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“Sphalerons”
4-th Nikhef Mini Workshop
“Theory Meets Experiment”
Oct 12, 2016
Agenda
•
Introduction
– Context of this mini-workshop,
•
M.M. – 10’
Part I: Theory
– “What are Sphalerons?”
Bert Schellekens – 25’
– “Sphalerons in the Early Universe”
Marieke Postma – 25’
– “Sphaleron signatures in QCD”
Chris Korthalsaltes – 15’
– “Sphaleron signatures for B+L Violation”
Jan Smit – 15’
•
Break
•
Part II: Experiment
– Search for Sphalerons in (high energy) LHC
Ivo van Vulpen – 20’
– Sphalerons in Alice: “Chiral magnetic effect”
Jacopo Margutti – 20’
– Search for Sphalerons in cosmic ray showers
Charles Timmermans – 20’
•
Borrel
Physics of the Early Universe
Chiral Symmetry Breaking (mass)
EW Symmetry Breaking (mass)
Electroweak Baryogenesis in the Standard Model?
broken phase
symmetric phase
T > Tc
T  Tc
T  Tc
expanding bubble (Higgs condensates)
Three Sacharov Conditions:
✔ Baryon Number Violation
Adler-BellJackiw
✔ C and CP Violation
‘t Hooft, PRL
37 (1976) 8
✔ Thermal non-equilibrium
V
1st order
Axial Anomaly:
f
tunnel
f
f
Quantum anomaly
Weak Interaction
Higgs Phase Transition
f
Electroweak Baryogenesis in the Standard Model?
 Search for new particles or fields!
CPV from CKM:
− ACP = Jinv * (mt2-mc2) (mc2-mu2) (mu2-mt2)
* (mb2-ms2) (ms2-md2) (md2-mb2)
− BAU: ΔnB/nγ ≈ 10-10
 From CKM: ACP / Tc12 ≈ 10-20
 Used: Tc ~ 100 GeV !
 SM: MH < ~70 GeV
 THDM: MH ~ 125 OK
✔ Baryon Number Violation
Adler-BellJackiw
✔
✖ C and CP Violation
✔
✖ Thermal non-equilibrium
st nd
12
order
order
‘t Hooft, PRL
37 (1976) 8
V SM
Axial Anomaly:
f
tunnel
f
f
Quantum anomaly
Weak Interaction
Higgs Phase Transition
f
<j> == 00
<j>
Recipes for Baryogenesis - skip
<j> = 0
<j> = 0
Figure 1.
1. Expanding
Expanding bubbles
bubbles of
of the
the electroweak-broken
electroweak-broken phase
phase within
within the
the
Figure
<j> = in
0 the electroweak-symmetric phase.
surrounding plasma
plasma
surrounding
in
the electroweak-symmetric phase.
<j> = 0
<j> = 0
CP
CP
c
c
c LL ++ c RR
<j> = 0
c
c LL
Sphaleron
Sphaleron
Figure 1. Expanding
bubbles of the electroweak-broken
Sphaleron
Sphaleron phase within the
surrounding plasma
in the electroweak-symmetric
phase.
Expanding
bubbles
of broken phase
B
B
In a medium of symmetric
phase
c
c
<f> = 0
<f>
CP = 0
L
+
R
Bubble Wall
Bubble Wall
<f> = 0
<f> = 0
Baryon production in front
of bubble wall
Figure 2. Baryon production in front of the bubble walls.
Figure 2. Baryon production in front of the bubble walls.
cL
2. These asymmetries diffuse into the symmetric phase ahead of the bubble wall, where they
2. These asymmetries diffuse
into the symmetric phase ahead of the bubble wall, where they
Sphaleron
Sphaleron
bias electroweak sphaleron
transitions [15, 16] to produce more baryons than antibaryons.
bias electroweak sphaleron transitions [15, 16] to produce more baryons than antibaryons.
3. Some of the net baryon charge created outside the bubble wall is swept up by the expanding
B charge created outside the bubble wall is swept up by the expanding
3. Some of the net baryon
wall into the broken phase. In this phase, the rate of sphaleron transitions is strongly
wall into the broken phase. In this phase, the rate of sphaleron transitions is strongly
suppressed, and can be small enough to avoid washing out the baryons created in the first
<f> = 0suppressed, and can be
<f>
= 0 enough to avoid washing out the baryons created in the first
small
two steps.
Bubble
Wall
two steps.
We illustrate these three steps in figure 2.
Figure 2.We
Baryon
production
in front
bubble
illustrate
these three
stepsofinthe
figure
2. walls.
Note:
new
must
be
abundant
theSakharov conditions for baryon
These physics
EWBG steps
satisfy
explicitly the in
three
These EWBG steps satisfy explicitly the three Sakharov conditions for baryon
creation [17]. Firstly, departure from thermodynamic equilibrium is induced by the passage
thermal
plasma
atsymmetric
the
time
ofthrough
EWSB.
creation
[17]. Firstly,
departure
from
thermodynamic
equilibrium
is induced
by the passage
2. These asymmetries
the
phase
ahead
ofthe
thecosmological
bubble
wall, plasma.
where
they
of the diffuse
rapidlyinto
expanding
bubble walls
Secondly, violation of
of
the
rapidly
expanding
bubble
walls
through
the
cosmological
plasma.
Secondly,
violation of
bias electroweak
sphaleron
transitions
[15,the
16]
to produce
more
baryons
than
baryon
number
comes
from
rapid
sphaleron
transitions
in theantibaryons.
symmetric phase. And thirdly,
Therefore
the
particles
must
be
roughly
at
baryon
number
comes
from
the rapid
sphaleron
transitions
the
phase. And thirdly,
3. Some of the net
baryon
charge
created
outside
thescattering
bubble
wall
is swept are
upinby
thesymmetric
expanding
both
C- and
CP-violating
(CPV)
processes
needed
at the phase boundaries to
the
TeV
scale.
both
Cand
CP-violating
(CPV)
scattering
processes
are
needed
at
the
phase
boundaries to
wall into the create
brokenthe
phase.
In this
phase,
the rate ofthat
sphaleron
particle
number
asymmetries
bias thetransitions
sphaleronsistostrongly
create more baryons than
create
particle
number
asymmetries
the sphalerons
to the
create
suppressed, and
can the
be small
enough
to avoid
washingthat
out bias
the baryons
created in
firstmore baryons than
antibaryons.
Sphaleron Discussions Today
Anomaly:
Quantum anomaly
•
•
•
•
•
•
•
What are sphalerons?
How do we go from the quantum anomaly to the nonperturbative picture?
What are differences/similarities between SU2 and SU3
Which quantum number play the role of “winding number” SU2:B+L, SU3:Q5?
What determines the height of the sphaleron potential?
How do sphalerons affect physics in the early universe: Baryogenesis/Leptogenesis
Are B+L violating interactions possible: qq 3 l + 7 q +nW, n’Z, n’’H (also Khoze talk 2014)
• What would be the experimental signatures:
- B+L violating interactions in the LHC (sphaleron potential is ~ 9 TeV)
- Chiral magnetic effects in Alice
- B+L violating interactions in Auger: shower depth and more?
- Km3Net?
Enjoy the workshop…
https://indico.nikhef.nl/categoryDisplay.py?categId=19
Agenda
•
Introduction
– Context of this mini-workshop,
•
M.M. – 10’
Part I: Theory
– “What are Sphalerons?”
Bert Schellekens – 25’
– “Sphalerons in the Early Universe”
Marieke Postma – 25’
– “Sphaleron signatures in QCD”
Chris Korthalsaltes – 15’
– “Sphaleron signatures for B+L Violation”
Jan Smit – 15’
•
Break
•
Part II: Experiment
– Search for Sphalerons in (high energy) LHC
Ivo van Vulpen – 20’
– Sphalerons in Alice: “Chiral magnetic effect”
Jacopo Margutti – 20’
– Search for Sphalerons in cosmic ray showers
Charles Timmermans – 20’
•
Borrel