Neutron Stars with a Stable, Light Supersymmetric Baryon

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Abstract
If a light gluino exists, the lightest gluino-containing baryon, S0, is a possible candidate for self-interacting dark matter. In this scenario, the simplest explanation for the observed ratio ΩDM/Ωb ≈ 6-10 is that m ~ 900 MeV c-2; at present, this is not excluded by particle physics. Such an S0 could be present in neutron stars, with the hyperon formation serving as an intermediate stage. We calculate equilibrium compositions and the equation of state for high-density matter with S0, and we find that for a wide range of parameters, the properties of neutron stars with S0 are consistent with observations. In particular, the maximum mass of a nonrotating star is 1.7-1.8 M☉, and the presence of S0 is helpful in reconciling observed cooling rates with hyperon formation.

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