tev particle physics and physics beyond the standard model · i.a., g.burdman, z.chacko - prl 92 -...
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TeV Particle Physics and PhysicsBeyond the Standard Model
Ivone Albuquerque, Alex Kusenko, Tom Weiler
TeV Particle Astrophysics
Madison, 28-31 Aug, 2006
TeV Particle Physics and Physics Beyond the Standard Model – p.1/29
Working Group Discussion
Probing Physics Beyond the SM with
∼> TeV νs, γs, Cosmic Rays
particle and astro experiments can becomplementary
together can better constrain models
SUSY: NLSP detection in neutrino telescopes
Dark Side:
DM, Black Holes
squishing DM with Black Holes
TeV Particle Physics and Physics Beyond the Standard Model – p.2/29
Looking for SUSY in the Ice
SUSY Breaking mechanism ⇒ mass spectrum ⇒ LSP
LSP is determined by the scale of SUSY breaking (√
F )
103 GeV <√
F < 1012 GeV
√F > 1010 GeV ⇒ LSP is neutralino
√F < 1010 GeV ⇒ LSP is gravitinoin most of these cases: NLSP is charged slepton(typically the τR with m = ϑ(150 GeV)
for√
F ∼> 106 GeV and HE collisions, NLSPs travellong distances before decaying
I.A., G.Burdman, Z.Chacko - PRL 92 - 04
TeV Particle Physics and Physics Beyond the Standard Model – p.3/29
SUSY Cross Section
10-36
10-35
10-34
10-33
10-32
10-31
105
106
107
108
109
1010
1011
E (GeV)
σ (cm
2 )
———– SM σ .- - - - - - SUSY σ (m(q) = 300) GeV———– SUSY σ (m(q) = 600) GeV− · − · − SUSY σ (m(q) = 900) GeV
I.A., G.Burdman, Z.Chacko - PRL 92 - 04
TeV Particle Physics and Physics Beyond the Standard Model – p.4/29
Long Range Compensates Small XS
M. Ahlers
TeV Particle Physics and Physics Beyond the Standard Model – p.5/29
Rate of Charged NLSPs in Neutrino Telescopes
10-2
10-1
1
10
10 2
10 3
10 4
10 5
10 6
106
107
108
109
1010
1011
Eν (GeV)
Eν d
Nl/d
Eν (k
m-2
yea
r-1)
Eν (GeV)
Eν d
Nl/d
Eν (k
m-2
yea
r-1)
I.A., G.Burdman, Z.Chacko
TeV Particle Physics and Physics Beyond the Standard Model – p.6/29
Flux of Staus and Muons
øStaus at the detector may dominate over muons aboveE ∼ 105 GeV, but with different energy loss properties!
Markus Ahlers (DESY Hamburg) Long-lived Staus at Neutrino Telescopes Madison, August 28-31, 2006
TeV Particle Physics and Physics Beyond the Standard Model – p.7/29
diµ mq = 300 GeV 600 GeV 900 GeVWB 15 17 2 0.5MPR 29 85 7 2
Table 1: Number of events per km2 per year assuming the WB and MPR limits. Thefirst column refers to upgoing di-muons. The last three columns correspond to upgoing NLSPpair events, for three different choices of squark masses: 300 GeV, 600 GeV and 900 GeV.
Z. Chacko
TeV Particle Physics and Physics Beyond the Standard Model – p.8/29
Stau Signature: 2 Tracks
00.05
0.10.15
0.20.25
0.30.35
0.40.45
0.5
0 200 400 600 800 1000track separation (m)
dist
ribu
tion
stau (300)
0
0.1
0.20.3
0.4
0.50.6
0 20 40 60 80 100 120 140 160 180 200track separation (m)
dist
ribu
tion
µ+µ-
I.A., G.Burdman,Z.Chacko
TeV Particle Physics and Physics Beyond the Standard Model – p.9/29
Observable Parallel Tracks
Rate of stau pairs for the Waxman-Bahcall flux at IceCube:
min m: N ∼ 5 per year SPS 7: N ∼ 1 per decade
Markus Ahlers (DESY Hamburg) Long-lived Staus at Neutrino Telescopes Madison, August 28-31, 2006
TeV Particle Physics and Physics Beyond the Standard Model – p.10/29
Km3 neutrino telescopes have the potential to discoverthe charged NLSP
Background (di-µ) is small and 2 track NLSP signatureis clear
Observation of the NLSP constitutes a direct probe ofthe scale of SUSY breaking
Complementary search to LHC
TeV Particle Physics and Physics Beyond the Standard Model – p.11/29
Stau Energy Loss
Energy Loss - Range
• Electromagnetic energy loss:ionization
bremsstrahlung
pair productionphotonuclear
• Weak interactions: neutral current
charged currentdecay
dE/dX = -(α + β E)
βNC
removes particles
M.H.Reno
TeV Particle Physics and Physics Beyond the Standard Model – p.12/29
Stau Radiative Energy Loss
M.H.Reno
TeV Particle Physics and Physics Beyond the Standard Model – p.13/29
Stau Weak Interactions
M.H.Reno
TeV Particle Physics and Physics Beyond the Standard Model – p.14/29
Determining SUSY parameters using DArk Matter
D. Hooper
TeV Particle Physics and Physics Beyond the Standard Model – p.15/29
1e-14
1e-12
1e-10
1e-08
1e-06
1e-04
1e-14 1e-12 1e-10 1e-08 1e-06
σ χN (p
b)
tan2β|N11|2N13|2/mA4
Direct Detection:
Models with large XS ⇒ dominated by Higgs exchange, couplings to b and squarks
Squark exchange contribution is only substantial below 108 pb
Leads to correlation between neutralino composition, tan β, mA and elasticscattering rate.
D. Hooper
TeV Particle Physics and Physics Beyond the Standard Model – p.16/29
UHE ν and Physics Beyond SM
I. Sarcevic
TeV Particle Physics and Physics Beyond the Standard Model – p.17/29
Detection of Cosmic Neutrinos
• Muon tracks (ICECUBE, RICE)
• Electromagnetic and Hadronic Showers (ICECUBE, RICE,
ANITA, Auger, OWL, EUSO)
• To determine the energy flux (muons or showers) that reaches
the detector we need to consider propagation of neutrinos and
leptons through the Earth and ice
• ντ give different contribution from νµ due to the very short τ
lifetime, i.e. the regeneration effect.
• New physics may be manifested via production of new particles
in neutrino interactions, such as supersymmetric charged
sleptons, staus, which after interactions with matter produce
charge tracks similar to muons, or hardonic showers.
I.Sarcevic
TeV Particle Physics and Physics Beyond the Standard Model – p.18/29
Probing the Physics Beyond the Standard Model with EUSO
1010
1011
1012
Esh [GeV]
1010
1011
1012
1013
1014
1015
1016
1017
1018
1019
E sh *
dNsh
/dE sh
[GeV
yr-1
]
Black : Standard Model
Red : Electroweak Instantons
Blue : Microscopic Black Holes
Green : TeV-scale String Excitations
Black : Standard Model
Red : Electroweak Instantons
Blue : Microscopic Black Holes
Green : TeV-scale String Excitations
I. Sarcevic
TeV Particle Physics and Physics Beyond the Standard Model – p.19/29
Bounds on DM annihilation XS
J. Beacom
TeV Particle Physics and Physics Beyond the Standard Model – p.20/29
J. Beacom
TeV Particle Physics and Physics Beyond the Standard Model – p.21/29
J. Beacom
TeV Particle Physics and Physics Beyond the Standard Model – p.22/29
TeV Particle Physics and Physics Beyond the Standard Model – p.23/29
TeV Particle Physics and Physics Beyond the Standard Model – p.24/29
TeV Particle Physics and Physics Beyond the Standard Model – p.25/29
TeV Particle Physics and Physics Beyond the Standard Model – p.26/29
TeV Particle Physics and Physics Beyond the Standard Model – p.27/29
TeV Particle Physics and Physics Beyond the Standard Model – p.28/29
A New Method
• Based on a Very Simple Idea
• Look for the Higgs FIELD instead of the Higgs PARTICLE
• PROBLEM: Higgs is very massive ⇒ very short rangeHiggs field
• A Particle very close to the Source of a Higgs Field willexperience a Mass Adjustment
• Look at the Effect of Pairs of Massive Particles near PairThreshold
Reucroft
TeV Particle Physics and Physics Beyond the Standard Model – p.29/29
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