Please use this identifier to cite or link to this item: https://hdl.handle.net/10316/113298
Title: Spanning the full range of neutron star properties within a microscopic description
Authors: Malik, Tuhin 
Ferreira, Márcio 
Albino, Milena Bastos 
Providência, Constança 
Keywords: Nuclear Theory; astro-ph.HE
Issue Date: 19-Jan-2023
Publisher: American Physical Society
Project: UIDP/04564/2020 
UIDB/04564/ 2020 
2022.06460.PTDC 
FCT - Ph.D. Grant No. 2022.11685.BD 
Serial title, monograph or event: Physical Review D
Volume: 107
Issue: 10
Abstract: The high-density behavior of nuclear matter is analyzed within a relativistic mean-field description with non-linear meson interactions. To assess the model parameters and their output, a Bayesian inference technique is used. The Bayesian setup is limited only by a few nuclear saturation properties, the neutron star maximum mass larger than 2 M$_\odot$, and the low-density pure neutron matter equation of state (EOS) produced by an accurate N$^3$LO calculation in chiral effective field theory. Depending on the strength of the non-linear scalar vector field contribution, we have found three distinct classes of EOSs, each one correlated to different star properties distributions. If the non-linear vector field contribution is absent, the gravitational maximum mass and the sound velocity at high densities are the greatest. However, it also gives the smallest speed of sound at densities below three times saturation density. On the other hand, models with the strongest non-linear vector field contribution predict the largest radii and tidal deformabilities for 1.4 M$_\odot$ stars, together with the smallest mass for the onset of the nucleonic direct Urca processes and the smallest central baryonic densities for the maximum mass configuration. These models have the largest speed of sound below three times saturation density, but the smallest at high densities, in particular, above four times saturation density the speed of sound decreases approaching approximately $\sqrt{0.4}c$ at the center of the maximum mass star. On the contrary, a weak non-linear vector contribution gives a monotonically increasing speed of sound. A 2.75 M$_\odot$ NS maximum mass was obtained in the tail of the posterior with a weak non-linear vector field interaction. We found that pQCD favors models with a large non-linear vector field contribution or hyperons.
Description: There are 17 pages, 16 figures (The typographical error in the supplemental update)
URI: https://hdl.handle.net/10316/113298
ISSN: 2470-0010
2470-0029
DOI: 10.1103/PhysRevD.107.103018
Rights: openAccess
Appears in Collections:I&D CFis - Artigos em Revistas Internacionais

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