Neutron stars in the large-$N_{c}$ limit

TL;DR

This paper investigates the phase transition from baryonic to quark matter in neutron stars within the large-$N_{c}$ limit, revealing how the transition affects star maximum mass and constrains the properties of dense matter.

Contribution

It derives the scaling of the critical chemical potential with $N_{c}$ and explores the implications for neutron star maximum mass and the stiffness of baryonic matter.

Findings

Quark matter suppression increases with $N_{c}$.

Phase transition occurs in stars for $3 o 5.5$ $N_{c}$, affecting maximum mass.

Constraints on baryonic matter stiffness are established.

Abstract

We study the phase transition from dense baryonic matter to dense quark matter within the large-$N_{c}$ limit. By using simple constant speed of sound equations of state for the two phases, we derive the scaling with $N_{c}$ of the critical quark chemical potential $\mu_{c}^{\mathrm{crit}}$ for this phase transition. While quark matter is strongly suppressed at large $N_{c}$, the phase transition at a large but finite density could nevertheless be important to determine the maximum mass of compact stars. In particular, in the range $3\leq N_{c}\lesssim5.5$ the quark phase would take place in compact stars and would lead to the formation of an unstable branch of hybrid stars. As a consequence, the maximum mass is restricted to the range $2.1M_{\odot}<M_{max}<3M_{\odot}$. For larger value of $N_{c}$, the phase transition would occur at densities too high to be reached in the core of compact stars. However, the very requirement that it occurs (although at a very large density) translates into interesting constraints on the stiffness of the baryonic phase: its speed of sound must exceed $\sqrt{1/3}$.