g ),(* )( N
Nj
NVNE
NVNE
jj
jee
eeNnNnNP
j
j
,
),(
),(* )()()(
g
g
NN
Grand Canonical Ensemble
Determination of Undetermined Multipliers
Nj
jj VNENPEU,
),()(
Nj
jj
Nj
jj VNdENPNdPVNEdU,,
),()()(),(
Nj
j
j
Nj
jj dVV
VNENPNdPNPNdU
,,
),()()(ln)(ln
1g
Nj
NVNEee j
,
),( g
dNpdVTdSdU Comparing two equation gives,
kT
g
kT
1
Nj
kTNkTVNEee j
,
//),(
Grand Canonical Partition Function
4. Classical Statistical Mechanics
The formalism of statistical mechanics relies very much at the
microscopic states.
Number of states , sum over states
convenient for the framework of quantum mechanics
What about “Classical Sates” ?
Classical states
• We know position and velocity of all particles in the system
Comparison between Quantum Mechanics and Classical Mechanics
EH QM Problem Finding probability and discrete energy states
maF CM Problem Finding position and momentum of individual molecules
Newton’s Law of Motion
Three formulations for Newton’s second law of motion
Newtonian formulation
Lagrangian formulation
Hamiltonian formulation
ii
i
ii
t
mt
Fp
pr
ijj
iji
zyx
zyx
ppp
rrr
1
),,(
),,(
FF
pp
rr
),...,,(2
),(
energy) alPE(potenti energy) KE(kinetic),(
21 N
i i
iNN
NN
Um
H
H
rrrp
pr
pr
i
i
i
i
H
H
rp
pr
Classical Statistical Mechanics
Instead of taking replica of systems, use abstract “phase space”
composed of momentum space and position space (total 6N-space)
Np
Nr
1t
2t
1
2
NN rrrrpppp ,...,,,,,...,,, 311321
Phase space
Classical Statistical Mechanics
“ Classical State “ : defines a cell in the space (small volume of
momentum and positions)
Ensemble Average
simplicityfor State" Classical" 33 rpdddrdrdrdqdqdq zyxzyx
dEdEU N
n)()(lim)(
1lim
0P
dN )(P Fraction of Ensemble members in this range
( to +d)
dkTH
dkTHdN
)/exp(...
)/exp()(P
Using similar technique used for
Boltzmann distribution
Classical Statistical Mechanics
Canonical Partition Function
dkTH )/exp(...TPhase Integral
dkTHc )/exp(...QCanonical Partition Function
dkTH
kTEi
i
T )/exp(...
)/exp(
limcMatch between Quantum
and Classical Mechanics
NFhN!
1c
For rigorous derivation see Hill, Chap.6 (“Statistical Thermodynamics”)
Classical Statistical Mechanics
Canonical Partition Function in Classical Mechanics
dkThN NF
)/exp(...!
1HQ
Example ) Translational Motion for
Ideal Gas
N
i i
i
N
i i
iNN
NN
m
pH
Um
H
H
3 2
21
2
),...,,(2
),(
energy) alPE(potenti energy) KE(kinetic),(
rrrp
pr
pr
N
N
NV
N
i
N
i
NN
i
i
N
Vh
mkT
N
drdrdrdpm
p
hN
drdrdpdpm
p
hNQ
2/3
2
0
321
3
3
11
2
3
2
!
1
)2
exp(!
1
......)2
exp(...!
1
No potential energy, 3 dimensional
space.
We will get ideal gas law
pV= nRT
Semi-Classical Partition Function
The energy of a molecule is distributed in different modes
Vibration, Rotation (Internal : depends only on T)
Translation (External : depends on T and V)
Assumption 1 : Partition Function (thus energy distribution) can be separated
into two parts (internal + center of mass motion)
),(),,(
)exp()exp()exp(
int
intint
TNQTVNQQ
kT
E
kT
E
kT
EEQ
CM
i
CM
ii
CM
i
Semi-Classical Partition Function
Internal parts are density independent and most of the
components have the same value with ideal gases.
For solids and polymeric molecules, this assumption is not
valid any more.
),0,(),,( intint TNQTNQ
Semi-Classical Partition Function
Assumption 2 : for T>50 K , classical approximation can be
used for translational motion
N
N
i
NNiziyix
N
N
i
iziyix
CM
drdrdrkTUZ
mkT
h
ZN
drkTUdpmkT
ppp
hNQ
rrrUm
pppH
321
2/12
3
33
222
3
321
222
...)/(...
2
!
)/(...)2
exp(...!
1
),...,,(2
ZQN
Q N3
int!
1
Configurational Integral
Another, Different Treatment
Statistical Thermodynamics:
the basics
• Nature is quantum-mechanical
• Consequence:
– Systems have discrete quantum states.
– For finite “closed” systems, the number of states is finite (but usually very large)
• Hypothesis: In a closed system, every state is equally likely to be observed.
• Consequence: ALL of equilibrium Statistical Mechanics and Thermodynamics
Basic assumptionEach individual
microstate is
equally probable
…, but there are not
many microstates that
give these extreme
results
If the number of
particles is large (>10)
these functions are
sharply peaked
Does the basis assumption lead to something
that is consistent with classical
thermodynamics?
1ESystems 1 and 2 are weakly coupled
such that they can exchange energy.
What will be E1?
1 1 1 1 2 1,E E E E E EW W W
BA: each configuration is equally probable; but the number of
states that give an energy E1 is not know.
2 1E E E
1 1 1 1 2 1,E E E E E EW W W
1 1 1 1 2 1ln , ln lnE E E E E EW W W
1 1
1 1
1 ,
ln ,0
N V
E E E
E
W
lnW1
E1
E1
N1,V
1
lnW
2E E
1 E
1
N2
,V2
0
1 1 2 2
1 1 2 1
1 2, ,
ln ln
N V N V
E E E
E E
W W
Energy is conserved!
dE1=-dE2
This can be seen as an
equilibrium condition
,
ln
N V
E
E
W
1 2
Conjecture:
Almost right.
•Good features:
•Extensivity
•Third law of thermodynamics comes for free
•Bad feature:
•It assumes that entropy is dimensionless but (for
unfortunate, historical reasons, it is not…)
Entropy and number of
configurations
lnS W
We have to live with the past, therefore
With kB= 1.380662 10-23 J/K
In thermodynamics, the absolute (Kelvin)
temperature scale was defined such that
But we found (defined):
lnBS k E W
,
1
N V
S
E T
,
ln
N V
E
E
W
dE TdS-pdV idNii1
n
And this gives the “statistical” definition of temperature:
In short:
Entropy and temperature are both related to
the fact that we can COUNT states.
,
ln1B
N V
Ek
T E
W
Basic assumption:
1. leads to an equilibrium condition: equal temperatures
2. leads to a maximum of entropy
3. leads to the third law of thermodynamics
How large is W?
•For macroscopic systems, super-astronomically large.
•For instance, for a glass of water at room temperature:
•Macroscopic deviations from the second law of
thermodynamics are not forbidden, but they are
extremely unlikely.
Number of configurations
252 1010 W
Canonical ensemble
Consider a small system that can exchange heat with a big reservoir
iE iE E ln
ln lni iE E E EE
WW W
ln
i i
B
E E E
E k T
W
W
1/kBT
Hence, the probability to find Ei:
exp
exp
i i B
i
j j Bj j
E E E k TP E
E E E k T
W
W
expi i BP E E k T
Boltzmann distribution
Example: ideal gas
3
1, , d exp
!
N N
NQ N V T U r
N
r
3 3
1d 1
! !
NN
N N
V
N N
r
Free energy:
3
3 3
ln!
ln ln ln ln
N
N
VF
N
NN N N N
V
Pressure:
T
F NP
V V
Energy:
3 3
2B
F NE Nk T
Thermo recall (3)
Helmholtz Free energy:
T
FP
V
d d dF S T p V
1
F T FE
T
Energy:
Pressure
Ensembles
• Micro-canonical ensemble: E,V,N
• Canonical ensemble: T,V,N
• Constant pressure ensemble: T,P,N
• Grand-canonical ensemble: T,V,μ
Basic assumptionEach individual
microstate is
equally probable
…, but there are not
many microstates that
give these extreme
results
If the number of
particles is large (>10)
these functions are
sharply peaked
Does the basis assumption lead to something
that is consistent with classical
thermodynamics?
1ESystems 1 and 2 are weakly coupled
such that they can exchange energy.
What will be E1?
1 1 1 1 2 1,E E E E E EW W W
BA: each configuration is equally probable; but the number of
states that give an energy E1 is not know.
2 1E E E
1 1 1 1 2 1,E E E E E EW W W
1 1 1 1 2 1ln , ln lnE E E E E EW W W
1 1
1 1
1 ,
ln ,0
N V
E E E
E
W
lnW1
E1
E1
N1,V
1
lnW
2E E
1 E
1
N2
,V2
0
1 1 2 2
1 1 2 1
1 2, ,
ln ln
N V N V
E E E
E E
W W
Energy is conserved!
dE1=-dE2
This can be seen as an
equilibrium condition
,
ln
N V
E
E
W
1 2
Conjecture:
Almost right.
•Good features:
•Extensivity
•Third law of thermodynamics comes for free
•Bad feature:
•It assumes that entropy is dimensionless but (for
unfortunate, historical reasons, it is not…)
Entropy and number of
configurations
lnS W
We have to live with the past, therefore
With kB= 1.380662 10-23 J/K
In thermodynamics, the absolute (Kelvin)
temperature scale was defined such that
But we found (defined):
lnBS k E W
,
1
N V
S
E T
,
ln
N V
E
E
W
dE TdS-pdV idNii1
n
And this gives the “statistical” definition of temperature:
In short:
Entropy and temperature are both related to
the fact that we can COUNT states.
,
ln1B
N V
Ek
T E
W
Basic assumption:
1. leads to an equilibrium condition: equal temperatures
2. leads to a maximum of entropy
3. leads to the third law of thermodynamics
How large is W?
•For macroscopic systems, super-astronomically large.
•For instance, for a glass of water at room temperature:
•Macroscopic deviations from the second law of
thermodynamics are not forbidden, but they are
extremely unlikely.
Number of configurations
252 1010 W
Canonical ensemble
Consider a small system that can exchange heat with a big reservoir
iE iE E ln
ln lni iE E E EE
WW W
ln
i i
B
E E E
E k T
W
W
1/kBT
Hence, the probability to find Ei:
exp
exp
i i B
i
j j Bj j
E E E k TP E
E E E k T
W
W
expi i BP E E k T
Boltzmann distribution
Example: ideal gas
3
1, , d exp
!
N N
NQ N V T U r
N
r
3 3
1d 1
! !
NN
N N
V
N N
r
Free energy:
3
3 3
ln!
ln ln ln ln
N
N
VF
N
NN N N N
V
Pressure:
T
F NP
V V
Energy:
3 3
2B
F NE Nk T
Thermo recall (3)
Helmholtz Free energy:
T
FP
V
d d dF S T p V
1
F T FE
T
Energy:
Pressure
Ensembles
• Micro-canonical ensemble: E,V,N
• Canonical ensemble: T,V,N
• Constant pressure ensemble: T,P,N
• Grand-canonical ensemble: T,V,μ