holography and mottness: a discrete...
TRANSCRIPT
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Holography and Mottness: a Discrete Marriage
Thanks to: NSF, EFRC (DOE)
M. Edalati R. G. LeighKa Wai Lo
Seungmin Hong
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emergentgravity
Mott problem
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Unsolved condensed matter problems
physics at strong coupling
magnetismin metals
nematicsheavy fermions
turbulence
quantum criticality
high T_c (cuprate, organics,...
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What computational tools do we have forstrongly correlated electron systems?
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interacting
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interacting
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non-interacting interacting
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DMFT
non-interacting interacting
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DMFT
the only differencebetween this and
a theory is that this is not a theory
non-interacting interacting
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DMFT
the only differencebetween this and
a theory is that this is not a theory
non-interacting interacting
why doesthis workat long
wavelengths?
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UV
QFT
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UV
QFTIR ??
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UV
QFTIR ??
Wilsonianprogram
(fermions: new degrees of
freedom)
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UV
QFTIR ??
Wilsonianprogram
(fermions: new degrees of
freedom)
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UV
QFT
g = 1/ego
coupling constant
IR ??
Wilsonianprogram
(fermions: new degrees of
freedom)
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UV
QFT
g = 1/ego
coupling constant
IR ??
Wilsonianprogram
(fermions: new degrees of
freedom)
dg(E)
dlnE= β(g(E))
locality in energy
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UV
QFT
g = 1/ego
coupling constant
IR ??
Wilsonianprogram
(fermions: new degrees of
freedom)
dg(E)
dlnE= β(g(E))
locality in energy
implement E-scaling with an extra dimension
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UV
QFT
g = 1/ego
coupling constant
IR ??
gauge-gravity duality(Maldacena, 1997)
UV
QFTIR gravity
Wilsonianprogram
(fermions: new degrees of
freedom)
dg(E)
dlnE= β(g(E))
locality in energy
implement E-scaling with an extra dimension
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ZQFT = e−Son−shellADS (φ(φ∂ADS=JO
))Claim:
UV
QFTIR
φfields
e�ddxφOO
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ZQFT = e−Son−shellADS (φ(φ∂ADS=JO
))Claim:
UV
QFTIR
operatorsOφ
fields
e�ddxφOO
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What holography does for you?
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What holography does for you?
RG equations
Landau-Wilson
Hamiltonian
long-wavelengths
ξt ∝ ξz
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What holography does for you?
holography
RG equations
Landau-Wilson
Hamiltonian
long-wavelengths
ξt ∝ ξz
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What holography does for you?
holography
RG=GR
RG equations
Landau-Wilson
Hamiltonian
long-wavelengths
ξt ∝ ξz
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What holography does for you?
holography
RG=GR
strong-coupling is easy
RG equations
Landau-Wilson
Hamiltonian
long-wavelengths
ξt ∝ ξz
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What holography does for you?
holography
RG=GR
strong-coupling is easy
microscopic UV model not easy(need M-theory)
RG equations
Landau-Wilson
Hamiltonian
long-wavelengths
ξt ∝ ξz
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What holography does for you?
holography
RG=GR
strong-coupling is easy
microscopic UV model not easy(need M-theory)
RG equations
Landau-Wilson
Hamiltonian
long-wavelengths
ξt ∝ ξz
so what(currents,
symmetries)
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Can holography solve the Mott problem?
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Half-filledband
Free electrons
U
ε
µ
gap with no symmetrybreaking!!
charge gap
U � t
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Why is the Mott problem important?
interactions dominate:Strong Coupling Physics
U/t = 10� 1
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cm-1
T=360 K
T=295 K
σ(ω) Ω-1cm-1
VO2
M. M. Qazilbash, K. S. Burch, D. Whisler, D. Shrekenhamer, B. G. Chae, H. T. Kim, and D. N. Basov PRB 74, 205118 (2006)
transferof spectralweight to
high energiesbeyond any ordering
scale
Recall, eV = 104K
∆ = 0.6eV > ∆dimerization(Mott, 1976) ∆
Tcrit≈ 20
Experimental facts: Mottness
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dynamically generated gap: Mott gap (for probe fermions)
What bulk gravitational theory gives rise to a gap in ImG without
`spontaneous’ symmetry breaking?
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S0
Charged system probe
JψOψ
UV
Jµ
what has been done?
MIT, Leiden, McMaster,...
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S0
Charged system probe
JψOψ
UV
Jµ
RN-AdSds2, At
what has been done?
MIT, Leiden, McMaster,...
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ψ Dirac Eq.
S0
Charged system probe
JψOψ
UV
Jµ
RN-AdSds2, At
what has been done?
MIT, Leiden, McMaster,...
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ψ Dirac Eq.
S0
Charged system probe
JψOψ
UV
Jµ
RN-AdSds2, At
what has been done?
MIT, Leiden, McMaster,...
in-falling boundary conditions
Retarded Green function:G =b
a
ψ(r → ∞) ≈ arm + br−m
=f(UV (k_F), IR (q,m))
a=0 defines FS
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boundary physics:AdS2 ×R2
ds2 =L22
ζ2�−dτ2 + dζ2
�+
r20R2
d�x2
ζ = ωL22/(r − r0)
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boundary physics:AdS2 ×R2
ds2 =L22
ζ2�−dτ2 + dζ2
�+
r20R2
d�x2
ζ = ωL22/(r − r0)
AdS2
O±G(ω) ∝ ω2ν±
O GR(k,ω) = f(G(ω))
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boundary physics:AdS2 ×R2
ds2 =L22
ζ2�−dτ2 + dζ2
�+
r20R2
d�x2
{�x, τ, ζ} → {�x,λτ,λζ}
ζ = ωL22/(r − r0)
AdS2
O±G(ω) ∝ ω2ν±
O GR(k,ω) = f(G(ω))
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boundary physics:AdS2 ×R2
�x → λ(1/z=∞)�x = �x
S ∝ T 2/z �= 0 T → 0
finite T=0 entropy
ds2 =L22
ζ2�−dτ2 + dζ2
�+
r20R2
d�x2
{�x, τ, ζ} → {�x,λτ,λζ}
ζ = ωL22/(r − r0)
AdS2
O±G(ω) ∝ ω2ν±
O GR(k,ω) = f(G(ω))
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√−giψ̄(D −m)ψ
?? Mott gap
AdS-RNMIT, Leiden group
G(ω, k) =Z
vF (k − kF )− ω − hω lnω
How to Destroy the Fermi surface?
decoherence
marginal Fermi liquid
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√−giψ̄(D −m)ψ
?? Mott gap
AdS-RNMIT, Leiden group
G(ω, k) =Z
vF (k − kF )− ω − hω lnω
How to Destroy the Fermi surface?
decoherence
marginal Fermi liquid
log-oscillatory regime
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Sprobe(ψ, ψ̄) =
�ddx
√−giψ̄(ΓMDM −m+ · · · )ψ
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Sprobe(ψ, ψ̄) =
�ddx
√−giψ̄(ΓMDM −m+ · · · )ψ
what is hidden here?
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√−giψ̄(D −m− ipF )ψconsider
FµνΓµν
Sprobe(ψ, ψ̄) =
�ddx
√−giψ̄(ΓMDM −m+ · · · )ψ
what is hidden here?
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QED anomalous magnetic moment of an electron (Schwinger 1949)
√−giψ̄(D −m− ipF )ψconsider
FµνΓµν
Sprobe(ψ, ψ̄) =
�ddx
√−giψ̄(ΓMDM −m+ · · · )ψ
what is hidden here?
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QED anomalous magnetic moment of an electron (Schwinger 1949)
√−giψ̄(D −m− ipF )ψconsider
FµνΓµν
Sprobe(ψ, ψ̄) =
�ddx
√−giψ̄(ΓMDM −m+ · · · )ψ
what is hidden here?
fermions in RN Ads_{d+1} coupled to a gauge fieldthrough a dipole interaction
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black hole
gravitons
electrons
boundary =???
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P=0
Fermi surfacepeak
How is the spectrum modified?
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P=0
Fermi surfacepeak
How is the spectrum modified?
P
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P=0
Fermi surfacepeak
How is the spectrum modified?
−1.54 < p < −0.53
1 > νkF > 1/2
�ω ∝ k − kF�ω ∝ (k − kF )
2νkF
`Fermi Liquid’
P
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P=0
Fermi surfacepeak
How is the spectrum modified?
P
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P=0
Fermi surfacepeak
How is the spectrum modified?
p = −0.53
νkF = 1/2
−0.53 < p < 1/√6
MFL
1/2 > νkF > 0
�ω = �ω ∝ (k − kF )1/(2νkF
)
NFL
P
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P=0
Fermi surfacepeak
How is the spectrum modified?
P
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P=0
Fermi surfacepeak
How is the spectrum modified?P > 4.2 P
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P=0
Fermi surfacepeak
How is the spectrum modified?P > 4.2 P
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P=0
Fermi surfacepeak
dynamically generated gap:
How is the spectrum modified?P > 4.2 P
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P=0
Fermi surfacepeak
dynamically generated gap:
spectralweight transfer
How is the spectrum modified?P > 4.2 P
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P=0
Fermi surfacepeak
dynamically generated gap:
spectralweight transfer
How is the spectrum modified?
Gubser, Gauntlett, 2011 similar results
P > 4.2 P
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Sonner, 2011 (top-down gravitino model)
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Mechanism?
log-oscillatory
k_F moves into log-oscillatory region: IRacquires a complex dimensionO±
UV
QFTIR
ψ ∝ ar∆ + br−∆
operatorsO
where is k_F
![Page 64: Holography and Mottness: a Discrete Marriagepeople.physics.illinois.edu/Phillips/images/talks/kitpnov142011talk.pdf · Why is the Mott problem important? interactions dominate: Strong](https://reader036.vdocuments.us/reader036/viewer/2022081617/60215360aa6c584a724cbbe1/html5/thumbnails/64.jpg)
near horizon
p: time-reversal breaking mass term (in bulk)
ψI±(ζ) = ψ(0)I±(ζ) + ω ψ(1)
I±(ζ) + ω2ψ(2)I±(ζ) + · · ·
−ψ(0)��I± (ζ) = iσ2
�1 +
qedζ
�− L2
ζ
�mσ3 +
�ped ±
kL
r0
�σ1
�ψ(0)I±(ζ),
m2k = m2 +
�ped ±
kL
r0
�2
ed = 1/�2d(d− 1)
radial Dirac Equation
ν±k =�m2
k±L22 − q2e2d − i�, δ± = ν±k + 1/2
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near horizon
p: time-reversal breaking mass term (in bulk)
ψI±(ζ) = ψ(0)I±(ζ) + ω ψ(1)
I±(ζ) + ω2ψ(2)I±(ζ) + · · ·
−ψ(0)��I± (ζ) = iσ2
�1 +
qedζ
�− L2
ζ
�mσ3 +
�ped ±
kL
r0
�σ1
�ψ(0)I±(ζ),
m2k = m2 +
�ped ±
kL
r0
�2
ed = 1/�2d(d− 1)
radial Dirac Equation
ν±k =�m2
k±L22 − q2e2d − i�, δ± = ν±k + 1/2
scaling dimension is complex!
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What does a complex scaling dimension mean?
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what about complex ∆
O = µ(λ)O(λr)
continuousscale invariance
1 = µ(λ)λ∆
∆ = − lnµ
lnλ
is real, independent of
scale
∆
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1 = µλ∆
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1 = µλ∆e2πin =
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1 = µλ∆e2πin =
Discrete scale invariance (DSI)
n=0:CSI
∆ = − lnµ
lnλ+
2πin
lnλ
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1 = µλ∆e2πin =
Discrete scale invariance (DSI)
n=0:CSI
∆ = − lnµ
lnλ+
2πin
lnλ
scaling dimension depends on scale
λn = λn
magnification
![Page 72: Holography and Mottness: a Discrete Marriagepeople.physics.illinois.edu/Phillips/images/talks/kitpnov142011talk.pdf · Why is the Mott problem important? interactions dominate: Strong](https://reader036.vdocuments.us/reader036/viewer/2022081617/60215360aa6c584a724cbbe1/html5/thumbnails/72.jpg)
example
![Page 73: Holography and Mottness: a Discrete Marriagepeople.physics.illinois.edu/Phillips/images/talks/kitpnov142011talk.pdf · Why is the Mott problem important? interactions dominate: Strong](https://reader036.vdocuments.us/reader036/viewer/2022081617/60215360aa6c584a724cbbe1/html5/thumbnails/73.jpg)
example
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example
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example
n iterations
number of segments
2n3−n
length
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example
n iterations
number of segments
2n3−n
length
scale invariance onlyfor λp = 3p
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example
n iterations
number of segments
2n3−n
length
scale invariance onlyfor λp = 3p
discrete scale invariance: D = − ln 2
ln 3+
2πin
ln 3
![Page 78: Holography and Mottness: a Discrete Marriagepeople.physics.illinois.edu/Phillips/images/talks/kitpnov142011talk.pdf · Why is the Mott problem important? interactions dominate: Strong](https://reader036.vdocuments.us/reader036/viewer/2022081617/60215360aa6c584a724cbbe1/html5/thumbnails/78.jpg)
discrete scale invariance
hidden scale(length, energy,...)
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toy model: merging of UV and IR fixed points
β = (α− α∗)− (g − g∗)2
BKT transition Kaplan, arxiv:0905.4752
g± = g∗ ±√α− α∗
β
gUV ≡ g+gIR ≡ g−
α > α∗
α = α∗
g∗
α < α∗
ΛIR = ΛUVe−π/
√α∗−α
are complex(conformality lost)g±
DSI
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G =β−(0, k)
α−(0, k)
p=-0.4 p=0.0
p=0.2 p=1.0
no poles outside log-oscillatory region for p > 1/√6
Mott physics and DSI are linked!
![Page 81: Holography and Mottness: a Discrete Marriagepeople.physics.illinois.edu/Phillips/images/talks/kitpnov142011talk.pdf · Why is the Mott problem important? interactions dominate: Strong](https://reader036.vdocuments.us/reader036/viewer/2022081617/60215360aa6c584a724cbbe1/html5/thumbnails/81.jpg)
is there an instability? (violation of BF bound)
x
y
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is there an instability? (violation of BF bound)
x
y
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is there an instability? (violation of BF bound)
E → E + iγ γ > 0
x
y
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is there an instability? (violation of BF bound)
E → E + iγ γ > 0
x
y �φ� �= 0
condensate(bosonic)
![Page 85: Holography and Mottness: a Discrete Marriagepeople.physics.illinois.edu/Phillips/images/talks/kitpnov142011talk.pdf · Why is the Mott problem important? interactions dominate: Strong](https://reader036.vdocuments.us/reader036/viewer/2022081617/60215360aa6c584a724cbbe1/html5/thumbnails/85.jpg)
is there an instability? (violation of BF bound)
E → E + iγ γ > 0
x
y �φ� �= 0
condensate(bosonic)
does this happen for fermions?
![Page 86: Holography and Mottness: a Discrete Marriagepeople.physics.illinois.edu/Phillips/images/talks/kitpnov142011talk.pdf · Why is the Mott problem important? interactions dominate: Strong](https://reader036.vdocuments.us/reader036/viewer/2022081617/60215360aa6c584a724cbbe1/html5/thumbnails/86.jpg)
quasi-normal modes
Imω < 0no instability
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quasi-normal modes
Imω < 0no instability
quasi-particle residue
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quasi-normal modes
Imω < 0no instability
quasi-particle residue
but the residue drops to zero:
opening of a gap
GR(ω,k) =b(0) + ωb1Gk(ω)
a(0) + ωa(1)Gk(ω)
![Page 89: Holography and Mottness: a Discrete Marriagepeople.physics.illinois.edu/Phillips/images/talks/kitpnov142011talk.pdf · Why is the Mott problem important? interactions dominate: Strong](https://reader036.vdocuments.us/reader036/viewer/2022081617/60215360aa6c584a724cbbe1/html5/thumbnails/89.jpg)
S(ϕ) + SD(ζ) + η5
�dd+1x
√−gϕζ̄CΓ5ζ̄T + cc
majorana coupling kills qp peaksthrough coupling to scaling dimension of spinor field
η5 = 0.075
η5 = 0.025
![Page 90: Holography and Mottness: a Discrete Marriagepeople.physics.illinois.edu/Phillips/images/talks/kitpnov142011talk.pdf · Why is the Mott problem important? interactions dominate: Strong](https://reader036.vdocuments.us/reader036/viewer/2022081617/60215360aa6c584a724cbbe1/html5/thumbnails/90.jpg)
Finite Temperature Mott transition from Holography
∆
Tcrit≈ 20 vanadium oxide
T/µ = 5.15× 10−3 T/µ = 3.92× 10−2
∆
Tcrit≈ 10
![Page 91: Holography and Mottness: a Discrete Marriagepeople.physics.illinois.edu/Phillips/images/talks/kitpnov142011talk.pdf · Why is the Mott problem important? interactions dominate: Strong](https://reader036.vdocuments.us/reader036/viewer/2022081617/60215360aa6c584a724cbbe1/html5/thumbnails/91.jpg)
spectral weighttransfer
UV-IR mixing
T ↑
p1
p3
σ(ω) Ω-1cm-1
VO2
![Page 92: Holography and Mottness: a Discrete Marriagepeople.physics.illinois.edu/Phillips/images/talks/kitpnov142011talk.pdf · Why is the Mott problem important? interactions dominate: Strong](https://reader036.vdocuments.us/reader036/viewer/2022081617/60215360aa6c584a724cbbe1/html5/thumbnails/92.jpg)
discrete scale invariancein energy
G(ω, k) = G(ωλn, k)
emergent IR scale
energy gap: Mott gap (Mottness)
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discrete scale invariancein energy
G(ω, k) = G(ωλn, k)
emergent IR scale
energy gap: Mott gap (Mottness)
no condensate
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continuous scale invariance
discrete scale invariancein energy
is this the symmetry that is ultimatelybroken in the Mott
problem?
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a.) yes
b.) no
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a.) yes
b.) no
holography
![Page 97: Holography and Mottness: a Discrete Marriagepeople.physics.illinois.edu/Phillips/images/talks/kitpnov142011talk.pdf · Why is the Mott problem important? interactions dominate: Strong](https://reader036.vdocuments.us/reader036/viewer/2022081617/60215360aa6c584a724cbbe1/html5/thumbnails/97.jpg)
a.) yes
b.) no
holography
VO_2, cuprates,...
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a.) yes
b.) no
holography
VO_2, cuprates,...
Does scaling in VO_2 obey: ΛIR = ΛUVe−π/
√Uc−U
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a.) yes
b.) no
holography
VO_2, cuprates,...
if yes: holography has solved the Mott problem
Does scaling in VO_2 obey: ΛIR = ΛUVe−π/
√Uc−U
![Page 100: Holography and Mottness: a Discrete Marriagepeople.physics.illinois.edu/Phillips/images/talks/kitpnov142011talk.pdf · Why is the Mott problem important? interactions dominate: Strong](https://reader036.vdocuments.us/reader036/viewer/2022081617/60215360aa6c584a724cbbe1/html5/thumbnails/100.jpg)
f(U) = c1sgn(δU)|δU |1/δ + c2|δ|2/δ + c3δU +Dc
Semon, Tremblay, arxiv:1110.6195
4 parameters
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f(U) = c1sgn(δU)|δU |1/δ + c2|δ|2/δ + c3δU +Dc
Semon, Tremblay, arxiv:1110.6195
4 parameters
?
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f(U) = c1sgn(δU)|δU |1/δ + c2|δ|2/δ + c3δU +Dc
Semon, Tremblay, arxiv:1110.6195
ΛIR = ΛUVe−γ/
√Uc−U
4 parameters
?
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f(U) = c1sgn(δU)|δU |1/δ + c2|δ|2/δ + c3δU +Dc
Semon, Tremblay, arxiv:1110.6195
ΛIR = ΛUVe−γ/
√Uc−U
4 parameters
??