Abstract
Magnetars have been observationally determined to have surface magnetic fields of order of 10 14 – 10 15 G, and the implied internal field strength may be even larger. We discuss the effect of strong field on the dense matter expected to be inside neutron stars. We describe the microphysics, phenomenology, and astrophysical implications of strong field induced unpairing effect that may occur in magnetars, if the local magnetic field in the core of a magnetar exceeds a critical value. The density dependence of the pairing of proton condensate implies that the critical value required for the unpairing effect to occur is maximal at the crust–core interface and decreases towards the center of the star. As a consequence, magnetar cores with homogeneous constant fields will be partially superconducting for “medium-field” magnetars, whereas “strong-field” magnetars will be void of superconductivity. We also discuss its effect on some observational phenomena which depend on the nature and composition of matter inside neutron stars.
Highlights
The densest matter in the universe is found inside neutron stars with average density of the order of 1014 g/cm3
It was soon established that pulsars are neutron stars with strong surface magnetic fields ranging from 108 to 1012−13 G [2,3]
We consider that the field inside the star increases gradually from the surface to the center, and the variation of field strength is modeled with the density profile of the field as [25]
Summary
The densest matter in the universe is found inside neutron stars with average density of the order of 1014 g/cm. Theoretical prediction of existence of neutron star was first established with the observation of pulsars—the pulsating astrophysical objects Radiation from these objects comes in pulses with periods in the range of ms–s. Later on, some astrophysical objects, namely soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs), were observed [4,5,6,7,8,9,10] They are believed to be neutron stars having very strong surface magnetic fields of the order of 1014–1015 G. We discuss the properties of dense matter relevant for compact stellar objects under the influence of a strong magnetic field with two models of neutron star matter: baryonic matter with and without hyperons and the strange quark matter. We discuss the superconducting nature of proton fluid inside the neutron star in the presence of a strong magnetic field
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