Connecting radio pulsars, magnetars, and XDINSs in a unified evolutionary framework using simulation-based inference
Abstract
Understanding the Galactic population of isolated neutron stars within a unified framework provides key insights into their birth properties, evolutionary pathways, and the connections between different neutron star classes. In this work, we aim to reproduce both the observed radio and quiescent X-ray emission from isolated neutron stars, including radio pulsars, magnetars and X-ray dim isolated neutron stars (XDINSs). We develop a comprehensive population synthesis framework that models neutron star birth properties, their dynamical, rotational, and magneto-thermal evolution, as well as radio and X-ray emission, and the selection effects of corresponding surveys. To simulate realistic X-ray spectra, we account for magnetospheric resonant cyclotron scattering and interstellar absorption. Additionally, we model the observational bias introduced by magnetar outbursts, by linking the outburst rate to magnetic stresses in the stellar crust. We then employ a simulation-based inference method, namely truncated sequential neural posterior estimation, to reconstruct the birth properties, such as the initial magnetic field distribution. We find that the Galactic neutron star population can be described by a two-component log-normal distribution of birth magnetic fields with peaks at 5 × 1012 G and 1014 G, respectively. We further find that the Galactic neutron star birth rate is around 3-4 per century. Our results help establish the contribution of neutron stars as central engines of powerful astrophysical transient phenomena, such as fast radio bursts, super-luminous supernovae and gamma ray bursts.
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BibTeX
@misc{ronchi2026connecting,
title = {{Connecting radio pulsars, magnetars, and XDINSs in a unified evolutionary framework using simulation-based inference}},
author = {Michele Ronchi and Celsa Pardo-Araujo and Vanessa Graber and Nanda Rea and Clara Dehman and Davide De Grandis and Alessio Marino and Francesco Coti Zelati and Joeri van Leeuwen and José A. Pons},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.00962},
eprint = {2609.00962},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.00962},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Connecting radio pulsars, magnetars, and XDINSs in a unified evolutionary framework using simulation-based inference
AU - Michele Ronchi
AU - Celsa Pardo-Araujo
AU - Vanessa Graber
AU - Nanda Rea
AU - Clara Dehman
AU - Davide De Grandis
AU - Alessio Marino
AU - Francesco Coti Zelati
AU - Joeri van Leeuwen
AU - José A. Pons
PY - 2026
DA - 2026/09/01
PB - arXiv
DO - 10.48550/arxiv.2609.00962
UR - https://arxiv.org/abs/2609.00962
AB - Understanding the Galactic population of isolated neutron stars within a unified framework provides key insights into their birth properties, evolutionary pathways, and the connections between different neutron star classes. In this work, we aim to reproduce both the observed radio and quiescent X-ray emission from isolated neutron stars, including radio pulsars, magnetars and X-ray dim isolated neutron stars (XDINSs). We develop a comprehensive population synthesis framework that models neutron star birth properties, their dynamical, rotational, and magneto-thermal evolution, as well as radio and X-ray emission, and the selection effects of corresponding surveys. To simulate realistic X-ray spectra, we account for magnetospheric resonant cyclotron scattering and interstellar absorption. Additionally, we model the observational bias introduced by magnetar outbursts, by linking the outburst rate to magnetic stresses in the stellar crust. We then employ a simulation-based inference method, namely truncated sequential neural posterior estimation, to reconstruct the birth properties, such as the initial magnetic field distribution. We find that the Galactic neutron star population can be described by a two-component log-normal distribution of birth magnetic fields with peaks at 5 × 10^12 G and 10^14 G, respectively. We further find that the Galactic neutron star birth rate is around 3-4 per century. Our results help establish the contribution of neutron stars as central engines of powerful astrophysical transient phenomena, such as fast radio bursts, super-luminous supernovae and gamma ray bursts.
ER -