Quark stars with `realistic' equations of state
Abstract
THE possibility of a phase transition between nuclear matter and quark matter has been discussed in recent work^{113}. Free quarks would presumably appear above a critical density pq, which is greater than the typical density ρ_{n} ~= 2.5 × 10^{14}g cm^{3} within ordinary atomic nuclei. Such a transition might allow stable collapsed stars to exist wherein much of the matter is in the form of quark matter (quark stars). The maximum masses of collapsed stars have been investigated for the extreme case of ρ_{q} ~= ρ_{n} and hard equations of state for quark matter^{5}. However, it has been argued^{6,8,9} that some equations of state for quark matter require ρ_{q} >> ρ_{n} and are therefore unlikely to permit the existence of stable quark stars. We investigate here the properties of collapsed stars in the context of another class of quarkmatter models that has recently been proposed^{1113}. These models^{12}, which are consistent with all experimental nuclear and highenergy physics data, are based on a quantum chromodynamic treatment of quarks that are assumed to be of low mass (≲100 MeV for the lightest quarks). We find that stable quark stars are possible (compare with refs 6, 8, 9). However, we also conclude (compare with refs 5, 14) that such stars need not have significantly different macroscopic properties from those of neutronstar models^{1517} based on conventional nuclearmatter equations of state.
 Publication:

Nature
 Pub Date:
 July 1978
 DOI:
 10.1038/274347a0
 Bibcode:
 1978Natur.274..347F
 Keywords:

 Black Holes (Astronomy);
 Neutron Stars;
 Quarks;
 Stellar Models;
 Equations Of State;
 Graphs (Charts);
 Moments Of Inertia;
 Particle Interactions;
 Phase Transformations;
 Red Shift;
 Stellar Mass;
 Stellar Structure;
 Astrophysics