TeV Particle Physics and PhysicsBeyond the Standard Model

Ivone Albuquerque, Alex Kusenko, Tom Weiler

TeV Particle Astrophysics

Madison, 28-31 Aug, 2006

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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

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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

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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

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Long Range Compensates Small XS

M. Ahlers

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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

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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

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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

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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

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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

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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

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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

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Stau Radiative Energy Loss

M.H.Reno

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Stau Weak Interactions

M.H.Reno

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Determining SUSY parameters using DArk Matter

D. Hooper

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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

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UHE ν and Physics Beyond SM

I. Sarcevic

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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

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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

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Bounds on DM annihilation XS

J. Beacom

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J. Beacom

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J. Beacom

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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

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