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We present new X-ray observations of the A0p stars alpha^2 CVn (log Lx < 26.0erg/s) and IQ Aur (log Lx = 29.6 erg/s) and find that their X-ray luminositiesdiffer by at least three orders of magnitude. IQ Aur possesses a strong coolplasma component with X-ray emitting regions located well above the stellarsurface, but also significant amounts of hot plasma. Further, a large X-rayflare is detected from IQ Aur, implying the presence of magnetic reconnection.Our comparison study of similar stars indicates that the occurrence of X-rayemission generated by magnetically channelled wind shocks (MCWS) stronglydepends on stellar properties. X-ray emission is preferably generated by moreluminous and massive objects such as IQ Aur. The MCWS scenario can consistentlydescribe the X-ray emission of these A0p stars, assuming that the very strongmagnetic confinement of the stellar wind has led to the build up of a rigidlyrotating disk around the star, where magnetic reconnection and centrifugalbreakout events occur.

New X-ray observations of IQ Aurigae and alpha2 Canum Venaticorum - Probing the magnetically channelled wind shock model in A0p stars