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Quark Matter In Massive Compact Stars

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arxiv 1102.2869 v2 pith:FMVB3MGO submitted 2011-02-14 astro-ph.HE hep-phnucl-th

Quark Matter In Massive Compact Stars

Simon Weissenborn , Irina Sagert , Giuseppe Pagliara , Matthias Hempel , J\"urgen Schaffner-Bielich This is my paper
classification astro-ph.HE hep-phnucl-th
keywords starsquarkmattermassivecompactconstrainthadronichybrid
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved
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The recent observation of the pulsar PSR J1614-2230 with a mass of 1.97 +/- 0.04 M_sun gives a strong constraint on the quark and nuclear matter equations of state (EoS). We explore the parameter ranges for a parameterized EoS for quark stars. We find that strange stars, made of absolutely stable strange quark matter, comply with the new constraint only if effects from the strong coupling constant and color-superconductivity are taken into account. Hybrid stars, compact stars with a quark matter core and an hadronic outer layer, can be as massive as 2 M_sun, but only for a significantly limited range of parameters. We demonstrate that the appearance of quark matter in massive stars depends crucially on the stiffness of the nuclear matter EoS. We show that the masses of hybrid stars stay below the ones of hadronic and pure quark stars, due to the softening of the EoS at the quark-hadron phase transition.

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Forward citations

Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Is the coexistence of strange quark stars and hadronic stars favored by astrophysical data? A Bayesian analysis

    nucl-th 2026-06 unverdicted novelty 6.0

    Bayesian analysis of astrophysical and laboratory data favors the two-families scenario of coexisting hadronic and strange quark stars over the one-family scenario.

  2. Hybrid Stars with Post-Merger Rotation Profiles

    gr-qc 2026-06 unverdicted novelty 5.0

    Differential rotation in hybrid stars with deconfinement phase transition allows quasi-toroidal configurations with quark matter rings and leads to degeneracies in rotational profiles at mass-radius curve intersections.

  3. Compact star and compact star matter properties from a baryonic extended linear sigma model with explicit chiral symmetry breaking

    nucl-th 2025-12 reject novelty 5.0

    Tuning the πN sigma term to about -600 MeV (or incompressibility to ~500 MeV) lets one RMF model match neutron-star observations, but the tuning is fitting, not prediction.