TeV Particle Physics and Physics Beyond the Standard Model

Transcription

1 TeV Particle Physics and Physics Beyond the Standard Model Ivone Albuquerque, Alex Kusenko, Tom Weiler TeV Particle Astrophysics Madison, Aug, 2006 TeV Particle Physics and Physics Beyond the Standard Model p.1/29

2 Working Group Discussion Probing Physics Beyond the SM with > TeV νs, γs, Cosmic Rays particle and astro experiments can be complementary 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

3 Looking for SUSY in the Ice SUSY Breaking mechanism mass spectrum LSP LSP is determined by the scale of SUSY breaking ( F ) 10 3 GeV < F < GeV F > GeV LSP is neutralino F < GeV LSP is gravitino in most of these cases: NLSP is charged slepton (typically the τ R with m = ϑ(150 GeV) for F > 10 6 GeV and HE collisions, NLSPs travel long distances before decaying I.A., G.Burdman, Z.Chacko - PRL TeV Particle Physics and Physics Beyond the Standard Model p.3/29

4 SUSY Cross Section σ (cm 2 ) E (GeV) 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 TeV Particle Physics and Physics Beyond the Standard Model p.4/29

5 Long Range Compensates Small XS M. Ahlers TeV Particle Physics and Physics Beyond the Standard Model p.5/29

6 Rate of Charged NLSPs in Neutrino Telescopes E ν dn l /de ν (km -2 year -1 ) E ν (GeV) I.A., G.Burdman, Z.Chacko TeV Particle Physics and Physics Beyond the Standard Model p.6/29

7 ux of Staus and Muons Staus at the detector may dominate over muons above E 10 5 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

8 diµ m q = 300 GeV 600 GeV 900 GeV WB MPR Table 1: Number of events per km 2 per year assuming the WB and MPR limits. The first column refers to upgoing di-muons. The last three columns correspond to upgoing NLSP pair 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

9 Stau Signature: 2 Tracks distribution distribution stau (300) track separation (m) µ + µ track separation (m) I.A., G.Burdman,Z.Chacko TeV Particle Physics and Physics Beyond the Standard Model p.9/29

10 servable Parallel Tracks Rate of stau pairs for the Waxman-Bahcall flux at IceCube: min m: Ṅ 5 per year SPS 7: Ṅ 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

11 Km 3 neutrino telescopes have the potential to discover the charged NLSP Background (di-µ) is small and 2 track NLSP signature is clear Observation of the NLSP constitutes a direct probe of the scale of SUSY breaking Complementary search to LHC TeV Particle Physics and Physics Beyond the Standard Model p.11/29

12 Stau Energy Loss Energy Loss - Range Electromagnetic energy loss: ionization bremsstrahlung pair production photonuclear de/dx = -(α + β E) Weak interactions: neutral current charged current decay β NC removes particles M.H.Reno TeV Particle Physics and Physics Beyond the Standard Model p.12/29

13 Stau Radiative Energy Loss TeV Particle Physics and Physics Beyond the Standard Model p.13/29

14 Stau Weak Interactions M.H.Reno TeV Particle Physics and Physics Beyond the Standard Model p.14/29

15 Determining SUSY parameters using DArk Matter D. Hooper TeV Particle Physics and Physics Beyond the Standard Model p.15/29

16 1e-04 1e-06 Direct Detection: σ χn (pb) 1e-08 1e-10 1e-12 1e-14 1e-14 1e-12 1e-10 1e-08 1e-06 tan 2 β N 11 2 N 13 2 /m A 4 Models with large XS dominated by Higgs exchange, couplings to b and s quarks Squark exchange contribution is only substantial below 10 8 pb Leads to correlation between neutralino composition, tan β, m A and elastic scattering rate. TeV Particle Physics and Physics Beyond the Standard Model p.16/29

17 UHE ν and Physics Beyond SM I. Sarcevic TeV Particle Physics and Physics Beyond the Standard Model p.17/29

18 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 ν τ give different contribution from ν µ 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

19 Probing the Physics Beyond the Standard Model with EUSO E sh * dn sh /de sh [GeV yr -1 ] Black : Standard Model Red : Electroweak Instantons Blue : Microscopic Black Holes Green : TeV-scale String Excitations I. Sarcevic E sh [GeV] TeV Particle Physics and Physics Beyond the Standard Model p.19/29

20 Bounds on DM annihilation XS J. Beacom TeV Particle Physics and Physics Beyond the Standard Model p.20/29

21 J. Beacom TeV Particle Physics and Physics Beyond the Standard Model p.21/29

22 J. Beacom TeV Particle Physics and Physics Beyond the Standard Model p.22/29

23 TeV Particle Physics and Physics Beyond the Standard Model p.23/29

24 TeV Particle Physics and Physics Beyond the Standard Model p.24/29

25 TeV Particle Physics and Physics Beyond the Standard Model p.25/29

26 TeV Particle Physics and Physics Beyond the Standard Model p.26/29

27 TeV Particle Physics and Physics Beyond the Standard Model p.27/29

28 TeV Particle Physics and Physics Beyond the Standard Model p.28/29

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 range Higgs field A Particle very close to the Source of a Higgs Field will experience a Mass Adjustment Look at the Effect of Pairs of Massive Particles near Pair Threshold Reucroft TeV Particle Physics and Physics Beyond the Standard Model p.29/29