neutralino dark matter with cp violation sabine kraml, cern
DESCRIPTION
Neutralino Dark Matter with CP Violation Sabine Kraml, CERN. GDR matière noir, Montpellier, 13-14 Feb 2006 in collab. w. G. Bélanger, F. Boudjema, A. Pukhov & A. Semenov. Relic density of WIMPs. Early Universe dense and hot; WIMPs in thermal equilibrium - PowerPoint PPT PresentationTRANSCRIPT
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Neutralino Dark Matter with CP Violation
Sabine Kraml, CERN
GDR matière noir,
Montpellier, 13-14 Feb 2006
in collab. w. G. Bélanger, F. Boudjema, A. Pukhov & A. Semenov
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S. Kraml Neutralino dark matter with CP violation 2
Relic density of WIMPs
(1) Early Universe dense and hot; WIMPs in thermal equilibrium
(2) Universe expands and cools; WIMP density is reduced through pair annihilation; Boltzmann suppression: n~e-m/T
(3) Temperature and density too low for WIMP annihilation to keep up with expansion rate → freeze out
Final dark matter density: h2 ~ 1/<v>Thermally avaraged cross section of all annihilation channels
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S. Kraml Neutralino dark matter with CP violation 3
Neutralino LSP of the MSSM
The generic O(100) GeV neutralino LSP has a too large relic density → need specific mechanism(s) for efficient enough annihilation
0.094 < h2 < 0.129 puts strong bounds on the parameter space
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S. Kraml Neutralino dark matter with CP violation 4
mSUGRA parameter space
GUT-scale boundary conditions: m0, m1/2, A0
4 regions with good h2
bulk (const. by LEP mh limit)
co-annihilation (small M)
Higgs funnel (tan ~ 50)
focus point (higgsino scenario)
Analogous scenarii in the general MSSM
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S. Kraml Neutralino dark matter with CP violation 5
Neutralino system
Neutralino mass eigenstates
Gauginos
Higgsinos
→ LSP
Gaugino and higgsino mass terms can be complex
→ CP violation ←
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S. Kraml Neutralino dark matter with CP violation 6
CP violation
In the general MSSM, gaugino and higgsino mass parameters and trilinear couplings can be complex:
Sparticle production and decay rates strongly depend on CPV phases → expect similar influence on <v>
Caution: also the sparticle masses depend on phases
→ disentangle effects from kinematics and couplings
NB1: M2 can also be complex, but its phase can be rotated away.
NB2: CPV phases are strongly constrained by dipole moments;
we set =0 and assume very heavy 1st+2nd generation sfermions
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S. Kraml Neutralino dark matter with CP violation 7
CP violation: Higgs sector
Non-zero phases induce CP violation in the Higgs sector through loop effects → mixing of h,H,A:
Couplings to neutralinos: scalar and pseudoscalar parts
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S. Kraml Neutralino dark matter with CP violation 8
Previous studies of relic with CPV
... typically concentrate on some particular aspect;no complete, general analysis so far; no public tools
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S. Kraml Neutralino dark matter with CP violation 9
CPV with micrOMEGAs
We have implemented the general MSSM Lagrangian with CP-violating phases in CalcHEP/micrOMEGAs
Higgs and sparticle masses and mixing matrices are computed with CPsuperH
Fully automatical computation of the relic density;
all contributing channels automatically included!
Now performing general analysis of CPV-MSSM parameter space ....
micrOMEGAs: G. Bélanger et al., Comput. Phys. Commun. 149 (2002), hep-ph/0112278CPsuperH: J.S. Lee et al., Comput. Phys. Commun. 156 (2004), hep-ph/0307377
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S. Kraml Neutralino dark matter with CP violation 10
Scan over phases in M1- plane
Blue: WMAP-allowed range in the CP-conserving MSSMGreen: same for the CP-violating case (arbitrary phases of M1 and )
M1 ~
main channel is annihilation into WW
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S. Kraml Neutralino dark matter with CP violation 11
With increasing (M1), the LSP mass increases; annihilation into WW becomes
less efficient while coannihilation with charginos can set in. Hence h2 ↑ or ↓ ...
()=180°
()=0°
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Scan over phases in M1- plane
mH+ = 500 GeVHiggs funnel
We find the conventional Higgs funnels just above and below 2m=mHi.The allowed bands are again wider than in the CP-conserving case.
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A closer look to the Higgs funnel
M1 = 150, M2 = 300, At = 1200 GeV, tan = 5
masses of 3rd gen: 500 GeV, 1st+2nd gen: 10 TeV
>>M1 → bino-like LSP, m ~ 150 GeV
h2 < 0.129 needs annihilation through Higgs
Scenario 1: = 500 GeV → small mixing in Higgs sector Scenario 2: = 1 TeV → large mixing in Higgs sector
Higgs mixing ~ Im(At)
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Scenario 1, = 500 GeV
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Scenario1: dependence on phase of At
dm2 = mh2−2m
WMAP allowed region follows position of h2 pole, deviation only 4%
0.094 < h2 < 0.129
h2 < 0.094
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When arg(M1) increases, h2 drops This is because m increases and hence dm2 decreases
Scenario1: dependence on phase of M1
0.094 < h2 < 0.129
h2 < 0.094
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S. Kraml Neutralino dark matter with CP violation 17
Keeping LSP and Higgs masses fixed
gS,P(h2) gS,P(h3)
(M1)=0 (~0, -.06) (-.05, ~0)
(M1)=90° (.05, -.01) (-.002, .04)
Scalar/pseudos. parts of H copuling
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Scenario 2, large Higgs mixing
Smaller mass difference needed
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S. Kraml Neutralino dark matter with CP violation 19
Order-of-magnitude effects due to t
Green bands: 0.94 < h2 < 0.129
dmi = mhi - 2mLSP, i=2,3
h3 h3
h3
h2
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S. Kraml Neutralino dark matter with CP violation 20
h3
h3
h2
h2 and h3 interchange scalar-pseudoscalar character
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S. Kraml Neutralino dark matter with CP violation 21
h3
Not only position but also height of peak varies.
m = −1.5
m = +1.5 GeV
Even for fixed masses order-of-magnitude variation in h2!
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Conclusions
CP-violating phases in the MSSM can have sizeable effects for collider phenomenology as well as for the relic density of the LSP
Implemented the CPV-MSSM into micrOMEGAs found up to order-of-magnitude effects in h2
no generically new features (same channels as in CP-conserving case) but important changes in the couplings; need to disentangle kinematic effects
detailed analysis of Higgs funnel (Higgs CP mixing) general analysis of annihilation is on the way
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S. Kraml Neutralino dark matter with CP violation 23
Green bands: 0.094 < h2 < 0.129
Yellow region: h2 < 0.094
Phase dependences, scenario 1, = 500 GeV