entropy bounds
DESCRIPTION
Entropy bounds. Introduction Black hole entropy Entropy bounds Holography. Macroscopic state. 1/3. 1/3. Microscopic states. Ex: (microcanonical) - k S p i ln(p i ) =k S1/ N ln N =k S ln N. 1/3. |☺☺O>. |☺O☺>. | O ☺☺>. r = S p i | F > ii < F |. What is entropy?. - PowerPoint PPT PresentationTRANSCRIPT
Entropy bounds
•Introduction
•Black hole entropy
•Entropy bounds
•Holography
Microscopic states
What is entropy?
S=k·ln(N)
S=-k piln(pi)
S=-k r(ln
Ex: (microcanonical)kpiln(pi) =k NlnN
=k lnN
= pi|>ii<| S=k ln 3
1/3
1/3
1/3
S=-k 3 1/3 ln 1/3 = k ln 3
|☺☺O>
|☺O☺>
| O ☺☺>
3
100
03
10
003
1
Macroscopic state
Examples• Free particle:
• Black body radiation:
• Debye Model (low temperatures):
23
22ln
2
3),,(
mkTV
NNNkTVNS
3
442
)(15),,(
c
VTkTVNS
Nc
TVkTVNS
33
432
10),,(
Entropy boundsWhat is the maximum of S?
Extremum problem:
S[pi]=-kpiln pi
subject to pi=1
pi =1/N
Smax=k ln dim H
N
N
100
00
001
Smax=k 100ln2
dimH= 2100
Example 1: maximum entropy of 100 spin 1/2 particles
= |, ,…, >
Entropy bounds
Example 2: maximum entropy of free fermions in a box
= |n0,0,0,, n0,0,0, , nħ/L,0,0,,n 0,ħ/L, 0,,…,n,>
Number of modes = 2k1 L3k2dk L33
Smax L33
dimH= 2N 2L33
Momentummode
Spin Maximalmomentum
Smax available phase space
N available phase space
Generalization:
dimH= ONSpin up and momentum kx=ħ/L
Entropy boundsWhy is this interesting?
Black hole entropy
Entropy boundson matter
Smax
Available phase spacein quantum gravity
r
p
What shoulda unified theory look like
?
Black holes
A wrong derivation yielding correct results:
R
GM2vescape
If nothing can escape then:
cescapev
Yielding:
12
2
Rc
GMRs=2GM/c2R≤
Scwartzschield radiusBlack hole condition
x
y
The event horizon
Schwartzshield radius
x
y
t
Event Horizon formed
Schwartzshield radius
Singularityformed
Singularityformed
Event Horizon formed
Black hole entropy(Bekenstein 1972)
S>0Sbh = 0
Assumption
ST>0ST=0
The area of a black hole always increases:A≥
Sbh =A/4
Via Hawking radiation: Sbh = 4kR2c3/4Għ
Generalized second lawSbhA ; ST=Sbh+Sm
Bekenstein entropy bound(Bekenstein 1981)
Adiabatic lowering
Initial entropy: mSG
ckR
4
4 32
Final entropy: bhSG
ckR
4
4 32
c
krEM
dM
dSSS bhbhm
2
SmEr
E’
Energy is red-shifted: E’=Erc2/4MG
Mass of black hole increases: M M+M M+E’/c2
Problems with the Bekenstein bound
h
Sm<2krE/cħ
Sm 2khE/cħ?
Susskind entropy bound(Susskind 1995)
Sm,M
R
G
RcM
2
2
Initial stage
Sm
Sshell,c2R/2G-M
Shell
G
RcM
2
2
Sm+ Sshell
After collapse
G
RcM
2
2
SBH
Sm≤SBH=4kR2c3/4Għ=A/4
Problems with a space-like bound
Sm
R
Sm≤A/4?
Bousso bound(Bousso 1999)
x
y
t
Light cone
x
y
t
Light sheet
V
Sm≤A/4
Possible conclusions from an entropy bound
Dim H A
In general, field theory over-counts the available degrees of freedom
L=L((x),(x))d4x
A fundamental theory of nature shouldhave the ‘correct’ number of degrees of freedom
?
Gravity restricts the number of degrees of freedom available GN
The Holographic principle(‘t Hooft 93, Susskind 94)
N, the number of degrees of freedom involved in the description of L(B), must not exceed A(B)/4. (Bousso 1999)
The light sheetof the region B
The surface area of B in planck units
A D dimensional quantum theory of gravity may be described by a D-1 dimensional Quantum field theory.
Proposition
A working example: AdS/CFT
Quantum gravity inD+1 dimensionalAnti de-Sitter space.
(Conformal) Field theory in D dimensionalflat space
Current research
•How does one generalize the AdS/CFT
correspondence to other space-times?
•What is the role of gravity in holography?
•Is string theory holographic?