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We present new stable solutions of the Tolman Oppenheimer Volkoff equationsfor quark stars using a quark matter equation of state based on the SU(3)Quark-Meson model that exhibits the onset of the chiral phase transition. Thesenew solutions appear as two stable branches in the mass-radius relationallowing for so called twin stars, i.e. two stable quark star solutions withthe same mass, but distinctly different radii. We find solutions which arecompatible with causality, the stability conditions of dense matter, theastrophysical constraints of the rotation of the millisecond pulsar PSRJ1748-2446ad and the 2$M_{\odot}$ pulsar mass constraint.

Twin Stars within the SU(3) Chiral Quark-Meson Model