Compact star properties from an extended linear sigma model
arXiv:1907.05841 · doi:10.3390/universe5070174
Abstract
The equation of state provided by effective models of strongly interacting matter should comply with the restrictions imposed by current astrophysical observations of compact stars. Using the equation of state given by the (axial-)vector meson extended linear sigma model, we determine the mass-radius relation and study whether these restrictions are satisfied under the assumption that most of the star is filled with quark matter. We also compare the mass-radius sequence with those given by the equations of state of somewhat simpler models.
11 pages, 6 figures
References in corpus (9)
- Shapiro delay measurement of a two solar mass neutron star
- A Massive Pulsar in a Compact Relativistic Binary
- Neutron Star Observations: Prognosis for Equation of State Constraints
- The QCD transition temperature: results with physical masses in the continuum limit
- Challenges in QCD matter physics - The Compressed Baryonic Matter experiment at FAIR
- A new quark-hadron hybrid equation of state for astrophysics - I. High-mass twin compact stars
- Nuclear symmetry energy and its density slope at normal density extracted from global nucleon optical potentials
- Constraining the properties of neutron-star matter with observations
- Estimating the variation of neutron star observables by symmetric dense nuclear matter properties