Strange Quark Stars with a Rotating Superfluid Core

The generation of a magnetic field and its distribution inside a rotating bare strange quark star are discussed. It is shown that the difference between the angular velocities of the superfluid and superconducting quark core Ω s and of the normal electron plasma Ω n increases because of spin-down of the star and this leads to the generation of a magnetic field. The magnetic field distribution in a star is found for a stationary value of ∆Ω=Ω s - Ω n = const . The magnetic field in the superconducting quark core and in the normal electron shell is continuous along the star’s axis of rotation and has the same value B q = B n , while it is a dipole field outside the star. In all parts of the star this field is determined entirely by the total magnetic moment M of the star. It is also shown that the star’s magnetic moment M is proportional to ΔW, and for some models of compact stars it can vary from 10 31 -10 34 G·cm 3 .