six lectures about (advanced) statistical...
TRANSCRIPT
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LECTURES ABOUT
(ADVANCED) STATISTICAL
PHYSICS
T.S.Biró, MTA Wigner Research Centre for Physics, Budapest
Lectures given at: University of Johannesburg, South-Africa,
November 26 – November 29, 2012.
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1. Ancient Thermodynamics (… - 1870)
2. The Rise of Statistical Physics (1890 – 1920)
3. Modern (postwar) Problems (1940 – 1980)
4. Corrections (1950 – 2005)
5. Generalizations (1960 – 2010)
6. High Energy Physics (1950 – 2010)
2
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LECTURE FIVE ABOUT
(ADVANCED) STATISTICAL
PHYSICS
T.S.Biró, MTA Wigner Research Centre for Physics, Budapest
Lectures given at: University of Johannesburg, South-Africa,
November 29, 2012.
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FAQ
• What is actually non-perturbative at T > Tc ? (low Q2 pairs)
• What is non-particle like (stringy) at T > Tc ? (interaction)
• Are all color charges stringed at T > Tc? No! (a small fraction
suffices for the effect.)
• Asymptotic freedom is incomplete at any finite temperature. Why
and what is the quantitative measure of this effect?
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Arguments
Non-perturbative effects at arbitrary high temperature:
1. Thermal distribution of Q²
2. NP order parameter: cut-off in Q²
3. Its thermal expectation value order of NP effects
4. high-T expansion
5. high-T NP terms in EoS (pressure, int.mesure)
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Pressure: NP effects at any T
)(1
)()0(22)(
)()(
)()(
222
2
2
/
00
22
0
2222
T
TfT
pppp
dxxfdQQP
dQQPpdQQPpp
NPpp
T
NPP
If it were f(0) = 0, then the QGP pressure would be free of NP effects!
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Thermal distribution of Q²
T
QK
T
Q
T
QK
T
Q
TQP
eEEddEdE
EEQeEEddEdEQP
EE
EE
22
2
13
3
2
2
)(2
2
2
121
21
2)(2
2
2
1212
264
1)(
)cos1(2)(
21
21
Q² 9T²
1/16T²
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Thermal expectation of NP order parameter
2
0
2222 )( dQQPQ
Q²
Λ²
1
T²
Λ²
1
22 16/~ T
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NP effects at high T in the EoS
22
224
31
23 Tcpe
TcTp
NP
NP
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WIKIPEDIA: TSALLIS ENTROPY In physics, the Tsallis entropy is a generalization of the
standard Boltzmann-Gibbs entropy. It was introduced in 1988
by Constantino Tsallis [1] as a basis for generalizing the
standard statistical mechanics. In the scientific literature, the
physical relevance of the Tsallis entropy was occasionally
debated. However, from the years 2000 on, an increasingly
wide spectrum of natural, artificial and social complex
systems have been identified which confirm the predictions
and consequences that are derived from this nonadditive
entropy, such as nonextensive statistical mechanics [2], which
generalizes the Boltzmann-Gibbs theory.
Among the various experimental verifications and applications
presently available in the literature, the following ones deserve
a special mention:
The distribution characterizing the motion of cold atoms in
dissipative optical lattices, predicted in 2003 [3] and observed
in 2006 [4].
The fluctuations of the magnetic field in the solar wind
enabled the calculation of the q-triplet (or Tsallis triplet) [5].
The velocity distributions in driven dissipative dusty plasma
[6]. Spin glass relaxation [7].
Trapped ion interacting with a classical buffer gas [8].
High energy collisional experiments at LHC/CERN (CMS,
ATLAS and ALICE detectors) [9] [10] and RHIC/Brookhaven
(STAR and PHENIX detectors) [11].
Among the various available theoretical results which clarify
the physical conditions under which Tsallis entropy and
associated statistics apply, the following ones can be selected:
Anomalous diffusion [12] [13].
Uniqueness theorem [14].
Sensitivity to initial conditions and entropy production at the
edge of chaos [15] [16].
Probability sets which make the nonadditive Tsallis entropy to
be extensive in the thermodynamical sense [17].
Strongly quantum entangled systems and thermodynamics [18].
Thermostatistics of overdamped motion of interacting
particles [19] [20].
Nonlinear generalizations of the Schroedinger, Klein-Gordon
and Dirac equations [21].
For further details a bibliography is available at
http://tsallis.cat.cbpf.br/biblio.htm
15
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Some applications
– Reservoir = QGP at constant volume
– Reservoir = QGP at constant pressure
– Reservoir = QGP at constant entropy
– Reservoir = classical Yang-Mills on lattice
– Reservoir = (Schwarzschild) black hole
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Heat capacity of QGP reservoir
• MIT bag model:
𝐸 = 𝑉 𝜎𝑇4 + 𝐵 , 𝑝 =𝜎𝑇4
3− 𝐵, 𝑆 = 4𝜎𝑉𝑇3/3
𝐶 = 𝑑𝐸
𝑑𝑇 = 4𝜎𝑉𝑇3 + 𝜎𝑇4 + 𝐵
𝑑𝑉
𝑑𝑇
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Heat capacity of QGP reservoir • MIT bag model:
𝐸 = 𝑉 𝜎𝑇4 + 𝐵 , 𝑝 =𝜎𝑇4
3− 𝐵, 𝑆 = 4𝜎𝑉𝑇3/3
𝐶𝑉 = 4𝜎𝑉𝑇3 = 3𝑆, 𝐶𝑝 = ∞, 𝐶𝑆 =
3 4𝑆 1−
𝑇4
𝑇04
𝑇𝑓𝑖𝑡 = 𝑇 lim𝐶→∞
𝑒−𝑆/𝐶 = 𝑒−1/3 ≈ 0.7
V const.
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Heat capacity of QGP reservoir
• Chaotic classical Yang-Mills: 𝑆 𝐸 = 𝐶0 ln 1 + 𝐸/𝐶0𝑇0 , constant heat capacity C !
𝑇𝑓𝑖𝑡 = 𝑇
• Schwarzschild black hole: 𝑆 = 𝛼𝐸2,
1
𝑇= 2𝛼𝐸, 𝐶 = −2𝛼𝐸2 = −2 𝑆
𝑇𝑓𝑖𝑡 = 𝑇 lim𝐶→∞
𝑒−𝑆/𝐶 = 𝑒1/2 ≈ 1.65
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Black hole or a QGP bag?
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Fitted slopes
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Reservoir models
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Conclusion • Improved Canonical Approach: assumes statistical entanglement by
using optimal L(S) agreeing to higher order with microcanonical
• Universally treats finite heat capacity reservoirs (but includes the infinite ones)
• Tsallis entropy is L(S), Rényi entropy is S
• Fitted Boltzmann-Gibbs temperature may differ from that of the reservoir
• For QGP T = 175 MeV V=const fit T = 125 MeV, S=const QGP smaller, Yang-Mills fit T same, mini BH fit T = 288 MeV
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LECTURE SIX ABOUT
(ADVANCED) STATISTICAL
PHYSICS
T.S.Biró, MTA Wigner Research Centre for Physics, Budapest
Lectures given at: University of Johannesburg, South-Africa,
November 29, 2012.
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Thermalization
Pre-thermalization
Pseudo-thermalization
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Arxiv: 1111.4817 Phys.Lett. B 708:276, 2012
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Why Photons (gammas) ?
• Zero mass: flow – Doppler, easy kinematics
• Color neutral: escapes strong interaction
• Couples to charge: Z / A sensitive
• Classical field theory also predicts spectra
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𝑨𝒖 + 𝑨𝒖 → 𝜸 + 𝑿
Experimental motivation: apparently thermal photons
RHIC: PHENIX
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Theoretical motivation
• Deceleration due to stopping
• Schwinger formula + Newton + Unruh = Boltzmann
T/m
3p
T
q/m2
3p
T
2T
epd
dNE
2
aT,amq,e
pd
dNE
Satz, Kharzeev, …
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Soft bremsstrahlung
𝑢 • Jackson formula for the amplitude:
𝐴 = 𝐾 𝑒𝑖𝜙 𝑑
𝑑𝑡
𝑛 × 𝑛 × 𝛽
1 − 𝑛 ∙ 𝛽 dt
With 𝐾2 =𝑒2
8𝜋𝑐2, 𝛽 =
𝑣
𝑐=1
𝑐
𝑑𝑟
𝑑𝑡
and the retarded phase 𝜙 = 𝜔 𝑡 −𝑛∙𝑟
𝑐= 𝑘 ∙ 𝑥
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• Covariant notation: 𝑘 = 𝜔,𝜔𝑛 = 𝑘⊥ cosh 𝜂, sinh 𝜂, cos𝜓, sin𝜓
𝑢 = 𝛾, 𝛾𝑣 = cosh 𝜉 , sinh 𝜉 , 0,0
ℵ = 𝑒𝑖𝜑 𝑑
𝑑𝜏
𝜖 ∙ 𝑢
𝑘 ∙ 𝑢 𝑑𝜏
Soft bremsstrahlung
Feynman graphs IR div, coherent effects
The Unruh effect cannot be calculated by any finite number of Feynman graphs!
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Kinematics, source trajectory
• Rapidity: 𝛽 =𝑣
𝑐= tanh(𝜉 + 𝜉0)
𝜉 =𝑔
𝑐 𝜏
Trajectory:
𝑡 = 𝑡0 +𝑐
𝑔sinh(𝜉 + 𝜉0) − sinh 𝜉0
𝑧 = 𝑧0 +𝑐2
𝑔cosh(𝜉 + 𝜉0) − cosh 𝜉0
Let us denote 𝝃 + 𝝃𝟎 by 𝝃 in the followings!
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Kinematics, photon rapidity • Angle and rapidity:
cos 𝜃 = tanh 𝜂
sin 𝜃 =1
cosh 𝜂
cot 𝜃 = sinh 𝜂
𝜼 = 𝐥𝐧 𝐜𝐨𝐭𝜽
𝟐
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Kinematics, photon rapidity
• Doppler factor:
k ∙ u = ω𝛾 1 − 𝛽 cos 𝜃 = 𝜔cosh(𝜉−𝜂)
cosh 𝜂 =
𝑑𝜙
𝑑𝜏
Phase:
𝜙 =𝜔𝑐
𝑔
sinh(𝜉−𝜂)
cosh 𝜂= ℓ𝑘⊥ sinh(𝜉 − 𝜂)
Magnitude of projected velocity:
𝑢 =sinh 𝜉
cosh(𝜉−𝜂),
𝑑𝑢
𝑑𝜉=
cosh 𝜂
cosh2(𝜉−𝜂)
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Intensity, photon number Amplitude as an integral over rapidities on the trajectory:
𝐴 = 𝐾𝑒 𝑒𝑖ℓ𝑘⊥ sinh(𝜉−𝜂) cosh 𝜂
cosh2(𝜉−𝜂)𝑑𝜉
𝜉2𝜉1
Here ℓ =𝑐2
𝑔 is a characteristic length.
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Intensity, photon number Amplitude as an integral over infinite rapidities on the trajectory (velocity goes from –c to +c):
𝐴 = 2𝐾𝑒 ℓ𝑘⊥ cosh 𝐾1(ℓ𝑘⊥)
With K1 Bessel function!
𝑑𝑁
𝑘⊥𝑑𝑘⊥𝑑𝜂 𝑑𝜓=4𝛼𝐸𝑀
𝜋 ℓ2 𝐾 (ℓ𝑘⊥)1
2
Flat in rapidity !
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Photon spectrum, limits Amplitude as an integral over infinite rapidities on the trajectory (velocity goes from –c to +c):
𝑑𝑁
𝑘⊥𝑑𝑘⊥𝑑𝜂𝑑𝜓 =4𝛼𝐸𝑀
𝜋 1
𝑘⊥2 for ℓ𝑘⊥ → 0
𝑑𝑁
𝑘⊥𝑑𝑘⊥𝑑𝜂 𝑑𝜓= 2𝛼𝐸𝑀
ℓ
𝑘⊥ 𝑒−2ℓ𝑘⊥ for ℓ𝑘⊥ → ∞
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Apparent temperature
• High - 𝑘⊥ infinite proper time acceleration:
𝑘𝐵 𝑇 =ℏ𝑐
2ℓ=ℏ𝑔
2𝑐= 𝜋 𝑘𝐵 𝑇
𝑈𝑛𝑟𝑢
Connection to Unruh:
𝑑𝑢
𝑑𝜏 → 𝑒−𝑖𝜈𝜏 proper time Fourier analysis of a
monochromatic wave
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Unruh temperature
• Entirely classical effect
• Special Relativity suffices
Unruh
Max Planck
1
1)(
)(
/2
2
0
1//
2
/)(1
/)(1
gc
gcigzic
dcV
cVi
edzzeI
deI
Constant ‚g’ acceleration in a comoving system: dv/d = -g(1-v²) 39
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Unruh temperature
22
2
g
c2
PPB
B
LgM
g
cTk
gT
Tk
Planck-interpretation:
The temperature in Planck units:
The temperature more commonly:
40
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Unruh temperature
2
2
P
2
B
2
R
L
2
McTk
R
GMg
gravity Newtonianfor Small
On Earth’ surface it is 10^(-19) eV, while at room temperature about 10^(-3) eV.
41
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Unruh temperature
2
mcTk
mc
L2
cg
collisions ionheavy in smallNot
2
B
32
Braking from +c to -c in a Compton wavelength:
kT ~ 150 MeV if mc² ~ 940 MeV (proton) 42
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Connection to Unruh
𝑑𝑁
𝑘⊥𝑑𝑘⊥𝑑𝜂 𝑑𝜓=
𝛼𝐸𝑀
2𝜋𝑘⊥2 cosh2 𝜂
𝑒𝑖𝜙(𝜏) 𝑑𝑢
𝑑𝜏 𝑑𝜏
+∞
−∞
2
𝑓𝑘 = 𝑒𝑖𝜙(𝜏) 𝑒𝑖𝜈𝜏𝑑𝜏
+∞
−∞
= ℓ
𝑐 𝑒𝑖ℓ𝑘⊥ sinh 𝜉 𝑒𝑖𝑘𝜉𝑑𝜉
+∞
−∞
Fourier component for the retarded phase:
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Connection to Unruh
𝑑𝑁
𝑘⊥𝑑𝑘⊥𝑑𝜂 𝑑𝜓
𝛼𝐸𝑀
2𝜋𝑘⊥2 cosh2 𝜂
𝑓𝑘2 𝑎𝑘
2 𝑐
ℓ 𝑑𝑘
2𝜋
+∞
−∞
𝑎𝑘 = 𝑑𝑢
𝑑𝜏𝑒𝑖𝜈𝜏
+∞
−∞
𝑑𝜏 = cosh 𝜂 1
cosh2 𝜉 𝑒𝑖𝑘𝜉𝑑𝜉
+∞
−∞
Fourier component for the projected acceleration:
Photon spectrum in the incoherent approximation:
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Connection to Unruh
𝑓𝑘 =ℓ
𝑐 𝑒𝑖ℓ𝑘⊥ sinh 𝜉 𝑒𝑖𝑘𝜉𝑑𝜉+∞
−∞=2ℓ
𝑐 𝐾𝑖𝑘 ℓ𝑘⊥ 𝑒
−𝜋𝑘/2
Fourier component for the retarded phase at constant acceleration:
KMS relation and Planck distribution:
𝑓−𝑘 = 𝑒𝑘𝜋 𝑓𝑘
∗, 𝑓−𝑘2 = 𝑒2𝜋𝑘 𝑓𝑘
2
−n −ν = 𝑒2𝜋ℓ𝜈 𝑐 𝑛 𝜈 = 1 + 𝑛 𝜈
𝑛 𝜈 = 1
𝑒2𝜋ℓ𝜈 𝑐 − 1
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Connection to Unruh
KMS relation and Planck distribution:
2π𝑘 =2𝜋𝑐
𝑔 𝜈 =
ℏ
𝑘𝐵𝑇𝑈 𝜈 ;
𝑇𝑈 = ℏ
2𝜋𝑘𝐵𝑐 𝑔
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Connection to Unruh
Note:
𝑎𝑘 = cosh 𝜂 𝑘𝜋
sinh 𝑘𝜋 2
It is peaked around k = 0, but relatively wide! (an unparticle…)
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Intensity, photon number Amplitude as an integral over infinite rapidities on the trajectory (velocity goes from –c to +c):
𝐴 = 2𝐾𝑒 ℓ𝑘⊥ cosh 𝐾1(ℓ𝑘⊥)
With K1 Bessel function!
𝑑𝑁
𝑘⊥𝑑𝑘⊥𝑑𝜂 𝑑𝜓=4𝛼𝐸𝑀
𝜋 ℓ2 𝐾 (ℓ𝑘⊥)1
2
Flat in rapidity !
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Transverse flow interpretation
Mathematica knows: ( I derived it using Feynman variables)
Alike Jüttner distributions integrated over the flow rapidity…
𝑑𝜃
sin 𝜃 𝐾2
𝑧
sin 𝜃 = 𝐾1
2𝑧
2
𝜋
0
1
sin 𝜃= cosh 𝜂
𝑑𝑁
𝑘⊥𝑑𝑘⊥𝑑𝜂 𝑑𝜓=
4𝛼𝐸𝑀 ℏ𝑐
𝜋 2𝜋𝑘𝐵𝑇𝑈2 𝐾2
ℏ𝑐 𝑘⊥
𝜋𝑘𝐵𝑇𝑈 cosh(𝜁 − 𝜂) 𝑑𝜁
+∞
−∞
𝒅𝑵
𝒌⊥𝒅𝒌⊥𝒅𝜼 𝒅𝝍=
𝟒𝜶𝑬𝑴
𝝅 𝒈 𝑲𝟐
𝒌∙𝒖𝑩𝒋𝒐𝒓𝒌𝒆𝒏
𝝅𝑻𝑼𝒏𝒓𝒖𝒉 𝒅𝜻
+∞
−∞
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Finite time (rapidity) effects
𝑑𝑁
𝑘⊥𝑑𝑘⊥𝑑𝜂 𝑑𝜓 =
4𝐾2
ℏ 𝑘⊥2
𝑒𝑖ℓ𝑘⊥𝑤
(1+𝑤2)3/2𝑤2𝑤1
2
with 𝑤 = sinh(𝜉 − 𝜂)
Short-time deceleration Non-uniform rapidity distribution; Landau hydrodynamics
Long-time deceleration uniform rapidity distribution; Bjorken hydrodynamics
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Short time constant acceleration
𝑑𝑁
𝑘⊥𝑑𝑘⊥𝑑𝜂 𝑑𝜓=
4𝛼𝐸𝑀
𝜋 1
𝑘⊥2 (𝑤2−𝑤1)
2
(1+𝑤02)3
𝑑𝑁
𝑘⊥𝑑𝑘⊥𝑑𝜂 𝑑𝜓= 4𝛼𝐸𝑀𝜋 4
𝜔2 1
cosh2 𝜂
Non-uniform rapidity distribution; Landau hydrodynamics
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Further analytic results x(t), v(t), g(t), τ(t), 𝒜, dN/kdkd limit
1 + 𝑡2 , 𝑡
1+𝑡2 , 1, Arc sh 𝑡 , 𝑏𝐾1 𝑏 ,
ℓ
𝑘𝑒−2ℓ𝑘
1 + ln (1 + 𝑡2), 2𝑡
1+𝑡2, 2 1+𝑡2
1−𝑡2 2, 2 atn 𝑡 − 𝑡, 𝑏𝑒−𝑏 , ℓ2𝑒−2ℓ𝑘
1 + 2𝑡
𝜋atn
𝑡
𝜋− ln 1 +
𝑡2
𝜋2,2
𝜋atn
𝑡
𝜋,
2𝛾3
𝜋2+𝑡2,𝜋2
2
1−𝑣2 𝑑𝑣
cos2𝜋𝑣
2
, 𝑒−𝑏,1
𝑘2𝑒−2ℓ𝑘
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𝑨𝒖 + 𝑨𝒖 → 𝜸 + 𝑿
Glauber model
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𝑨𝒖 + 𝑨𝒖 → 𝜸 + 𝑿
Glauber model
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Summary
• Semiclassical radiation from constant accelerating point charge occurs rapidity-flat and thermal
• The thermal tail develops at high enough k_perp
• At low k_perp the conformal NLO result emerges
• Finite time/rapidity acceleration leads to peaked rapidity distribution, alike Landau - hydro
• Exponential fits to surplus over NLO pQCD results reveal a ’’pi-times Unruh-’’ temperature
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