Transcript MATERIA OSCURA Y EL SECTOR DE HIGGS Primer Avance

PHENOMENOLOGY OF SCALAR
DARK MATTER CANDIDATES
Lilian Prado González
Director: Dr. J. Lorenzo Díaz Cruz
Co-Director: Dr. Jose A.R. Cembranos
12 October 2011
Phenomenology of Scalar DM
candidates
The Universe and the Dark Matter
• Cosmological Standard Model
• Relic Density
Scalar Candidates:
• Inert Higgs Doublet Model
• Branons
Dark Matter Search
• Direct
• Colliders
• Indirect
Conclusions
Phenomenology of Scalar DM candidates
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Phenomenology of Scalar DM candidates
3
Expansion: Hubble Parameter
v  Hd
H t  
a t 
at 
H0  H t0   h 100km1Mpc1
Friedmann equation
8G
k
a

H2   
 2
3
a
a
2
Phenomenology of Scalar DM candidates
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Dark Matter (DM): WIMPs
Rotation
Curves of
Spiral
Galaxies
Gravitational
Lensing
Phenomenology of Scalar DM candidates
CMBR
8
Big-Bang Thermal Relics
Early Universe: Relativistic Particles
Thermal Equilibrium in regions (e+e-  gg)
Cosmic Expansion Rate H (a, t, T)
For Weak Interacting Particles: Particle Interaction < Expansion Rate
Decoupling: n, g, c
Phenomenology of Scalar DM candidates
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Boltzmann Equation
Gondolo & Gelmini
Describes the evolution of the phase space density f(p,x,t)
of a particle species.
L[f] = C[f]
Collision operator C:
Liouville operator L:
Changing rate of f in t
Number of particles per unit
of volume of phase
space/collision time with
other particles
Phenomenology of Scalar DM candidates
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Boltzmann Equation
• With RW metric:
2
p f
f
L( f ) 
H
t
E E
H = Hubble parameter
(
R = Universe scale factor
R
H 
R
Phenomenology of Scalar DM candidates
)
11
For standard RW
• Hubble parameter
1/ 2
8

H   G 
3

• Total Energy Density of the Universe
• Entropy Density
  g eff (T )
2
30
T4
2 2 3
s  heff (T )
T
45
heff = Effective Degrees of Freedom for s
geff = Effective Degrees of Freedom for E
Phenomenology of Scalar DM candidates
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Conditions
1. Identical particles
2. Negligible Chemical Potential
m = Energy change of an homogeneous mass/Quantity of substance added to the system
3. Density decrese due to the Universe expansion
Y = n/s
Phenomenology of Scalar DM candidates
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Density Y(x)
x = m/T
• T= Photons temperature (Thermal Bath)
• Universe content is introduced as:
s (in Y(s))
Phenomenology of Scalar DM candidates
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Boltzmann Equation
1/ 2
 M 
dY

 
dx
 45 
2
P
heff m
1/ 2 2
g eff
x
v (Y 2  Yeq 2 )
Where:
 = Total annihilation cross-section
v = velocity invariant under Lorentz
transformations
Phenomenology of Scalar DM candidates
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Relic Density
Decoupling
Temperature
Energy fraction of
Species X
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Two Higgs Doublet Model
(THDM)
• One of the simplest extensions to Electroweak Symmetry Breaking
Higgs Mechanism, beyond SM
• Two Higgs fields doublets are introduced
Ta  a , a  ica 
a = 1, 2
They interact between themselves and SM particles through the
right potential
• Presents New Physics:
– Flavor Changing Neutral Currents, (FCNC)
– CP violation
Phenomenology of Scalar DM candidates
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IHDM (Model I)
•
•
Only one doublet interacts with matter fields.
Yukawa couplings:
~ u  Y ( d ) q  d  h.c.  leptons
LY  Yij(u ) q Li 
1 Rj
ij
1 Rj
Li
•
Potential:

V  m  1  m   2  1  1
2
1


†
1
†
2
2
2


 3  1   2  4   2
•
•
•
†
1
†
2
†
1

†
1


2

 2   2

1
 1  5 1† 2
2
†
2
†
2

2
     
2
†
2
2
1
1†2
An additional Z2 symmetry is introduced to avoid mixing terms
1 has a vacuum expectation value (VEV) v/2 = 174 GeV as in SM
 has no VEV.
2
Phenomenology of Scalar DM candidates
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IHDM (Model I)
Physical fields for Higgs sector:
• Two scalar charged Higgs bosons : H±
• Two neutral scalar Higgs bosons: H0, h0
• One neutral pseudo-scalar Higgs boson:
A0
 H 

H 2  

H

iA
0
 0

H  H
†
2
Phenomenology of Scalar DM candidates

H 0  iA0
21

IHDM as DM candidate
Phenomenology of Scalar DM candidates
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IHDM Relic Abundance
According to WMAP:
DM h  0.112 0.0056
2
Obtained relic Abundance for IHDM:
IHDM h2  106
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IHDM Relic Abundance
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IHDM Relic Density
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Reported IHDM
Phys. Rev. D 80, 055012 (2009)

Co-annihilations are important to be considered
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Brane Worlds
Extra Dimensions
• Theoretical origin
• KK Theories, SUSY, SUGRA, Superstrings, M-Theory
Brane Worlds (BW)
• New scenarios to solve hierarchy problem
• ADD, RS
• SM matter confined in a tridimensional
hypersurface: Brane
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Brane Worlds
Our Universe is embedded in a higher D dimensional Space
D=4+d
d = extra diemsions compactified
SM particles confined to the 3-brane but gravitons can propagate along
the whole bulk space.
MF = Fundamental gravitational scale in D dimensions
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Branons
Brane = New dynamical object (Rigid objects do not exist in relativistic
theories)
Branons = Brane fluctuations: New fields which represent the position
of the brane in the bulk space
Pseudo-Goldstone bosons corresponding to spontaneous symmetry
breaking of the translational invariance produced by the presence of
the brane.
f = Brane tension scale
F<<MF: The KK modes decouple from the SM particles on the brane
Phenomenology of Scalar DM candidates
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Branons
• For flexible branes (f<<MF), the only relevant
degrees of freedom at low energies are SM
particles and branons.
f
M
N
Parameters
Phenomenology of Scalar DM candidates
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Branons
Phenomenology of Scalar DM candidates
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DM Detection Experiments
• Direct:
Observe elastic scattering of
DM particles with nuclei
• Colliders:
Production of WIMPS,
detection of missing
energies (LHC)
• Indirect:
Detect DM annihilation
productions such as protons,
neutrinos, etc.
Phenomenology of Scalar DM candidates
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Direct Detection
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Event Rate for WIMP Direct Detection
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Branons Direct Search
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Collider Search
• Production of WIMPS
• Detection of missing energies
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Branons Collider Search
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Branons Collider Search
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Branons Collider Search
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DM Indirect Detection Experiments
Detect DM
annihilation
products such as:
• Protons
• Electrons
• Neutrinos
• Gamma rays
Phenomenology of Scalar DM candidates
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Conclusions
DM is a cornerstone of our current knowledge of the
Universe
IHDM is a DM viable candidate only in co-anihilations
are considered
Branons are viable DM candidates and their search in
colliders (LHC) is constrained with the current data
Direct and indirect DM search also give constrains on
these candidates.
Phenomenology of Scalar DM candidates
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