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P-stars are compact stars made of up and down quarks in $\beta$-equilibriumwith electrons in a chromomagnetic condensate. We discuss p-stars endowed withsuper strong dipolar magnetic field which, following consolidated tradition inliterature, are referred to as magnetars. We show that soft gamma-ray repeatersand anomalous $X$-ray pulsars can be understood within our theory. We find awell defined criterion to distinguish rotation powered pulsars from magneticpowered pulsars. We show that glitches, that in our magnetars are triggered bymagnetic dissipative effects in the inner core, explain both the quiescentemission and bursts in soft gamma-ray repeaters and anomalous $X$-ray pulsars.We account for the braking glitch from SGR 1900+14 and the normal glitch fromAXP 1E 2259+586 following a giant burst. We discuss and explain the observedanti correlation between hardness ratio and intensity. Within our magnetartheory we are able to account quantitatively for light curves for bothgamma-ray repeaters and anomalous $X$-ray pulsars. In particular we explain thepuzzling light curve after the June 18, 2002 giant burst from AXP 1E 2259+586.Comment: 42 pages, 15 figures, accepted for publication in Astronomy &  Astrophysic

Magnetars: structure and evolution from p-star models