Adiabatic evolution of hadronic neutron stars
Abstract
In this paper we compute several structural properties of static and rotating neutron stars, considering both rigid and differential rotation. To this end, we use a finite-temperature beta-stable equation of state (EOS) extending the zero-temperature hadronic EOS derived by Fortin et al. (2017). We account for the formation of hyperons and the presence of a neutrino-trapped component. Our goal is to provide insights into the long-term evolution of a protoneutron star (PNS) formed after a core-collapse supernova (CCSN) or a remnant resulting from a binary neutron star merger (BNSM). The EOS is derived using a relativistic mean-field quantum many-body theory within the Hartree approximation. Coupling constants are determined using experimental data on hypernuclei and hypernuclear matter to better account for uncertainties in hyperon single-particle potentials. Our EOS models reproduce the typical features of cold neutron stars and PNSs for nucleonic and hyperonic compositions. In particular, they are consistent with measured masses (2.01 M_sun and 2.14 M_sun for PSR J0348+0432 and PSR J0740+6620) and dimensionless tidal deformabilities from GW170817. Thermal contributions act differently depending on composition and rotation state. Finally, our evolutionary scheme provides a simple way to interpret the long-term evolution of BNSM remnants or PNSs from CCSNe, complementing dynamical simulations unable to cover full evolutionary timescales.
Related
- Thermal evolution of neo-neutron stars. II. Temperature-dependent crusts
- Magnetic, thermal and rotational evolution of isolated neutron stars
- General Relativistic Simulations of the Nonlinear Evolution of r-modes in Rapidly Rotating Neutron Stars
- Thermal evolution of neo-neutron stars. II. Temperature-dependent crusts
- Structural quasi-universality in highly magnetized, differentially rotating neutron stars
BibTeX
@misc{logoteta2026adiabatic,
title = {{Adiabatic evolution of hadronic neutron stars}},
author = {Domenico Logoteta and Francesco Zeno Constanzo and Ignazio Bombaci and Sebastiano Bernuzzi and Albino Perego and David Radice},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.13926},
eprint = {2610.13926},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.13926},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Adiabatic evolution of hadronic neutron stars
AU - Domenico Logoteta
AU - Francesco Zeno Constanzo
AU - Ignazio Bombaci
AU - Sebastiano Bernuzzi
AU - Albino Perego
AU - David Radice
PY - 2026
DA - 2026/10/09
PB - arXiv
DO - 10.48550/arxiv.2610.13926
UR - https://arxiv.org/abs/2610.13926
AB - In this paper we compute several structural properties of static and rotating neutron stars, considering both rigid and differential rotation. To this end, we use a finite-temperature beta-stable equation of state (EOS) extending the zero-temperature hadronic EOS derived by Fortin et al. (2017). We account for the formation of hyperons and the presence of a neutrino-trapped component. Our goal is to provide insights into the long-term evolution of a protoneutron star (PNS) formed after a core-collapse supernova (CCSN) or a remnant resulting from a binary neutron star merger (BNSM). The EOS is derived using a relativistic mean-field quantum many-body theory within the Hartree approximation. Coupling constants are determined using experimental data on hypernuclei and hypernuclear matter to better account for uncertainties in hyperon single-particle potentials. Our EOS models reproduce the typical features of cold neutron stars and PNSs for nucleonic and hyperonic compositions. In particular, they are consistent with measured masses (2.01 M_sun and 2.14 M_sun for PSR J0348+0432 and PSR J0740+6620) and dimensionless tidal deformabilities from GW170817. Thermal contributions act differently depending on composition and rotation state. Finally, our evolutionary scheme provides a simple way to interpret the long-term evolution of BNSM remnants or PNSs from CCSNe, complementing dynamical simulations unable to cover full evolutionary timescales.
ER -