Abstract
The birth function of neutron stars in magnetic field \(B\) is estimated for two models of the evolution of radio pulsars corresponding to different directions of evolution of the inclination angle of the magnetic axis to the rotation axis \(\chi\) (toward small angles \({\sim}0^{\circ}\) or angles close to \(90^{\circ}\)). We show that for both models at magnetic fields \(B>10^{12}\) G it is a power law with a break near \(10^{13}\) G. At the same time, however, the number of born pulsars with a super-strong magnetic field \(B>10^{14}\) G in the first model turns out to be smaller than that in the second one by an order of magnitude.
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ACKNOWLEDGMENTS
We are grateful to A.V. Biryukov and E.M. Novoselov for the useful discussion and to R.V. Todorov for his help with the calculations. We also thank the referees for their important remarks that allowed many of the questions touched on in the paper to be clarified.
Funding
This work was supported by the Russian Foundation for Basic Research (project no. 20-02-00469).
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Translated by V. Astakhov
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Beskin, V.S., Zagorulia, D.S. & Istomin, A.Y. Magnetic Fields of Neutron Stars. Astron. Lett. 47, 686–694 (2021). https://doi.org/10.1134/S1063773721100017
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DOI: https://doi.org/10.1134/S1063773721100017