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Structure of ultra-magnetised neutron stars

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Abstract

In this review we discuss self-consistent methods to calculate the global structure of strongly magnetised neutron stars within the general-relativistic framework. We outline why solutions in spherical symmetry cannot be applied to strongly magnetised compact stars, and elaborate on a consistent formalism to compute rotating magnetised neutron star models. We also discuss an application of the above full numerical solution for studying the influence of strong magnetic fields on the radius and crust thickness of magnetars. The above technique is also applied to construct a “universal” magnetic field profile inside the neutron star, that may be useful for studies in nuclear physics. The methodology developed here is particularly useful to interpret multi-messenger astrophysical data of strongly magnetised neutron stars.

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Data Availability Statement

This manuscript has no associated data or the data will not be deposited. [Authors’ comment: As this article is a review, we have taken only figures or compilation of data from other recently published articles, to which the references have been provided.]

Notes

  1. For a derivation of the following equations, see e.g. the textbooks [18], chapter 4, or [20].

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Acknowledgements

D.C. would like to thank Veronica Dexheimer and Constança Providência for kindly providing the data for Figs. 1 and 2 on equations of state in this paper.

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Authors and Affiliations

  1. Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune University Campus, Pune, 411007, India

    Debarati Chatterjee

  2. LUTH, Observatoire de Paris, Université PSL, CNRS, Université de Paris, 92195, Meudon, France

    Jérôme Novak & Micaela Oertel

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  1. Debarati Chatterjee
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  2. Jérôme Novak
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Correspondence to Debarati Chatterjee.

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Chatterjee, D., Novak, J. & Oertel, M. Structure of ultra-magnetised neutron stars. Eur. Phys. J. A 57, 249 (2021). https://doi.org/10.1140/epja/s10050-021-00525-5

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