Tidal deformability and other global parameters of compact stars with strong phase transitions

Strong WQO phase transitions

We elaborate Weiermann-style phase transitions for Gordeev well-quasi-ordering (called well-partial-ordering below, abbr.: wpo) results with respect to nested finite sequences and nested finite trees under the homeomorphic embedding with symmetrical gap condition. For every nested partial ordering in question, E, we fix a natural extension of Peano Arithmetic, T, that proves the corresponding 2...

Spin - down of Relativistic Stars with Phase Transitions and PSR

Quark phases in neutron stars and a “ third family ” of compact stars as a signature for phase transitions ∗

Quark phases in neutron stars and a " third family " of compact stars as a signature for phase transitions * Abstract The appearance of quark phases in the dense interior of neutron stars provides one possibility to soften the equation of state (EOS) of neutron star matter at high densities. This softening leads to more compact equilibrium configurations of neutron stars compared to pure hadron...

The Energy Release–stellar Angular Momentum Independence in Rotating Compact Stars Undergoing First-order Phase Transitions

We present the general relativistic calculation of the energy release associated with a first order phase transition (PT) at the center of a rotating neutron star (NS). The energy release, Erel, is equal to the difference in mass-energies between the initial (normal) phase configuration and the final configuration containing a superdense matter core, assuming constant total baryon number and th...

Single-flavor CSL phase in compact stars

We suggest a scenario where the three light quark flavors are sequentially deconfined under increasing pressure in cold asymmetric nuclear matter as, e.g., in neutron stars. The basis for our analysis is a chiral quark matter model of Nambu–Jona-Lasinio (NJL) type with diquark pairing in the spin-1 single flavor (CSL), spin-0 two flavor (2SC) and three flavor (CFL) channels. We find that nucleo...