On the origin of the strong internal magnetic fields of central compact objects
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arXiv
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| Format: | Preprint |
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2026
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| _version_ | 1866914413520355328 |
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| author | Ekşi, Kazım Yavuz Bakır, İrem |
| author_facet | Ekşi, Kazım Yavuz Bakır, İrem |
| contents | Central compact objects are radio-quite young neutron stars associated with supernova remnants. They have relatively small dipole fields, $B_{\rm p} \sim 10^{10}\,{\rm G}$ as inferred from their spin parameters. X-ray observations and theoretical arguments imply the presence of stronger internal magnetic fields. We argue that the dipole fields of these objects are very close to what they had inherited from the \textit{core} of the progenitor by flux conservation and their small initial rotation frequency does not allow for the $α$-process to enhance their poloidal fields. Although a full-fledged dynamo process can not proceed, relatively strong toroidal magnetic fields, $B_ϕ\sim 10^{13}\,{\rm G}$, can be generated from the seed poloidal fields via the $Ω$-effect in the proto-neutron star stage. We present a simplistic model for these processes and further speculate that the reason why these objects are born relatively slow-rotating is that they were not spun-up by acquiring angular momentum from the fallback matter. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2603_21103 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | On the origin of the strong internal magnetic fields of central compact objects Ekşi, Kazım Yavuz Bakır, İrem High Energy Astrophysical Phenomena Central compact objects are radio-quite young neutron stars associated with supernova remnants. They have relatively small dipole fields, $B_{\rm p} \sim 10^{10}\,{\rm G}$ as inferred from their spin parameters. X-ray observations and theoretical arguments imply the presence of stronger internal magnetic fields. We argue that the dipole fields of these objects are very close to what they had inherited from the \textit{core} of the progenitor by flux conservation and their small initial rotation frequency does not allow for the $α$-process to enhance their poloidal fields. Although a full-fledged dynamo process can not proceed, relatively strong toroidal magnetic fields, $B_ϕ\sim 10^{13}\,{\rm G}$, can be generated from the seed poloidal fields via the $Ω$-effect in the proto-neutron star stage. We present a simplistic model for these processes and further speculate that the reason why these objects are born relatively slow-rotating is that they were not spun-up by acquiring angular momentum from the fallback matter. |
| title | On the origin of the strong internal magnetic fields of central compact objects |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2603.21103 |