Charged rho superconductor in the presence of magnetic field and rotation

In this work, we mainly explore the possibility of charged rho ($$\rho ^\pm $$ ρ ± ) superconductor in the presence of parallel magnetic field and rotation within three-flavor Nambu–Jona-Lasino model. By following similar schemes as in the previous studies of charged pion ($$\pi ^\pm $$ π ± ) superfluid, the $$\rho ^\pm $$ ρ ± superconductor is found to be favored for both choices of Schwinger phase in Minkowski and curved spaces. Due to the stability of the internal spin structure, charged rho begins to condensate at a smaller threshold of angular velocity than charged pion for the given large magnetic fields. Even the axial vector meson condensation is checked – the conclusion is that $$\rho ^\pm $$ ρ ± superconductor is the robust ground state at strong magnetic field and fast rotation, which actually sustains to very large angular velocity.

a1-meson-baryon coupling constants in the framework of soft-wall and hard-wall AdS/QCD models

We calculate the [Formula: see text]-meson-nucleon ([Formula: see text]-baryon) coupling constant in the framework of soft-wall and hard-wall AdS/QCD models. Interaction Lagrangian in the bulk of AdS space was written for a minimal gauge coupling, a magnetic type coupling and a triple coupling of bulk fields. Applying AdS/CFT correspondence from the bulk interaction Lagrangian, we obtain holographic expressions for the [Formula: see text]-axial-vector meson-nucleon ([Formula: see text]-baryon) coupling constant in the boundary QCD theory. Numerical results for the [Formula: see text] coupling constant in the framework of both models are close to the known phenomenological estimates. The [Formula: see text]-axial-vector meson-[Formula: see text]-baryon coupling constant was considered in the framework of hard-wall model.

Compact Star Properties from an Extended Linear Sigma Model

The equation of state provided by effective models of strongly interacting matter should comply with the restrictions imposed by current astrophysical observations of compact stars. Using the equation of state given by the (axial-)vector meson extended linear sigma model, we determine the mass–radius relation and study whether these restrictions are satisfied under the assumption that most of the star is filled with quark matter. We also compare the mass–radius sequence with those given by the equations of state of somewhat simpler models.