We present the results of a 140 ks XMM-Newton observation of the B2 star Ï Oph A. The star has exhibited strong X-ray variability: a cusp-shaped increase of rate, similar to that which we partially observed in 2013, and a bright flare. These events are separated in time by about 104 ks, which likely correspond to the rotational period of the star (1.2 days). Time resolved spectroscopy of the X-ray spectra shows that the first event is caused by an increase of the plasma emission measure, while the second increase of rate is a major flare with temperatures in excess of 60 MK (kT â¼ 5 keV). From the analysis of its rise, we infer a magnetic field of â¥300 G and a size of the flaring region of â¼ 1.4 - 1.9 Ã 1011cm, which corresponds to â¼25%-30% of the stellar radius. We speculate that either an intrinsic magnetism that produces a hot spot on its surface or an unknown low mass companion are the source of such X-rays and variability. A hot spot of magnetic origin should be a stable structure over a time span of â¥2.5 yr, and suggests an overall large scale dipolar magnetic field that produces an extended feature on the stellar surface. In the second scenario, a low mass unknown companion is the emitter of X-rays and it should orbit extremely close to the surface of the primary in a locked spin-orbit configuration, almost on the verge of collapsing onto the primary. As such, the X-ray activity of the secondary star would be enhanced by its young age, and the tight orbit as in RS Cvn systems. In both cases Ï Oph would constitute an extreme system that is worthy of further investigation.
|Numero di pagine||10|
|Rivista||ASTRONOMY & ASTROPHYSICS|
|Stato di pubblicazione||Published - 2017|
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