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In massive stars, magnetic fields are thought to confine the outflowingradiatively-driven wind, resulting in X-ray emission that is harder, morevariable and more efficient than that produced by instability-generated shocksin non-magnetic winds. Although magnetic confinement of stellar winds has beenshown to strongly modify the mass-loss and X-ray characteristics of massive OBstars, we lack a detailed understanding of the complex processes responsible.The aim of this study is to examine the relationship between magnetism, stellarwinds and X-ray emission of OB stars. In conjunction with a Chandra survey ofthe Orion Nebula Cluster, we carried out spectropolarimatric ESPaDOnSobservations to determine the magnetic properties of massive OB stars of thiscluster. We found of two new massive magnetic stars in the Orion NebulaCluster: HD 36982 and HD 37061, for which the estimated dipole polar strengthsare 1150 (+320 -200) G and 620 (+220 -170) G, respectively. However, theapparent lack of clear correlation between X-ray indicator and the presence ofa magnetic fields brings forth new challenges for understanding the processesleading to X-ray emission in massive stars.

Magnetic fields, winds and X-rays of massive stars: A spectropolarimetric survey of the Orion cluster