Effects of the Symmetry Energy and its Slope on Neutron Star Properties

Abstract

In this work we study the influence of the symmetry energy and its slope on three major properties of neutron stars: the maximum mass, the radii of the canonical 1.4$M_{\odot }$ and the minimum mass that enables the direct URCA effect. We utilize four parametrizations of the relativistic quantum hadrodynamics and vary the symmetry energy within accepted values. We see that although the maximum mass is almost independent of it, the radius of the canonical $1.4M_{\odot }$ and the mass that enables the direct URCA effect is strongly correlated with the symmetry energy and its slope. Also, since we expect that the radius grows with the slope, a theoretical limit arises when we increase this quantity above certain values.

RevTEX; 19 pages, 13 figures

References in corpus (9)

• Shapiro delay measurement of a two solar mass neutron star
• A Massive Pulsar in a Compact Relativistic Binary
• Neutron-Rich Nuclei in Heaven and Earth
• Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
• Constraints on the symmetry energy and on neutron skins from the pygmy resonances in 68Ni and 132Sn
• Magnetic Hydrogen Atmosphere Models and the Neutron Star RX J1856.5-3754
• A Second Relativistic Mean Field and Virial Equation of State for Astrophysical Simulations
• The physics of strong magnetic fields in neutron stars
• The importance of the mixed phase in hybrid stars built with the Nambu-Jona-Lasinio model

Cited by in corpus (7)

• Broken SU(6) symmetry and massive hybrid stars
• A Neutron Star is born
• Reconciling Nuclear and Astrophysical Constraints
• Role of the symmetry energy slope in neutron stars: exploring the model-dependency
• Imprints of the nuclear symmetry energy slope in gravitational wave signals emanating from neutron stars
• The neutron star inner crust: an empirical essay
• Correlation between the symmetry energy slope and the deconfinement phase transition