2002/12/31 by M. Baldo, Michael Buballa, M. Buballa +6 · 3 citations
Earth and Planetary Sciences · Physics and Astronomy · #Atomic and Subatomic Physics Research #High-pressure geophysics and materials #Pulsars and Gravitational Waves Research #astro-ph #hep-ph #nucl-th
paper · pdf · doi:10.1016/s0370-2693(03)00556-2
published as Phys.Lett.B562:153-160,2003 · 11 pages, 3 figures, v2: minor corrections in the text, layout of the figures improved, references added, v3: transition densities from hadronic to quark matter added, version accepted for publication in PLB
arxiv created 2003/04/02 · openalex publication_date 2003/05/13 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We explore the relevance of color superconductivity inside a possible quark matter core for the bulk properties of neutron stars. For the quark phase we use an Nambu--Jona-Lasinio (NJL) type model, extended to include diquark condensates. For the hadronic phase, a microscopic many-body model is adopted, with and without strangeness content. In our calculations, a sharp boundary is assumed between the hadronic and the quark phases. For NJL model parameters fitted to vacuum properties we find that no star with a pure quark core does exist. Nevertheless the presence of color superconducting phases can lower the neutron star maximum mass substantially. In some cases, the transition to quark matter occurs only if color superconductivity is present. Once the quark phase is introduced, the value of the maximum mass stays in any case below the value of two solar masses.