Pulsar Population Synthesis with Magnetorotational Evolution: Constraining the Decay of Magnetic field
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arXiv
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| Autores principales: | , |
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| Formato: | Preprint |
| Publicado: |
2024
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| _version_ | 1866918446524006400 |
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| author | Shi, Zhihong Ng, C. -Y. |
| author_facet | Shi, Zhihong Ng, C. -Y. |
| contents | 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_14786 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Pulsar Population Synthesis with Magnetorotational Evolution: Constraining the Decay of Magnetic field Shi, Zhihong Ng, C. -Y. High Energy Astrophysical Phenomena 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. |
| title | Pulsar Population Synthesis with Magnetorotational Evolution: Constraining the Decay of Magnetic field |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2408.14786 |