Abstract
Magnetars are neutron stars in which a strong magnetic field is the main energy source. About two dozens of magnetars, plus several candidates, are currently known in our Galaxy and in the Magellanic Clouds. They appear as highly variable X-ray sources and, in some cases, also as radio and/or optical pulsars. Their spin periods (2–12 s) and spin-down rates (\(\sim10^{-13}\mbox{--}10^{-10}~\mbox{s}\,\mbox{s}^{-1}\)) indicate external dipole fields of \(\sim10^{13-15}\) G, and there is evidence that even stronger magnetic fields are present inside the star and in non-dipolar magnetospheric components. Here we review the observed properties of the persistent emission from magnetars, discuss the main models proposed to explain the origin of their magnetic field and present recent developments in the study of their evolution and connection with other classes of neutron stars.
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Mereghetti, S., Pons, J.A., Melatos, A. (2016). Magnetars: Properties, Origin and Evolution. In: Beskin, V., et al. The Strongest Magnetic Fields in the Universe. Space Sciences Series of ISSI, vol 54. Springer, New York, NY. https://doi.org/10.1007/978-1-4939-3550-5_10
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