On the initial spin period distribution of neutron stars
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2024
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866909228502876160 |
|---|---|
| author | Du, Shen-Shi Liu, Xiao-Jin Chen, Zu-Cheng You, Zhi-Qiang Zhu, Xing-Jiang Zhu, Zong-Hong |
| author_facet | Du, Shen-Shi Liu, Xiao-Jin Chen, Zu-Cheng You, Zhi-Qiang Zhu, Xing-Jiang Zhu, Zong-Hong |
| contents | We derive the initial spin period distribution of neutron stars by studying the population of young pulsars associated with supernova remnants. Our hierarchical Bayesian approach accounts for the measurement uncertainties of individual observations and selection effects. Without correcting for selection effects, as done in previous studies, we find that pulsar initial spin periods follow a Weibull distribution, peaking at 40~ms, which is favoured against the log-normal distribution with a Bayes factor of 200. The known selection effects in radio pulsar surveys, including pulse broadening and a period-dependent beaming fraction, have been quantitatively investigated. We show that, based on measurements of pulsar luminosity and spin period from the ATNF Pulsar Catalogue, the impact of pulse broadening on the inference of pulsar period distribution is likely to be insignificant. Correcting for the beaming selection effect, a Weibull distribution remains to be the preferred model, while its peak slightly shifts to longer periods at 50~ms. Our method will prove useful in constraining the birth properties of neutron stars in the Square Kilometre Array era. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2402_14030 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | On the initial spin period distribution of neutron stars Du, Shen-Shi Liu, Xiao-Jin Chen, Zu-Cheng You, Zhi-Qiang Zhu, Xing-Jiang Zhu, Zong-Hong High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We derive the initial spin period distribution of neutron stars by studying the population of young pulsars associated with supernova remnants. Our hierarchical Bayesian approach accounts for the measurement uncertainties of individual observations and selection effects. Without correcting for selection effects, as done in previous studies, we find that pulsar initial spin periods follow a Weibull distribution, peaking at 40~ms, which is favoured against the log-normal distribution with a Bayes factor of 200. The known selection effects in radio pulsar surveys, including pulse broadening and a period-dependent beaming fraction, have been quantitatively investigated. We show that, based on measurements of pulsar luminosity and spin period from the ATNF Pulsar Catalogue, the impact of pulse broadening on the inference of pulsar period distribution is likely to be insignificant. Correcting for the beaming selection effect, a Weibull distribution remains to be the preferred model, while its peak slightly shifts to longer periods at 50~ms. Our method will prove useful in constraining the birth properties of neutron stars in the Square Kilometre Array era. |
| title | On the initial spin period distribution of neutron stars |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2402.14030 |