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ENTROPY AND DECOHERENCE IN QUANTUM THEORIES
Tomislav Prokopec, ITP & Spinoza Institute, Utrecht University
Nikhef, Mar 30 2012
Based onBased on: : Jurjen F. Koksma, Tomislav Prokopec and Michael G. Schmidt,Jurjen F. Koksma, Tomislav Prokopec and Michael G. Schmidt, Phys. Rev. D (2011Phys. Rev. D (2011)) [ [arXiv:1102.4713 [hep-th]];arXiv:1101.5323 [quant-ph]; Annals Phys. (2011), arXiv:1012.3701 [quant-ph];
Phys. Rev. D Phys. Rev. D 8181 (2010) 065030 (2010) 065030 [[arXiv:0910.5733 [hep-th]]]
Annals Phys. Annals Phys. 325325 (2010) 1277 (2010) 1277 [[arXiv:1002.0749 [hep-th]]]
Tomislav Prokopec and Jan Weenink, [Tomislav Prokopec and Jan Weenink, [arXiv:1108.3994[gr-qc]]+ in preparation]+ in preparation
˚ 1˚
PLAN˚ 2˚
ENTROPY as a physical quantity and decoherence
ENTROPY of (harmonic) oscillators
ENTROPY and DECOHERENCE in relativistic QFT’s
APPLICATIONS
DISCUSSION
● bosonic oscillator● fermionic oscillator
● CB● neutrino oscillations and decoherence
VON NEUMANN ENTROPY ˚ 3˚
von Neumann entropy (of a closed system):
operatordensity)(ˆ)],ˆln(ˆTr[)(vN ttS
]ˆ,ˆ[)(ˆ Htt
..OBEYS A HEISENBERG EQUATION:
as a result, von Neumann entropy is conserved:
Consequently, von Neumann entropy is conserved, hence USELESS.
constant.)(0)( vNvN tStSdt
d
However: vN entropy is constant if applied to closed systems, whereall dof’s and their correlations are known. In practice: never the case!
CLOSED SYSTEM
const.)(vN tS
OPEN SYSTEMS ˚ 4˚
◙ OPEN SYSTEMS (S) interact with an environment (E).If observer (O) does not perceive SE correlations (entanglement),(s)he will detect a changing (increasing?) vN entropy.
von Neumann entropy is not any more conserved
timein(?)increases)(
0)(
vN
vN
tS
tSdt
d
NB: entropy/decoherence is an observer dependent concept. Hence, arguably there is no unique way of defining it. Some argue: useless. In practice: has shown to be very useful.
OPEN SYSTEM
Proposal: vN entropy (of S) is a quantitative measure for decoherence.
SE
ENTROPY, DECOHERENCE, ENTANGLEMENT
˚ 5˚
system (S) + environment (E) + observer (O)
E interacts very weakly with O: unobservable
O sees a reduced density matrix:
Tracing over E is not unitary: destroys entanglement;responsible for decoherence & entropy generation
1]ˆTr[]ˆTr[ red2red
]ˆ[Trˆ ESEred )]ˆln(ˆTr[)( redredvN tS
DIVISION S-E can be in physical space: traditional entropy; black holes; CFTsSrednicki, 1992Srednicki, 1992
CORRELATOR APPROACH TO DECOHERENCE
˚ 6˚
BASED ON (UNITARY, PERTURBATIVE) EVOLUTION OF 2-pt FUNCTIONS (in field theory or quantum mechanics)
Koksma, Prokopec, Schmidt (‘09, ‘10), Giraud, Serreau (‘09)Koksma, Prokopec, Schmidt (‘09, ‘10), Giraud, Serreau (‘09)
ADVANTAGES:
evolution is in principle unitary: reduction of does not affect the evolution, i.e. it happens in the channel: O-S, and not S-E
NEW INSIGHT: decoherence/entropy increase is due to unobservable higher order correlations (non-gaussianities) in the S-E sector:realisation of COARSE GRAINING.
(almost) classical systems tend to behave stochastically, i.e. there is a stochastic force, kicking particles in unpredictable ways.Examples: Solar Planetary System; Large scalar structure of the Universe
DECOHERENCE AND CLASSICIZATION˚ 7˚
A theory that explains how quantum systems become (more) classicalZeh (1970), Joost, Zurek (1981) & othersZeh (1970), Joost, Zurek (1981) & others
Decoherence has gained in relevance: EPR paradox; quantum computational systems
Phase space picture:
p(t)
x(t)
EARLY TIME t LATE TIME t’>t
x(t’)
p(t’)
EVOLUTION: IRREVERSIBLE! – in discord with quantum mechanics!
HARMONIC OSCILLATORS
˚ 8˚
BOSONIC OSCILLATORS (bHO)˚ 9˚
● HAMILTONIAN & HAMILTON EQUATIONS
i
N
ii qqtHtHqm
m
ptH ˆ)(ˆ,)(ˆˆ
2
1
2
ˆ)(ˆ
1intint
222
Htqdt
dHtp
dt
dpqˆ)(ˆ,ˆ)(ˆ
● GAUSSIAN DENSITY OPERATOR
)1(,]ˆ,ˆ[,}ˆ,ˆ){(ˆ)(ˆ)(exp1
)(ˆ 2221
g pqpqtqtptZ
t
NB: knowing (t), (t), (t) is equivalent to solving the problem exactly!
● THE FOLLOWING TRANSFORMATION DIAGONALISES :
1]ˆ,ˆ[,ˆˆ12
)(ˆ,ˆˆ12
)(ˆ
bbpqtbpqtb
BOSONIC OSCILLATOR: GAUSSIAN ENTROPY
˚10˚
● DIAGONAL DENSITY OPERATOR
σeZbbNNtZ
t 1,ˆˆˆ,,)2/1ˆ)((exp1
)(ˆ 12g
● Can relate parameters in (, , ) to correlators:
2
2
1ˆ,ˆ,
2
1)ln(2ˆ,
2
1)ln(2 22
npqnZqnZp
● INTRODUCE A FOCK BASIS: nnInnn
0
,,..1,0,
● IN THIS BASIS:1
1ˆ)(,)1(
)(,)(ˆ1g
e
Ntnn
ntnnt
n
n
nn
n
2
coth21ˆ,ˆˆˆ4 222
21222
npqpq
● AN INVARIANT OF A GAUSSIAN DENSITY OPERATOR
GAUSSIAN ENTROPY˚11˚
● in terms of and
2
1ln
2
1
2
1ln
2
1))(ˆln()(ˆTr gg ttS
● is an invariant measure (statistical particle number) of the phase space volume of the state in units of ħ/2.
Ntn ˆ)(
nnnnS ln1ln)1(
2
1ˆ)(
Ntn
p
q
ENTROPY GROWTH IS THUS PARAMETRIZED BY THE GROWTH OF THE PHASE SPACE AREA (in units of ħ) (t)
1)1/()( nnn nnnnt● is the
probability that there are n particles in the state.
ENTROPY FOR 1+1 bHO˚12˚
(ENTROPY)
NB: grey: UNPHYSICAL SECULAR GROWTH AT LATE TIMES
►UNITARY EVOLUTION (black); REDUCED EVOLUTION (gray)
► LEFT: nonresonant regime; RIGHT: resonant regime
TIME
NB: relatively small Poincaré recurrence time.
TIME
NB: If initial conditions are Gaussian, the evolution is linear and will preserve Gaussianity. Scorr will be generated by <xq>0 correlators.
ES
SS
E-SS
SS
SS
(PERT. MASTER EQ)
ENTROPY FOR 50+1 bHO˚13˚
(ENTROPY)
NB: gray: UNPHYSICAL SECULAR GROWTH AT LATE TIMES (PERT. MASTER EQ)
►UNITARY EVOLUTION (black); REDUCED EVOLUTION (gray)
► LEFT: nonresonant regime; RIGHT: resonant regime
TIME
NB: exponentially large Poincaré recurrence time.
TIME
SS(PERT. MASTER EQ)
SS
SS
FERMIONIC OSCILLATORS (fHO)˚14˚
● LAGRANGIAN & EQUATIONS OF MOTION FOR fHOs
i
N
iitt ttjjjttL ˆ)()(ˆ,ˆˆˆˆˆ)(
2
1
2
1ˆ)(ˆ
1
E
● DENSITY OPERATOR FOR fHO
aeZNNNNtaZ
t 1,ˆˆ,ˆˆˆ,1ˆ,ˆ,ˆ)(exp1
)(ˆ 2
..or:
jtjt ttˆˆ)(,ˆˆ)(
)(1
1,
1
1,ˆ)12()1()(ˆ th
a
en
enNnnt
a
● DENSITY OPERATOR IN THE FOCK SPACE REPRESENTATION
1,0,110)1(0)(ˆ :spaceFocknnt
Tomislav Prokopec and Jan Weenink, in preparationTomislav Prokopec and Jan Weenink, in preparation
ENTROPY OF FERMIONIC OSCILLATOR˚15˚
● ENTROPY OF fHO
)'(ˆ),(ˆ2
1)';(,
2tanh)(21);(2)( ttttF
atnttFt
● INVARIANT PHASE SPACE AREA:
: (statistical) number of particles)(tn
]1,1[,2
1ln
2
1
2
1ln
2
1)(
tS
]1,0[2
1),ln()1ln()1()(
nnnnntS
ALSO FOR FERMIONS: ENTROPY IS PARAMETRIZED BY THE PHASE SPACE INVARIANT (in units of ħ)(can be >0 or <0)
)(t
][
][
ENTROPY FOR 1+1 fHO˚16˚
ENTROPY
NB2: For 2 oscillators, small Poincare recurrence time: quick return to initial state.
► LEFT PANEL: WEAK COUPLING RIGHT: STRONG COUPLING
TIME
NB1: MAX ENTROPY ln(2) approached, but never reached.
TIME
ENTROPY
ENTROPY FOR 50+1 fHO˚17˚
ENTROPY
► LEFT: LOW TEMPERATURE RIGHT: HIGH TEMPERATURE
TIME
NB: exponentially large Poincaré recurrence time. When i<<1, Smax=ln(2) reached
TIME
random frequencies i[0,5]0
evenly distributed frequencies i[0,5]0
ENTROPY AND DECOHERENCE IN FIELD THEORIES
˚18˚
TWO INTERACTING SCALARS˚19˚
ACTION:
Can solve pertubatively for the evolution of (S) and (E)
O only sensitive to (near) coincident Gaussian (2pt) correlators. Cubic interaction generates non-Gaussian S-E correlations: Sng,corr, e.g. 3pt fn:
intSSSS
2222
2
1
2
1,
2
1
2
1
mxdSmxdS DD
,!32
1 32int
hxdS D
tot S corr S g,S ng,S corr g,corr ng,corr corrES S S S 0; S S S 0, S S S I 0
)()'()()'()()(~)''()'()( yxyxyxydhxxx D
NB: Expressible in terms of (non-coincident!) Gaussian S-E (2pt) correlators
EVOLUTION EQUATIONS˚20˚
baxxixyciyxyMdxxim Dab
c
cbacDab ,),'()';();()';( 322
In the in-in formalism: the keldysh propagator i is a 2x2 matrix:
ii
iii
► are the time ordered (Feynman) and anti-time ordered propagators ii ,
► are the Wightman functions ii ,
► is the self-energy (self-mass). At one loop:abM
2
2
);(2
);( yxiih
yxiM abab
Solve the above KB Eq.: spatially homogeneous limit; m=0
PROBLEM: scattering in presence of thermal bath
Kadanoff, Baym (1961); Hu (1987)
);( yxi ab► are the thermal correlators.
QUANTUM FIELD THEORY: 2 SCALARS˚20˚
1 LOOP SCHWINGER-DYSON EQUATION FOR & :
= +
= + +
NB: INITIALLY we put in a pure state at T=0 (vacuum) & in a thermal state at temp. T
0)',,(),,()',,(),,()',,( ccth,
'
cc
'
22222 tktkMdtktkZdkttkmkt
t
t
t
tc
t
1 LOOP KADANOFF-BAYM EQUATIONS (in Schwinger-Keldysh formalism):
)',,(),,()',,(),,()',,( cFc22222 tktkZtkFtkZdkttkFmkt
tt
0)',,(),,()',,(),,( cFth,
cth,
tktkMtkFtkMdt
► are the renormalised `wave function’ and self-massesFc,Fc, , MZ
iiiiiF2
1,
2
1 c STATISTICAL & CAUSAL CORRELATORS:
RESULTS FOR SCALARS
˚21˚
STATISTICAL CORRELATOR AT T>0˚23˚
► t-t’: DECOHERENCE DIRECTION
HIGH TEMPERATURE LOW TEMPERATURE
)';,( ttkF
˚24˚PHASE SPACE AREA AND
ENTROPY AT T>0
TIMETIME
HIGH TEMPERATURELOW TEMPERATURE
► Entropy reaches a value Sms we can (analytically) calculate.
DECOHERENCE RATE @ T>0˚25˚
2/)(exp1
2/)(exp1log
1632
1 22
χχφdec k
k
k
hh
► decoherence rate can be well approximated by perturbative one-particle decay rate:
0)( msdec
MIXING FERMIONS˚26˚
EQUATION OF MOTION (homogeneous space):
N
iioit tkmtkjtkjtkmk
1
0 ),(ˆ),(ˆ),,(ˆ),(ˆ)(
Helicity h is conserved: work with 2 spinors . Diagonalise:
223130 ||),,(ˆ),(ˆ)( mktkjmhk
tk hht
),(ˆ tkh
22
*12
1211
''''',
,),'(ˆ),,(ˆ,),(ˆ),(),(ˆexp1
)(ˆ
hkkhhhhhhk
hh tktktktktkZ
t
ENTROPY
..can be diagonalised
0
0,),(ˆ),(),(ˆexp
1)(ˆ
,
dh
dh
hk
dhh
d tktktkZ
t
a (diagonal) Fock representation:
),(ˆ),(ˆˆ,ˆ)12()1()(ˆ,)(ˆ)(ˆ tktkNNnnttt hhhkhkhkhkhkhk
hk
ENTROPY OF FERMIONIC FIELDS˚27˚
● FERMIONIC ENTROPY:
]1,0[2
1),ln()1ln()1()(,)()(
hkhkhkhkhkhkhk
hkhk
nnnnntStStS
FOR FERMIONIC FIELDS: ENTROPY PER DOF ALSO PARAMETRIZED BY THE PHASE SPACE INVARIANT
)(thk
][
hk
][
hk
)';(ˆ),;(ˆ2
1)';;(,
2tanh)(21);;(2)( tktkttkFtnttkFt hhh
hkhkhhk
]1,1[,2
1ln
2
1
2
1ln
2
1)(
hkhkhkhkhk
hktS
hk
RESULTS FOR FERMIONS
˚28˚
ENTROPY OF TWO MIXING FERMIONS˚29˚
● TOTAL ENTROPY OF THE SYSTEM FIELD
► LEFT PANEL: LOW TEMP. 0=1 RIGHT: HI TEMP: 0=1/2
HI TEMP: 0=1/10 ● TERMALISATION RATE
T
APPLICATIONS TO NEUTRINOS
˚30˚
NEUTRINOS ˚31˚
There are 3 active (Majorana) left-handed neutrino species, that mix and possibly violate CP symmetry.
Majorana condition implies that each neutrino has 2 dofs (helicities):
IN GAUSSIAN APPROXIMATION, ONE CAN DEFINE GENERAL INITIAL CONDITIONS FOR NEUTRINOS IN TERMS OF EQUAL TIME STATISTICAL CORRELATORS:
*2)(
Tc C
tt'(flavour),2,1,,)';(ˆ),;(ˆ2
1);;( '
jitktkttkF tthjhihij
Mark Pinckers, Tomislav Prokopec, in preparation
NEUTRINO OSCILLATIONS ˚32˚
IF INITIALLY PRODUCED IN A DEFINITE FLAVOUR, NEUTRINOS DO OSCILLATE:
eV1032.2,eV106.7 3213
223
5212
mmm
861.0)2(sin,97.0)2(sin,10.0)2(sin 122
232
132
BLUE = MUON ; RED = TAU ; BLACK=ELECTRON
INITIAL ELECTRON
INITIAL MUON
OSCILLATIONOS ARE A MANIFESTATION OF QUANTUM COHERENCE, BUT ARE NOT GENERIC!
ExmP 4/sin)2(sin 2212
212
˚34˚
),(2
1ˆˆ),(,0ˆˆ&)2,1(,1 tkFtkninn ihihihihiiii
EXAMPLE A:
other (mixed) correllators vanish.
Q: can one construct such a state in laboratory?
NB: albeit neutrinos coming e.g. from the Sun are coherent and do oscillate, when averaged over the source localtion, oscillations tend to cancel,and one observes neutrino deficit, but no oscillations.
NEUTRINOS NEED NOT OSCILLATE WE FOUND GENERAL CONDITIONS ON F’s UNDER WHICH NEUTRINOS DO NOT OSCILLATE.
EXAMPLES (WHEN MAJORANA NEUTRINOS DO NOT OSCILLATE):
COSMIC NEUTRINO BACKGROUND˚34˚
)2,1(,1ˆ,ˆ2
1ˆ,ˆ
2
1
inn
khFF
kh iiiiiiii
EXAMPLE B: thermal cosmic neutrino background (CB):
NB1: CB neutrinos do not oscillates (by assumption)
NB2: CB violates both lepton number and helicity and CB contains a calculable lepton neutrino condensate.
NB3: A similar story holds for supernova neutrinos (they are believed to be approximately thermalised).
NB4: Can construct a diagonal thermal density matrix for CB (that is neither diagonal in helicity nor in lepton number)
In flavour diagonal basis:
K73.2,K95.1)11/4( 3/1 TTTCurrent temperature:
APPLICATIONS: Need to understand better how neutrinos affect CB
CONCLUSIONS˚35˚
Correlator approach to decoherence is based on perturbative evolution of 2 point functions & neglecting observationally inaccessible (non-Gaussian) correlators.
DECOHERENCE: the physical process by which quantum systems become (more) classical, i.e. they become classical stochastic systems.
Our methods permit us to study decoherence/classicization in realistic (quantum field theoretic) settings.There is no classical domain in the usual sense: phase space area – and therefore the `size’ of the system – never decreases in time.Particular realisations of a stochastic system (recall: large scale structure of our Universe) behave (very) classically.
Von Neumann entropy (of a suitable reduced sub-system) is a good quantitative measure of decoherence, and can be applied to both bosonic and fermionic systems.
APPLICATIONS˚35b
˚
Quantum information
Classicality of scalar & tensor cosmological perturbations (observable in CMB?)
Thermal cosmic neutrino background: - relation to lepton number and baryogenesis via leptogenesis
Lab experiments on neutrinos; neutrinos from supernovae
Baryogenesis: CP violation (requires coherence)
INTUITIVE PICTURE: WIGNER FUNCTION
˚36˚
GAUSSIAN STATE (momentum space: per mode):
WIGNER FUNCTION:
22t tt'2 t' t t' t
4F(t,t) F(t,t ' ) F(t,t ' )
g
1 1 1 1S Log Log
2 2 2 2
ENTROPY ~ effective phase space area of the state
2/)'(],,',[e)'(],,W[ )'( xxxtxxxxtpx xxip D
p
x
WIGNER FUNCTION: SQUEEZED STATES
˚37˚
PURE STATE (=1,Sg=0) MIXED STATE (>1,Sg>0)
EVOLUTI ON
NB: ORIGIN OF ENTROPY GROWTH: neglected S-E (nongaussian) correlators
STATISTICAL ENTROPY: g
1S (n 1)Log n 1 nLog n , n : uncorr.regions
2
GENERALISED UNCERTAINTY RELATION:
2
2 2 22
4 1x p x, p 1 n 0, S 0
2
WIGNER FUNCTION AS PROBABILITY˚38˚
WIGNER ENTROPY (Wigner function = quasi-probability)
GAUSSIAN ENTROPY:
2
1),(
2
11)ln()ln()1ln()1( 2
g
nnO
nnnnnnS
1)ln(W nS
THE AMOUNT OF QUANTUMNESS IN THE STATE: the difference of the two entropies:
1),(6
1
2
1 32g nnOnn
SSS W
WIGNER FUNCTION OF NONGAUSSIAN STATE
˚39˚
POSITIVE KURTOSIS : NEGATIVE KURTOSIS :
2
2 2 22
4 1x p x, p 1 n 0, S 0
2
Q: can non-Gaussianity – e.g. a negative curtosis – break the Heiselberg uncertainty relation?
Naïve Answer: YES(!?); but it is probably wrong.
CLASSICAL STOCHASTIC SYSTEMS
˚40˚
DISTRIBUTION OF GALAXIES IN OUR UNIVERSE (2dF): ● amplified vacuum fluctuations ● we observe one realisation (breaks homogeneity of the vacuum)
BROWNIAN PARTICLE (3 dim)● exhibits walk of a drunken man/woman● distance traversed: d ~ t
NB: first order phase transitions also spont.break spatial homogeneity of a state.
NB2: planetary systems are stochastic, and essentially unstable.
RESULTS: CHANGING MASS
˚41˚
CHANGING MASS CASE˚42˚
► RELEVANCE: ELECTROWEAK SCALE BARYOGENESIS: axial vector current is generated by CP violating scatterings of fermions off bubble walls in presence of a plasma. ► Since the effect vanishes when ħ0, quantum coherence is important.
► ANALOGOUS EFFECT: double slit with electrons in presence of air
BUBBLE WALL: m²(t)
TIME: t
PROBLEMS:
► non-equilibrium dynamics in a plasma at T>0;
► non-adiabatically changing mass term;
► apply to Yukawa coupled fermions.
CHANGING MASS: STATISTICAL PROPAGATOR
˚43˚
► NOTE: ADDITIONAL OSCILLATORY STRUCTURE
DELTA: FREE CASE, CHANGING MASS
˚44˚
► CONSTANT GAUSSIAN ENTROPY
TIME
► the state gets squeezed, but the phase space area is conserved
EXACT SOLUTION: in terms of hypergeometric functions
Pure + frequency mode at t- becomes a mixture of + & - frequencysolutions at t+ Mixing amplitude: (t)
Particle production:
inout
outin
22
2
1,
/sinh/sinh
/sinh
kn
outin
2
in
in
,,2
12
n
MASS CHANGE AT T>0 ˚45˚
LOW T MASS INCREASE: T=/2, k=, h=4, m= 2
LOW T MASS DECREASE: T=/2, k=, h=4, m=2
timetime
NB: ENTROPY CHANGES AT THE ONE PARTICLE DECAY RATEdec
NB2: MASS CHANGES MUCH FASTER THAN ENTROPY: dec/ mm
MASS CHANGE AT T>0 ˚46˚
HIGH T MASS INCREASE: T=2, k=, h=3, m= 2
HIGH T MASS DECREASE: T=2, k=, h=3, m=2
time
EVOLUTION OF SQUEEZED STATES ˚47˚
HIGH T: 2r=ln(5), =/2 T=2m, h=3m, k=m
LOW T: 2r=ln(5), =0T=2m, h=3m, k=m
timetime
NB: ADDITIONAL OSCILLATIONS DECAY AT THE RATE = dec.
► of relevance for baryogenesis: changing mass induces squeezing (coherent effect)
QUANTUM COHERENCE IS NOT DESTROYED BY THERMAL EFFECTS.
CONJECTURE: THIN WALL BG UNAFFECTED BY THERMAL EFFECTS.
► ► related work: Herranen, Kainulainen, Rahkila (2007-10) related work: Herranen, Kainulainen, Rahkila (2007-10)
KADANOFF-BAYM EQUATIONS˚48˚
0)',,(),,()',,(),,()',,( ccth,
'
cc
'
22222 tktkMdtktkZdkttkmkt
t
t
t
tc
t
IMPORTANT STEPS: calculate 1 loop self-masses renormalise using dim reg solve for the causal and statistical correlators (must be done numerically, since it involves memory effects)
calculate the (gaussian) entropy of (S)
)',,(2
1)',,(),',,()',,( ttkiittkFttkiittki c
► here: m² is the renormalised mass term (the only renormalisation needed at 1loop)
Fc,Fc, , MZ
KB equations can be written in a manifestly causal and real form:Berges, Cox (1998); Koksma, TP, Schmidt (2009)
22t tt'2 t' t t' t
4F(t,t) F(t,t ' ) F(t,t ' )
g
1 1 1 1S Log Log
2 2 2 2
)',,(),,()',,(),,()',,( cFc22222 tktkZtkFtkZdkttkFmkt
tt
0)',,(),,()',,(),,( cFth,
cth,
tktkMtkFtkMdt
► are the renormalised `wave function’ and self-masses
SELF-MASSES˚49˚
)'()4)(3(16
12
)';(2/
42
cct, xxi
DD
Dih
xxiM DD
D
► there are also thermal contributions to the self-masses (which are complicated)
LOCAL VACUUM MASS COUNTERTERM
RENORMALISED VACUUM SELF-MASSES
)',,()()',,( 22 ttkiZkttkiM abt
ab
|)|2si(|)|2ci(2||2
log64
||2
||2
2
tkitkeit
ke
hiZ tik
Etik
|)|2si()sign(|)|2ci()sign(2||2
log64 22
2
tktitketit
ke
k
hiZ tik
Etik
► CURIOUSLY: we could not find these expressions in literature or textbooks
► there is also the subtlety with KB eqs: in practice t0=- should be made finite. But then there is a boundary divergence at t=t0, which can be cured by (a) adiabatically turning on coupling h, or (b) by modifying the initial state.
˚50˚
h=4m, k= m
PHASE SPACE AREA AND ENTROPY AT T=0
ENTROPY
TIMETIME
TIME
► evolution towards the new (interacting) vacuum with stationary ms (calculated)
ms
ms
► initial conditions `forgotten’
► ms reached at perturbative rate=decoherence/entropy growth rate:
2
treepert,dec 32
1 h
► wiggles (in part) due to imperfect memory kernel
˚51˚ENTROPY AT T>0
NB: COUPLING h IS PERTURBATIVE UP TO h~3 (k²+m² )
● ms as a function of coupling h, T=2m, k=m
LOW TEMPERATURE vs VACUUM CASE:T= m /10 (black) & T=0 (gray), h=4m, k=m
● ENTROPY
TWO POINT FUNCTION˚52˚
QUANTUM COMPUTATION˚53˚
CLASSICAL LOGICAL GATES
Feynman; Shore (factoring into primes)Feynman; Shore (factoring into primes)
E.g. NAND GATE 2 STATE SYSTEM WAVE FUNCTION:
0111
1010
1101
1000
QUANTUM LOGICAL GATES
NOT GATE
10
01
1,1022
quantum NOT GATE
01
10NOT 1
* general q-gate: any `rotation’ on the Bloch sphere; e.g. Pauli matrices: rotation around x, y and z axes)
Bloch sphere: {{,} | ||²+||²=1}
{1,0}
{0,1}
MAIN PROBLEM of quantum computation: how to reduce decoherence of q-gates
A MEASURE OF DECOHERNECE: GAUSSIAN VON NEUMANN ENTROPY
˚54˚
STATISTICAL (HADAMARD) 2-pt GREEN FUNCTION:
CAUSAL (SPECTRAL) FUNCTION (PAULI-JORDAN, SCHWINGER) 2-pt GREEN FUNCTION:
one solves the perturbative dynamical equations for of S+E c &F
PROGRAM:
one calculates the Gaussian von Neumann entropy Sg of S:
g
1 1 1 1S Log Log
2 2 2 2
Gaussian density matrix:
)])x(t'x(t),[Tr();'( tti c
)}x(t'x(t),{
2
1Tr);'( ttF
2
'''22 )';F()';F();F(
2)( ttttttt ttttttt
')(2')()(exp);',( 22
gauss xxtcxtbxtaNtxx
INTERMEDIATE SUMMARY˚55˚
CONVENTIONAL APPROACH:
S+E E weakly coupledEvolve Ered Tr S red redS Tr log 0
NEW FRAMEWORK:
E weakly coupledS+E Evolve 2pt correlators for S & E: perturbatively c, F
g,S S SS Tr log 0
tot S corr S g,S ng,S corr g,corr ng,corr corrES S S S 0; S S S 0, S S S I 0
BROWNIAN PARTICLE ˚56˚
])(/[,1/log)2/1( 2200 TkmtttS B LATE TIME ENTROPY: grows without limit
)'(2)'()(),()(' ttTktFtFtFxVvvm B
DYNAMICS: LANGEVIN EQUATION
► Describes motion of a Brownian particle (Einstein); of a drunken man/woman; also: inflaton fluctuations during inflation (Starobinsky; Woodard; Tsamis; TP)
► v=dx/dt; F(t)=Markovian (noise), V(x)= potential, = friction coefficient
Q: How can we understand this unlimited growth of phase space area?
WHEN V(x)=0: t
BROWNIAN PARTICLE 2˚57˚
Consider a free moving quantum particle (described by a wave packet)
But x keeps growing!: explains the (unlimited) growth of phase space area.
Quantum evolution: preserves the minimum phase space area xp=ħ/2
p(t)
x(t)
EARLY TIME t LATE TIME t’>t
x(t’)
p(t’)
BROWNIAN PARTICLE gets thermal kicks: keeps p constant! 22
2 Tk
m
p B