التفاصيل البيبلوغرافية
| العنوان: |
Implications of oscillating toroidal fields of proto-neutron stars for pulsars and magnetars |
| المؤلفون: |
Bak��r, ��rem, Ek��i, Kaz��m Yavuz |
| بيانات النشر: |
arXiv, 2021. |
| سنة النشر: |
2021 |
| مصطلحات موضوعية: |
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences |
| الوصف: |
A fraction of young neutron stars, magnetars, have ultra-strong magnetic fields. Models invoked for their strong fields require highly specific conditions with extreme parameters which are incompatible with the inference that the magnetar birth rate is comparable to the rate of core-collapse supernovae. We suggest that these seemingly contradictory trends can be reconciled if the toroidal magnetic fields are subject to oscillations following the proto-neutron star (PNS) dynamo stage. Depending on the phase of the oscillation at which the oscillations are terminated, the neutron star can have a very high ($\gtrsim 10^{15}\,{\rm G}$) or relatively small ($\sim 10^{14}\,{\rm G}$) toroidal field. As an example, we invoke a shear-driven dynamo model for the generation of PNS magnetic fields and show that the toroidal field indeed exhibits oscillations following the dynamo stage. We argue that these Alfv��nic oscillations can lead to the formation of both magnetars and ordinary neutron stars depending on at what phase of the oscillation the fields froze.
5 pages, 1 figure and supplementary material (3 pages, 3 figures). Some change in the terminology to comply with the referee comments + further explanations |
| DOI: |
10.48550/arxiv.2108.01051 |
| URL الوصول: |
https://explore.openaire.eu/search/publication?articleId=doi_________::ae13cb77683b394c9e3a3bc9c133cace |
| رقم الانضمام: |
edsair.doi...........ae13cb77683b394c9e3a3bc9c133cace |
| قاعدة البيانات: |
OpenAIRE |