Fermi-Dirac and Bose-Einstein...
-
Upload
duongquynh -
Category
Documents
-
view
219 -
download
0
Transcript of Fermi-Dirac and Bose-Einstein...
Phys 112 (S2005) 6 1 B.Sadoulet
Fermi-Dirac and Bose-EinsteinDistributions
Beg. chap. 6 and chap. 7 of K &KQuantum Gases
Fermions, BosonsPartition functions and distributionsDensity of states
Non relativisticRelativistic
Classical LimitFermi Dirac Distribution
Fermi Energy Electrons in solids
Nuclear matterWhite Dwarf
Bose Einstein DistributionBose-Einstein CondensationLiquid Helium
Phys 112 (S2005) 6 2 B.Sadoulet
Quantum GasesBosons, Fermions
Integer spin= Boson = number of particles in a given state isarbitraryHalf Integer spin=Fermion= at most one on each orbital:
Pauli exclusion principlePartition Functions and mean occupation numbers
FermionAt most one
BosonSum on all integers
Z = 1+ expµ ! "#
$%&
'()
s !( ) =1
exp! " µ
#$ % & '
( ) +1
Z= exp sµ ! "#
$%&
'()
s=0
*
+ =1
1! exp µ ! "#
$%&
'()
s !( ) =1
exp! " µ
#$ % & '
( ) "1
Phys 112 (S2005) 6 3 B.Sadoulet
Ideal quantum gases“Ideal gas” approximation
States are not modified by presence of other particles
“Density “ of statesmultiplicity x density in phase space change of variable to energy
Non relativistic
Ultra-Relativistic
gi !d3x d3p
h3
gi !p2dp d"
h3"# = D($ )d$ where D($) is the density of states
D !( )d! = 4"gip2dp
h3=
gi
4"22m
h2
#
$ %
&
' (
3
2 !d!
D !( )d! = 4"gip2dp
h3=
gi
2"2h3c3
!2d!
Phys 112 (S2005) 6 4 B.Sadoulet
BehaviorSign is critical for (ε-µ)/τ small
Fermi-Dirac
Bose-EinsteinBose condensation
For (ε-µ)/τ large, classical limitOccupation number << 1
Same old resultsBoltzmann /Gibbs !
s !( ) =1
exp! " µ
#$ % & '
( ) + 1
=1
2 for ! = µ
= 1 for ! << µ
s !( ) =1
exp! " µ
#$ % & '
( ) "1
*+ for ! * µ
s !( ) " exp
µ # !$
%&'
()*= + exp #
!$
%&'
()*
independent of F.D. or B.E.
Prob !( ) =s !( )
N!!!!< N >= V s !( )" D !( )d! = V exp
µ
#$%&
'()exp *
!#
$%&
'()"d3p
h3
!!!< N >= V expµ
#$%&
'()nQ + µ = log
n
nQ
$
%&
'
()
<s(ε)>
µ ε
1
Phys 112 (S2005) 6 5 B.Sadoulet
Thermo functions for ideal quantum gases
Number of Particles
µ(τ) set by requirement that N=total number of particles
Energy
- Bose- Einstein + Fermi-Dirac
Entropy
N =V s !( ) D !( )d!0
"# = V
D !( )d!
exp! $ µ
%& ' ( )
* + ±1
0
"#
U = V!D !( )d!
exp! " µ
#$ % & '
( ) ±1
0
*+
! "( ) =
# $ logZ( )
#$ !=! " µ
#s + logZ ! " log prob s =< s >( )$% &'
Phys 112 (S2005) 6 6 B.Sadoulet
Fermi Gas Ground State (Non relativistic)
Fermi EnergyCalculation :
Energy/Free Energy
Pressure Repulsive!
s !( )
!
!F
! << µ
s !( ) =1
exp! " µ
#$ % & '
( ) + 1
*1 for ! < µ
! 0 for " > µ
N =V s !( ) D !( )d!0
"# = V D !( )d!
0
! F#
!F = µ " = 0( )
!"F =
h2
2m3#
2n( )
2
3 with n =N
V
U = F = V !D !( )d!0
!F
" =3
5N!
F
p = !"F
"V #
=2
5n$F %V
!5
3
Spin 1/2
Phys 112 (S2005) 6 7 B.Sadoulet
Fermi Gas Ground State (Relativistic)Note that even at zero temperature very large kinetic energies: in
some case ultra-relativistic
Fermi Energy
Energy
Pressure
!F = µ " = 0( )
N =V D !( )d!0
! F" =
V
3#2h3c3!F3
!"F = 3#
2n( )1
3 hc
U = F = V !D !( )d!0
! F" =
3
4N!F
p = !"F
"V #
=1
4n$F %V
!4
3
Phys 112 (S2005) 6 8 B.Sadoulet
Hole and Electron ExcitationsSymmetry of Fermi Dirac distribution
Basic symmetry (except for lower bound at δ =-µ ).Note:
Decomposition into hole-like and electron-likeexcitations
Number of excited electrons= number of excited holes
When referenced to the Fermi energy, the energy of holes are opposite tothat of the corresponding missing electrons and is positive
With !="-µ !!!!!!!! f ",#( ) =1
exp!#
$%&
'()+1
1* f ",#( ) =1
exp *!#
$%&
'()+1
N
V= D !( ) f !,"( )
0
#$ d! = D !( )
0
!F$ d!
D !( ) f !,"( )!F#$ d!
B = "electrons"
1 2444 3444= D !( ) 1% f !,"( )( )0
!F$ d!
A = "holes"
1 24444 34444
�
f ! ,"( )
�
!
u !( ) " u 0( ) = # " #F( )D #( ) f #,!( )#F$% d#
"electrons"
1 24444 34444+ #F " #( )D #( ) 1" f #,!( )( )0
#F% d#
"holes"
1 244444 344444
for ! << µ,!µ !( ) " µ 0( ) = #
F
f !,"( ) = s !( )"
Phys 112 (S2005) 6 9 B.Sadoulet
Energy Band structurePeriodicity of the lattice (e.g., spacing a)
Resonant tunelling: free propagation of specific modes
gap (cf. Kittel, introduction to Solid States Physics Chap. 7))≈ 1 eV
Seen in projection on the energy axis: energy bands• Valence band• Conduction band
Metal: Fermi level = chemical potential in conduction band => conductioncan be described by free Fermi gas
Insulator: Fermi level in gap
Electrons in crystals: Quantum States
�
Discrete E k( )
E
k
εc
εv
conduction band
valence band
Gap
Phys 112 (S2005) 6 10 B.Sadoulet
Electrons in metalsOrder of magnitude
τ=o : very good approximation at room temperature and below
Heat Capacity
use: • Conservation of number of particles• df /dτ only large close to εF• µ does not vary fast with τ• εF/τ large
!F " 5 eV # TF " 5 104
K >> Tlab
�
Cel = kBdU
d!= kB
d
d!V"D "( ) f ",!( )
0
#
$ d" = kBV "D "( )d
d!f " ,!( )
0
#
$ d"
Cel!"2
3kBVD #
F( )$
Ctot = Cel +C! = "T + AT3
�
!F
�
!�
f ! ,"( )
Phys 112 (S2005) 6 11 B.Sadoulet
Insulators: Density of states cf. K&K chap 13
Often called intrinsic semiconductors (no role of impurities)
Statistical distributionStill good approximation to consider free electrons as quantum ideal gas=> occupation number
Density of states
We then get
f !( ) =1
exp ! " µ( ) /#( ) +1
Dh(!)d! =2
4" 22mh
*
h2
#
$ %
&
' (
3
2
(!v )! )d!
De(!)d! =2
4" 22me
*
h2
#
$ %
&
' (
3
2
(! ) !c)d!!c
!v
! !
Gap
D (!)
conduction band
valence band
2 spin states
Parabolicat gap edge
Electron state density below the gap
1
exp µ ! "( ) / #( ) +1Dh"( )d"
0
"v
$holes
1 244444 344444
=1
exp " ! µ( ) / #( ) +1De"( )d"
"c
%
$electrons
1 244444 344444
ne =2
4! 2
2me
*
h2
"#$
%&'
3/2
1
exp ( ') µ ) (c( )( ) / *( ) +1( 'd( '
0
+
, - nQe exp )(c ) µ*
"#$
%&'
with!nQe = 2me
**2!h
2
"#$
%&'
3
2
!!
for ! << "v = nh =2
4# 2
2mh
*
h2
$%&
'()
3/2
1
exp " '* "v * µ( )( ) / !( ) +1" 'd" '
0
+
, - nQh exp *µ * "v!
$%&
'()
with!nQh = 2mh
*!2#h
2
$%&
'()
3
2
Phys 112 (S2005) 6 12 B.Sadoulet
Determining the chemical potentialNo impurities: intrinsic semiconductors
!v !
c
!µ
f
!v !
c
µµ
logne(µ)
lognhµ( )
Phys 112 (S2005) 6 13 B.Sadoulet
SemiconductorsLarge role of impurities: localized states (Not band !) in gap
If they are shallow (≈ 40meV (Si) ≈10meV (Ge)) can be excited at roomtemperature. This modifies totally the behavior!Donors
Acceptors note: 2 A0 state because a bond is missing and the missing electron
can be spin up or down, A- bond established (pair of electrons of antiparallel spins) : 1state
⇒The number of free electrons(holes) is no moreconstant
Can be increased by donors and decreased by acceptorsBut we need to keep charge neutrality = method to compute the
Fermi level⇒For large enough impurities concentration, the Fermi level can
move close to the edge of the gap⇒(Thermally generated) conductivity either dominated by
• electron like excitation: negative carriers (n type)• hole like excitation: positive carriers (p type)
do! d
++ e
" nd = nd + + ndo
a!" a
o+ e
! na = na!+ n
ao
k
εc
εv
εDεA
Phys 112 (S2005) 6 14 B.Sadoulet
Donors
negative carriers (n type)
Acceptors
positive carriers (p type)
Semiconductors cf. K&K fig 13.6
!v !
c
µ
µ
logne(µ)
lognhµ( )
d0 ! d
++ e
"
nd+ = nd
exp "#+
$%&'
()*
exp "#+
$%&'
()*+ 2exp "
#0 " µ
$%&'
()*
= nd
1
1+ 2expµ " #
d
$%&'
()*
with!!!#d+ #0 " #+ , #
c"0.04 !eV !Si
0.01!eV !Ge
lognd+ µ( )
!d
Electric neutrality
ne= n
d+ + nh ! nd+
!v !
c
µ
µ
logne(µ)
lognhµ( )
lognd+ µ( )
!a
Electric neutrality
ne+ n
a!= n
h" n
a!
a0+ e
! " d+
na! = na
exp !#! ! µ
$%&'
()*
2exp !#0$
%&'
()*+ exp !
#! ! µ
$%&'
()*
= nd
1
1+ 2exp#a! µ
$%&'
()*
with!!!#a+ #! ! #0 , #
v+0.04 !eV !Si
0.01!eV !Ge
Phys 112 (S2005) 6 15 B.Sadoulet
Other examples of degenerate Fermigas3He
Spin 1/2Very different behavior from 4He: phase separation
Nuclear Matter
⇒Fermi momentumR ! 1.3 10
"13 A
1
3 cm
np ! nn ! 5 1037
cm-3"#F = 4 10
$12 J ! 30 MeV
Phys 112 (S2005) 6 16 B.Sadoulet
White Dwarfs and Neutron StarsWhite dwarf stars (and core of massive stars)
=> Degenerate Fermi gasFermi pressure balances gravity => Condition for equilibriumNon relativistic minimum of total energy: stable!
Ultra RelativisticDegeneracy pressure cannot balance gravity if M too big!
Chandrasekhar limitNeutron stars
Same story for neutrons (uncertainty of equation of state)Similar Chandrasekhar limit if larger => black hole
! " 106 g/cm3 n " 1030 cm-3
!F " 0.5 10#13
J " 3 105
eV TF " 3 109
K >> Tstar
1.4 M!
3 M!
R
UUFD Non Relativistic
UT NR
UG
R
UFD Relativistic
UTRel UG
Phys 112 (S2005) 6 17 B.Sadoulet
White Dwarf Explosions: SN Ia
time
Lum
inos
ity
Distance
Ωm=1ΩΛ=0
Fain
ter
An acceleratinguniverse?
Supernovae Type Ia at high redshift (2 groups) Ωm-ΩΛDistant supernovae appear dimmer
than expected in a flat universe
Potential problemsAre supernova properties
really constant?Dust?
The Uninvited Guest:Dark Energy
Large negative energy
aacceleration
{ =G
r2
1
c2
uenergy density
{ + 3 p
pressure
{
!
"#
$
%&
GR gravitational mass
1 24444 34444
V
Gravity becomes repulsive!
Phys 112 (S2005) 6 18 B.Sadoulet
Bose-Einstein CondensationCalculation of chemical potential
Let us take the origin of energy at the ground state
Separating between the ground state s=1 and the other states
Forwe can solve the equation by having
Bose Einstein condensation. For large number of particles, not a verylow temperature phenomenon
�
1
exp!µ
"#
$ %
&
' ( !1
+1
exp)s! µ
"#
$ %
&
' ( !1s>1
* = N
�
exp!µ
"#
$ %
&
' ( ) 1
exp!s
"#$%
&'(>> 1+
1
N)" << !
sN
f 0,!( ) = s 0( ) =1
exp "µ
!#$%
&'("1
) "!µ) N ** µ ) "
!N
! << "sN
! Nexc = 2.612m"2#h
2
$
% &
'
( )
3 /2
V = 2.612nQV
�
!E
=2"h
2
m
N
2.612 V
#
$ %
&
' (
2/3
) Nexc
= N!!E
#
$ %
&
' (
3/2
Phys 112 (S2005) 6 19 B.Sadoulet
Liquid Helium 4Properties of 4He
Loose coupling =>liquid (4.2K at 1 Atm) ≈ ideal gas 4He has spin 0 => boson ≠ 3He spin 1/2
=> expect condensation at ≈3.1KExperimentally “lambda point” 2.17K (Landau temp.)
Phase transition => peculiar propertiesMacroscopic quantum state
=> Quantization phenomenae.g. Vortex Equivalent of Josephson effect
=>Superfluidity
! = n1/2
ei" t,
r x ( )
!" = 2n# where n is integer
C 4He
T2.17K
Phys 112 (S2005) 6 20 B.Sadoulet
Much cleaner system: Alcali VaporsBE condensation for atoms demonstrated in 1995=> 2001 Nobel Prize in Physics
awarded jointly to Eric A. Cornell of NIST / JILA; WolfgangKetterle of MIT; and Carl E. Wieman of CU / JILA.
Time sequence of imagesshowing one cycle of the ringingof a Bose-Einsteincondensate (BEC) in the JILATOP (time-averaged orbitingpotential) trap after being drivenby strong oscillationsof trap potential.
Phys 112 (S2005) 6 21 B.Sadoulet
Pairing of FermionsSuperconductivity
Pairing of electrons s=0 (Cooper pairs) <= phonon interactionBut condensation theory bad approximation (not free)Similar effects
• Zero resistance• Quantization of flux : Vortices
3HeSpin 1/22 phases of pairing s=1
similar to superconductivity but magnetic properties
τcondensation = 0.95mK and 2.5mK
Phys 112 (S2005) 6 22 B.Sadoulet
Energy Density of Ultra Relativistic GasesGeneralizationImportant for behavior of early universe (energy density =>expansion)
Suppose that particles are non degenerate (µ<<τ)
Density of energy
f !( ) "1
exp!#
$
% &
'
( ) ±1
u = gbosons +7
8gfermions
!
" #
$
% & 'aB
2T4