Neutron Stars with a Stable, Light Supersymmetric Baryon

Details Neutron Stars with a Stable, Light Supersymmetric Baryon Neutron Stars with a Stable, Light Supersymmetric Baryon

2000-10-05

arxiv.org/abs/astro-ph/0010112v2

Astrophys.J. 548 (2001) L179-L182

Astronomy and Astrophysics

Astrophysics

ApJL submitted, 4 pages, using emulateapj (very very minor changes to match published version

Scientific paper

10.1086/319101

If a light gluino exists, the lightest gluino-containing baryon, the \OSO, is a possible candidate for self-interacting dark matter. In this scenario, the simplest explanation for the observed ratio $\Omega_{dm}/\Omega_b \approx 6-10$ is that $m_{S^0} \sim 900$\MeVcs; this is not at present excluded by particle physics. Such an \OSO could be present in neutron stars, with hyperon formation serving as an intermediate stage. We calculate equilibrium compositions and equation of state for high density matter with the \OSO, and find that for a wide range of parameters the properties of neutron stars with the \OSO are consistent with observations. In particular, the maximum mass of a nonrotating star is $1.7-1.8 M_\odot$, and the presence of the \OSO is helpful in reconciling observed cooling rates with hyperon formation.

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