The thermal structure of neutron star envelopes is discussed with emphasis on analytic results. Recent progress on the effect of chemical constitution and high magnetic fields on the opacities and the thermal structure is further reviewed in view of the application to pulsar cooling and magnetars.

‎In this work, we review the formalism which would allow us to model magnetically deformed neutron stars. We study the effect of different magnetic field configurations on the equation of state (EoS) and ‎the ‎structure of such stars. ‎For this aim‎, the EoS of magnetars is acquired by using the lowest order constraint variational (LOCV) method ‎‎and ‎employing‎ the AV18 potential‎.‎...

The natural candidates for the realization of color superconductivity are the extremely dense cores of compact stars, many of which have very large magnetic fields, especially the so-called magnetars. In this paper we discuss how a color superconducting core can serve to generate and enhance the stellar magnetic field without appealing to a magnetohydrodynamic dynamo mechanism.

ABSTRACT We study dynamics of relativistic coronal mass ejections (CMEs), from launching by shearing foot-points (either slowly – the ‘Solar flare’ paradigm, or suddenly ‘star quake’ paradigm), to propagation in preceding magnetar wind. For slow shear, most energy injected into CME is first spent on work done breaking through overlaying magnetic field. At later stages, sufficiently powerful CME...

We calculated the ellipticity of the deformed star due to the rotation or magnetic field. These two effects are compared to each other within general relativity. It turned out that the magnetic distortion is important for recently observed candidates of magnetars, while the magnetic effect can be neglected for well-known typical pulsars.

There is growing evidence that two classes of high-energy sources, the Soft Gamma Repeaters and the Anomalous X-ray Pulsars contain slowly spinning “magnetars”, i.e. neutron stars whose emission is powered by the release of energy from their extremely strong magnetic fields (> 1015 G). We show here that the enormous energy liberated in the 2004 December 27 giant flare from SGR 1806-20 (∼ 5×1046...