Role of the symmetry energy slope in neutron stars: exploring the model-dependency

Abstract

Using six different parametrizations of the quantum hadrodynamics (one of which is original), I study how different values of the symmetry energy slope ($L)$ affect some microscopic and macroscopic properties of neutron stars, such as the proton fraction, the maximum mass, the radius of the canonical 1.4$M_{\odot }$ star and its dimensionless tidal parameter $\Lambda$. I show that while most quantities present the same qualitative results, the tidal parameter can increase or decrease with the slope, depending on the model. Moreover, special attention is given to the minimum mass that enables the direct URCA process to occur in neutron stars' interiors ($M_{DU})$. Assuming the weak constraint $M_{DU}>1.35M_{\odot }$, we see that the maximum value of $L$ that satisfies it lies between 79 and 86 MeV. A range of only 7 MeV. Therefore, $M_{DU}$ is an easy way to impose upper bounds to the slope.

7 pages + Appendix. Similar to the published version

References in corpus (26)

• GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
• A Massive Pulsar in a Compact Relativistic Binary
• PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter
• A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation
• Tidal Love numbers of neutron stars
• Constraining neutron star tidal Love numbers with gravitational wave detectors
• A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy
• PSR J0952-0607: The Fastest and Heaviest Known Galactic Neutron Star
• Implications of PREX-II on the equation of state of neutron-rich matter
• Relativistic Mean-Field Hadronic Models under Nuclear Matter Constraints
• Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
• Relativistic effective interaction for nuclei, giant resonances, and neutron stars
• Neutron star tidal deformability and equation of state constraints
• Constraints on the Symmetry Energy Using the Mass-Radius Relation of Neutron Stars
• GW190814: Impact of a 2.6 solar mass neutron star on nucleonic equations of state
• Probing the Symmetry Energy with the Spectral Pion Ratio
• The Equation of State for the Nucleonic and Hyperonic Core of Neutron Stars
• Neutron skins and neutron stars
• Neutron star cooling: Theoretical aspects and observational constraints
• Statistical theory of thermal evolution of neutron stars - II. Limitations on direct Urca threshold
• On the nature of the mass-gap object in the GW190814 event
• Neutron star structure and collective excitations of finite nuclei
• Effects of the Symmetry Energy and its Slope on Neutron Star Properties
• Imprints of the nuclear symmetry energy slope in gravitational wave signals emanating from neutron stars
• Decoding rotating neutron stars: Role of the symmetry energy slope
• Correlation between the symmetry energy slope and the deconfinement phase transition

Cited by in corpus (8)

• Dense Matter in Neutron Stars with eXTP
• XTE J1814-338 as a dark matter admixed neutron star
• An Undergraduate Approach to the Quantum Hadrodynamics and the Physics of Neutron Stars
• Strongly interacting matter in extreme magnetic fields
• Novel features of asymmetric nuclear matter from terrestrial experiments and astrophysical observations of neutron stars
• New solution to the hyperon puzzle of neutron stars: Quantum many-body effects
• On the Cooling of Compact Stars in Light of the HESS J1731-347 Remnant
• Effects of the symmetry energy slope on magnetized neutron stars