Lepton Flavor Violation and Supersymmetric Dirac Leptogenesis.pdf

Lepton Flavor Violation and Supersymmetric Dirac Leptogenesis.pdf

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Lepton Flavor Violation and Supersymmetric Dirac Leptogenesis

a r X i v : h e p - p h / 0 6 0 7 2 8 5 v 2 2 9 A u g 2 0 0 6 Lepton Flavor Violation and Supersymmetric Dirac Leptogenesis Brooks Thomas and Manuel Toharia Michigan Center for Theoretical Physics (MCTP) Department of Physics, University of Michigan, Ann Arbor, MI 48109 MCTP 06-17 July 25, 2006 Abstract Dirac leptogenesis (or Dirac neutrinogenesis), in which neutrinos are purely Dirac particles, is an interesting alternative to the standard leptogenesis scenario. In its supersymmetric version, the modified form of the superpotential required for successful baryogenesis contributes new, generically non-flavor-diagonal terms to the slepton and sneutrino mass matrices. In this work, we examine how current experimental bounds on flavor-changing effects in the lepton sector (and particularly the bound on μ → eγ) constrain Dirac leptogenesis and we find that it is capable of succeeding with superpartner masses as low as ~ 100 GeV. For such light scalars and electroweakinos, upcoming experiments such as MEG are generically expected to observe signals of lepton flavor violation. 1 Introduction When singlet fermions are not present in a given theory, Dirac leptogenesis [1, 2], or Dirac neutrinogenesis, represents a very interesting alternative to the traditional leptogenesis scenario, which relies on the existence of heavy Majorana neutrinos. In Dirac leptogenesis, neutrinos are purely Dirac particles whose small but nonzero masses appear as ratios of dimensionful parameters in an effective field theory. It has been shown [3] that, in the context of split supersymmetry [4, 5], Dirac leptogenesis is a phenomenologically viable scenario capable of satisfying all relevant constraints from cosmology and neutrino physics as well as reproducing the observed baryon-to- photon ratio η of the universe. Split supersymmetry is advantageous primarily for two reasons. The first of these is that very heavy gravitinos can easily evade the constraints that big bang nucleosynthesis (BBN

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