Oscillating Magnetized Color Superconducting Quark Stars

TL;DR

This paper investigates the structure and oscillation properties of magnetized color superconducting quark stars using the MIT bag model, providing insights relevant for gravitational wave astronomy and neutron star asteroseismology.

Contribution

It introduces a detailed model of magnetized color superconducting quark stars and calculates their oscillation modes, aligning theoretical predictions with astrophysical observations.

Findings

Color superconducting magnetized quark stars satisfy pulsar mass constraints.

Oscillation $f$ mode frequencies follow universal relations for compact objects.

Results support the potential detectability of quark star oscillations via gravitational waves.

Abstract

The main objective of this work is to study the structure, composition, and oscillation modes of color superconducting quark stars with intense magnetic fields. We adopted the MIT bag model within the color superconductivity CFL framework, and we included the effects of strong magnetic fields to construct the equation of state of stable quark matter. We calculated observable quantities, such as the mass, radius, frequency, and damping time of the oscillation fundamental $f$ mode of quark stars, taking into account current astrophysical constraints. The results obtained show that color superconducting magnetized quark stars satisfy the constraints imposed by the observations of massive pulsars and gravitational wave events. Furthermore, the quantities associated with the oscillation $f$ mode of these objects fit the universal relationships for compact objects. In the context of the new multi-messenger gravitational wave astronomy era and the future asteroseismology of neutron stars, we hope that our results contribute to the understanding of the behavior of dense matter and compact objects.