Relativistic hybrid stars with sequential first-order phase transitions and heavy-baryon envelopes

Understand

We compute the mass, radius and tidal deformability of stars containing phase transitions from hadronic to quark phase(s).

• These quantities are computed for three types of hadronic envelopes: purely nuclear, hyperonic, and $\Delta$-resonance--hyperon admixed matter.
• We consider either a single first-order phase transition to a quark phase with a maximally stiff equation of state (EOS) or two sequential first-order phase transitions mimicking a transition from hadronic to a quark matter phase followed by a second phase transition to another quark phase.
• We explore the parameter space which produces low-mass twin and triplet configurations where equal-mass stars have substantially different radii and tidal deformabilities.