Q-balls and the proton stability in supersymmetric theories

Abstract

Abelian non-topological solitons with Baryon and/or Lepton quantum numbers naturally appear in the spectrum of the minimal supersymmetric standard model. They arise as a consequence of the existence of flat directions in the potential lifted by nonrenormalizable operators and SUSY breaking. We examine the conditions that these operators should satisfy in order to ensure proton stability and present a realistic string model which fulfils these requirements. We further identify a generic U(1) breaking term in the scalar potential and discuss its effect of rendering Q-balls unstable.

Q-Stars in Anti de Sitter Spacetime

“…The energy density within the soliton is approximately constant and equal to m 4 (or φ 4 ). So, one can find that, in 3 + 1 dimensions: 19) and, consequently,r ∼ 1, simplifying considerably the numerical procedures. Inside the soliton both the metric and matter fields variate extremely slowly with respect to the radius.…”

Q-BALLS CONSTRUCTED OF SPINORS IN LAGRANGIANS WITH SU(2) SYMMETRY

“…The minimum of this quantity should be less than the particle mass, in order the soliton to be stable. Much more interest was concentrated on the subject when their possible existence in supersymmetric extensions of the Standard Model was considered [5,6,7,8], where the U(1) charge is for example the baryon number of the supersymmetric partners of baryons. Flat U(1) directions in the potential of such extensions can offer a plausible explanation to the problem of baryogenesis ( [9,10]).…”

Q-stars in scalar–tensor gravitational theories

“…Q-balls are non-topological solitons in Lagrangians with a global U(1) symmetry, [19], or a local one, [24], or a global SU(3) or SO(3) symmetry, [20]. Q-balls are supposed to appear in the flat directions of the superpotential in supersymmetric extensions of Standard Model, [21,22], and play a special role in the baryogenesis, [23]. Q-stars are relativistic extensions of q-balls, with one or two scalar fields and a global, [25], or local, [28], U(1) symmetry, non-abelian symmetry, [26], or with fermions and a scalar field, [27] in asymptotically flat or anti de Sitter spacetime, [29].…”