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Novel Clues to the Physics of Magnetars as Probed with Detailed Pulse-Timing Studies

Published online by Cambridge University Press:  27 February 2023

Kazuo Makishima Open the ORCID record for Kazuo Makishima [Opens in a new window]
Kazuo Makishima*
Affiliation:
Kavli IPMU, University of Tokyo, 5-1-5 Kashiwa-no-ha, Kashiwa, Chiba, Japan, 277-8583 email: [email protected] Dept. of Physics, University of Tokyo, 7-3-1 Hong, Bunkyo-ku, Tokyo, Japan, 113-0033
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Abstract

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Broadband X-ray data of five magnetars show that their hard X-ray pulses suffer periodic phase modulations, at a period ∼ 104 times their pulse period. The phenomenon is interpreted as a result of free precession of neutron stars that are prolately deformed to an asphericity of ∼ 10−4, by the magnetic stress of toroidal fields reaching ∼ 1016 G. The behavior is absent in their soft X-ray pulses, probably due to a higher emission symmetry. The ultra-high toroidal fields, considered common to magnetars, may persist longer than their dipole fields.

Keywords

MagnetarsAstrophysical magnetismNeutron starsPulsarsX-ray sources
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S363: Neutron Star Astrophysics at the Crossroads: Magnetars and the Multimessenger Revolution , June 2020 , pp. 267 - 270
Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

References

Ioka, K., & Sasaki, M. 2004, ApJ, 600, 296 CrossRefGoogle Scholar
Makishima, K. 2016, Proc. Japan Academy, Ser. B, 92, 135 Google Scholar
Makishima, K., Enoto, T., Hiraga, J. S., Nakano, T., 2014, Phys. Rev. Lett., 112, id.171102Google Scholar
Makishima, K., Enoto, T., Murakami, H., Furuta, Y., Nakano, T., 2016, PASJ, 68S, id.12CrossRefGoogle Scholar
Makishima, K., Murakami, H., Enoto, T., & Nakazawa, K. 2019, PASJ, 71, id.15Google Scholar
Makishima, K., Enoto, T., Yoneda, H., & Odaka, H. 2021a, MNRAS, 502, 2266 CrossRefGoogle Scholar
Makishima, K., Tamba, T., Aizawa, Y., Odaka, H., Yoneda, H., 2021b, ApJ, 923, id.63CrossRefGoogle Scholar
Nakano, T., Murakami, H., Makishima, K., Hiraga, J. S., 2015, PASJ 67, id.9CrossRefGoogle Scholar
Yatabe, F., Makishima, K., Mihara, T., Nakajima, M., 2016, PASJ, 70, id.89Google Scholar
Yoneda, H., Makishima, K., Enoto, T., 2020, Phys. Rev. Lett., 125, id.111103Google Scholar