Quark-quark interaction and quark matter in neutron stars
arXiv:2112.12931 · doi:10.1103/PhysRevC.105.015804
Abstract
Hyperon () mixing in neutron-star matter brings about a remarkable softening of the equation of state (EoS) and the maximum mass is reduced to a value far less than . One idea to avoid this "hyperon puzzle in neutron stars" is to assume that the many-body repulsions work universally for every kind of baryons. The other is to take into account the quark deconfinement phase transitions from a hadronic EoS to a sufficiently stiff quark-matter EoS. In the present approach, both effects are handled in a common framework. As well as the hadronic matter, the quark matter with the two-body quark-quark interactions are treated within the Brueckner-Bethe-Goldstone theory beyond the mean field frameworks, where interaction parameters are based on the terrestrial data. The derived mass-radius relations of neutron stars show that maximum masses reach over even in the cases of including hadron-quark phase transitions, being consistent with the recent observations for maximum masses and radii of neutron stars by the NICER measurements and the other multimessenger data.
References in corpus (24)
- GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
- Shapiro delay measurement of a two solar mass neutron star
- A Massive Pulsar in a Compact Relativistic Binary
- The equation of state for nucleon matter and neutron star structure
- Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar
- A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy
- From hadrons to quarks in neutron stars: a review
- Implications of PREX-II on the equation of state of neutron-rich matter
- Hyperon mixing and universal many-body repulsion in neutron stars
- Phenomenological QCD equation of state for massive neutron stars
- Neutron stars and quark phases in the NJL model
- Extended-soft-core Baryon-Baryon Model Esc08 II. Hyperon-Nucleon Interactions
- Hybrid equation of state with pasta phases and third family of compact stars
- Chiral phase transition in an extended NJL model with higher-order multi-quark interactions
- Impact of the neutron star crust on the tidal polarizability
- Hybrid and quark star matter based on a non-perturbative equation of state
- Hyperon-mixed neutron star with universal many-body repulsion
- First-order phase transition from hypernuclear matter to deconfined quark matter obeying new constraints from compact star observations
- Constraining quark-hadron interface tension in the multi-messenger era
- Two novel approaches to the hadron-quark mixed phase in compact stars
- Heavy hybrid stars from multi-quark interactions
- Neutron-star radii based on realistic nuclear interactions
- Extended-soft-core Baryon-Baryon Model ESC08 I. Nucleon-Nucleon Scattering
- Mixed phase transition from hypernuclear matter to deconfined quark matter fulfilling mass-radius constraints of neutron stars