Crystalline chiral condensates as a component of compact stars

TL;DR

This paper explores how inhomogeneous chiral condensates in magnetic fields affect the equation of state of compact stars, showing that such models can support observed massive neutron stars with magnetic fields consistent with magnetar data.

Contribution

It introduces a model incorporating crystalline chiral condensates and magnetic fields into the star's equation of state, demonstrating compatibility with observed neutron star masses.

Findings

Supports stars with masses around 2 solar masses

Magnetic fields consistent with magnetar observations

Inclusion of vector interactions enhances model viability

Abstract

We investigate the influence of spatially inhomogeneous chiral symmetry-breaking condensates in a magnetic field background on the equation of state for compact stellar objects. After building a hybrid star composed of nuclear and quark matter using the Maxwell construction, we find, by solving the Tolman-Oppenheimer-Volkoff equations for stellar equilibrium, that our equation of state supports stars with masses around 2 $M_\odot$ for values of the magnetic field that are in accordance with those inferred from magnetar data. The inclusion of a weak vector interaction term in the quark part allows one to reach 2 solar masses for relatively small central magnetic fields, making this composition a viable possibility for describing the internal degrees of freedom of this class of astrophysical objects.