The birth mass function of neutron stars
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arXiv
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| Auteurs principaux: | , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866912257468792832 |
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| author | You, Zhi-Qiang Zhu, Xingjiang Liu, Xiaojin Müller, Bernhard Heger, Alexander Stevenson, Simon Thrane, Eric Chen, Zu-Cheng Sun, Ling Lasky, Paul Galloway, Duncan K. Hobbs, George Manchester, Richard N. Gao, He Zhu, Zong-Hong |
| author_facet | You, Zhi-Qiang Zhu, Xingjiang Liu, Xiaojin Müller, Bernhard Heger, Alexander Stevenson, Simon Thrane, Eric Chen, Zu-Cheng Sun, Ling Lasky, Paul Galloway, Duncan K. Hobbs, George Manchester, Richard N. Gao, He Zhu, Zong-Hong |
| contents | The birth mass function of neutron stars encodes rich information about supernova explosions, double star evolution, and properties of matter under extreme conditions. To date, it has remained poorly constrained by observations, however. Applying probabilistic corrections to account for mass accreted by recycled pulsars in binary systems to mass measurements of 90 neutron stars, we find that the birth masses of neutron stars can be described by a unimodal distribution that smoothly turns on at $1.1 M_{\odot}$, peaks at $1.27 M_{\odot}$, before declining as a steep power law. Such a ``turn-on" power-law distribution is strongly favoured against the widely-adopted empirical double-Gaussian model at the $3 σ$ level. The power-law shape may be inherited from the initial mass function of massive stars, but the relative dearth of massive neutron stars implies that single stars with initial masses greater than $\approx 18 M_{\odot}$ do not form neutron stars, in agreement with the absence of massive red supergiant progenitors to supernovae. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2412_05524 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The birth mass function of neutron stars You, Zhi-Qiang Zhu, Xingjiang Liu, Xiaojin Müller, Bernhard Heger, Alexander Stevenson, Simon Thrane, Eric Chen, Zu-Cheng Sun, Ling Lasky, Paul Galloway, Duncan K. Hobbs, George Manchester, Richard N. Gao, He Zhu, Zong-Hong High Energy Astrophysical Phenomena Solar and Stellar Astrophysics The birth mass function of neutron stars encodes rich information about supernova explosions, double star evolution, and properties of matter under extreme conditions. To date, it has remained poorly constrained by observations, however. Applying probabilistic corrections to account for mass accreted by recycled pulsars in binary systems to mass measurements of 90 neutron stars, we find that the birth masses of neutron stars can be described by a unimodal distribution that smoothly turns on at $1.1 M_{\odot}$, peaks at $1.27 M_{\odot}$, before declining as a steep power law. Such a ``turn-on" power-law distribution is strongly favoured against the widely-adopted empirical double-Gaussian model at the $3 σ$ level. The power-law shape may be inherited from the initial mass function of massive stars, but the relative dearth of massive neutron stars implies that single stars with initial masses greater than $\approx 18 M_{\odot}$ do not form neutron stars, in agreement with the absence of massive red supergiant progenitors to supernovae. |
| title | The birth mass function of neutron stars |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2412.05524 |