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The young O9.5 V spectroscopic binary Theta 2 Ori A shows moderately hardX-ray emission and relatively narrow X-ray lines, suggesting that it may be aMagnetically Confined Wind Shock (MCWS) source, similar to its more massiveanalogue Theta 1 Ori C. X-ray flares occurring near periastron led to thesuggestion that the flares are produced via magnetic reconnection asmagnetospheres on both components of the Theta 2 Ori A binary interact atclosest approach.  We use a series of high-resolution spectropolarimetric observations of Theta2 Ori A to place an upper limit on the magnetic field strength of 135 G (95%credible region). Such a weak dipole field would not produce magneticconfinement, or a large magnetosphere. A sub-pixel analysis of the Chandra ACISimages of Theta 2 Ori A obtained during quiescence and flaring show that thehard, flaring X-rays are offset from the soft, quiescent emission by 0.4arcsec. If the soft emission is associated with the A1/A2 spectroscopic binary,the offset and position angle of the hard, flaring source place it at thelocation of the intermediate-mass A3 companion, discovered via speckleinterferometry. The spectropolarimetric and X-ray results taken together pointto the A3 companion, not the massive A1/A2 binary, as the source of hard,flaring X-ray emission.  We also discuss a similar analysis performed for the magnetic Bp star SigmaOri E. We find a similar origin for its X-ray flaring.

Solving the Puzzle of the Massive Star System Theta 2 Orionis A