Pulsar Population Synthesis with Magnetorotational Evolution: Constraining the Decay of Magnetic field

[2408.14786] Pulsar Population Synthesis with Magnetorotational Evolution: Constraining the Decay of Magnetic field Skip to main content Search Submit Donate Log in Search arXiv Press Enter to search · Advanced search Astrophysics > High Energy Astrophysical Phenomena arXiv:2408.14786 (astro-ph) [Submitted on 27 Aug 2024 ( v1 ), last revised 15 Apr 2026 (this version, v4)] Title: Pulsar Population Synthesis with Magnetorotational Evolution: Constraining the Decay of Magnetic field Authors: Zhihong Shi , C.-Y. Ng View a PDF of the paper titled Pulsar Population Synthesis with Magnetorotational Evolution: Constraining the Decay of Magnetic field, by Zhihong Shi and C.-Y. Ng View PDF HTML (experimental) Abstract: We present a population synthesis model for normal radio pulsars in the Galaxy incorporating the latest developments in the field and the magnetorotational evolution processes. Our model considers spin-down with a force-free magnetosphere and the decay of the magnetic field strength and its inclination angle. The simulated pulsar population is fit to a large observation sample that covers the majority of radio surveys using the Markov Chain Monte Carlo technique. We compare the distributions of four major observables: spin period (P), spin down rate($\dot{P}$), dispersion measure, and radio flux density using accurate high-dimensional Kolmogoro-Smirnov statistics. We test two B-field decay scenarios, an exponential model motivated by ohmic dissipation and a power-law model motivated by the Hall effect. The former clearly provides a better fit, and it can successfully reproduce the observed pulsar distributions with a decay timescale of $8.3_{-3.0}^{+3.9}$ Myr. The result suggests that significant B-field decay in aged pulsars and ohmic dissipation could be the dominant process. Comments: 17 pages, 10 figures. Published by APJ. A typo was found in Figure 7 x-axis and Table 3 in the published APJ version, we corrected that and included two addition figures for better visualization of the birth location, and core and cone model in this version Subjects: High Energy Astrophysical Phenomena (astro-ph.HE) Cite as: arXiv:2408.14786 [astro-ph.HE] (or arXiv:2408.14786v4 [astro-ph.HE] for this version) https://doi.org/10.48550/arXiv.2408.14786 Focus to learn more arXiv-issued DOI via DataCite Related DOI : https://doi.org/10.3847/1538-4357/ad5af8 Focus to learn more DOI(s) linking to related resources Submission history From: Zhihong Shi [ view email ] [v1] Tue, 27 Aug 2024 05:26:31 UTC (1,982 KB) [v2] Tue, 3 Sep 2024 16:18:11 UTC (12,138 KB) [v3] Fri, 20 Sep 2024 07:15:30 UTC (7,038 KB) [v4] Wed, 15 Apr 2026 04:36:24 UTC (7,731 KB) Full-text links: Access Paper: View a PDF of the paper titled Pulsar Population Synthesis with Magnetorotational Evolution: Constraining the Decay of Magnetic field, by Zhihong Shi and C.-Y. 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