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Exploring Stau Propagation at High Energies for Neutrino Telescopes

Investigating the Stau radiative energy loss and discovery potential for neutrino telescopes probing new physics beyond the Standard Model. Studying Stau propagation energy loss mechanisms such as photonuclear, bremsstrahlung, and pair production. Analysis of Stau range determinants at different energy levels.

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Exploring Stau Propagation at High Energies for Neutrino Telescopes

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  1. Propagation of Supersymmetric Charged Slepton at High Energies Shufang Su • U. of Arizona M.H. Reno, I. Sarcevic and S. Su hep-ph/0503030

  2. Msl=250 GeV Mwino=250 GeV  earth   ~ ~     earth N ~ l ~ q ~ ~   Motivation - Neutrino telescopes have great potential to probe new physics beyond SM Gravitino LSP Stau NLSP Albuquerque, Chacko and Burdman (2003) Larger production rate smaller production rate  = 2.197£ 10-6 sec c=659 meter Larger effective detector volumn stau propagation

  3. stau energy loss - • Discovery potential for neutrino telescope depends on the stau lifetime and range • Crucial to determine the energy loss of the high energy stau as it traverse the earth stau propagation

  4. energy ionization energy loss Constant: =2 £ 10-3 cm2/g radiative energy loss m,  , more later … c = E / () stau energy loss - Average energy loss of a particle traversing distance X WhenE ¿, i.e. E ¿ 4 £ 105 GeV £ (msl/150 GeV) Stau range determined by ionization energy loss or lifetime c stau propagation

  5. radiative energy loss:  - • photonuclear • bremsstrahlung • pair production stau propagation

  6. muon Stau: mass dependence / 1/m radiative energy loss:  - Stau / 1/m2 stau propagation

  7. E ¿ m=250 GeV m=150 GeV E À E0=106 GeV stau range: X(E, E0) - m=250 GeV lifetime lifetime m=250 GeV m=150 GeV m=150 GeV E0=103 GeV stau propagation

  8. Xus / XABC Comparison - • InAlbuquerque, Chacko and Burdman (2003) • Rescale from: •  = 0.8 £ 10-6 cm2/g •  • stau=9.5 £ 10-9 (150 GeV/mstau) cm2/g • No energy dependence ? Improve the potential of neutrino telescopes for detecting metastable stau stau propagation

  9. Conclusion - • Stau radiative energy loss  is dominated by photo-nuclear and pair production • Photonuclear and pair: / 1/m • Bremsstrahlung: / 1/m2 • Low energy ( E ¿), stau range is determined by ionization energy loss or stau lifetime, X / E • High energy ( E À), stau range is determined by radiative energy loss, X / log (E) • Previous estimation (scale stau) underestimate stau range by about a factor of two stau propagation

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