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

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

2011-05-18

arxiv.org/abs/1105.3688v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

11 pages, 10 figures, accepted by A&A

Scientific paper

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

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