SIMBAD references

The X-ray properties of twenty ∼1 Myr old O, B, and A stars of the Orion Trapezium are examined with data from the Chandra Orion Ultradeep Project (COUP). On the basis of simple theories for X-ray emission, we define two classes separated at spectral type B4: hotter stars have strong winds that may give rise to X-ray emission in small- or large-scale wind shocks, and cooler stars that should be X-ray dark due to their weaker winds and absence of outer convection zones where dynamos can generate magnetic fields. Emission by late-type magnetically active companions may be present in either class. Sixteen of the 20 stars are detected with a wide range of X-ray luminosities, logL_Xergs/s∼29-33, and X-ray efficiencies, log(L_X/L_bol)~-4 to -8. Only two stars, θ¹ Ori D (B0.5) and NU Ori (B1), show exclusively the constant soft-spectrum emission at log(L_X/L_bol)~-7 expected from the standard model involving many small shocks in an unmagnetized radiatively accelerated wind. Most of the other massive O7-B3 stars exhibit some combination of soft-spectrum wind emission, hard-spectrum flaring, and/or rotational modulation indicating large-scale inhomogeneity. Magnetic confinement of winds with large-scale shocks can be invoked to explain these phenomena. This is supported in some cases by nonthermal radio emission and/or chemical peculiarities, or direct detection of the magnetic field (θ¹ Ori C). Most of the stars in the weak-wind class exhibit X-ray flares and logL_X<31 ergs/s, consistent with magnetic activity from known or unseen low-mass companions. In most cases, the X-ray spectra can be interpreted in terms of a two-temperature plasma model with a soft component of 3-10 MK and a hard component up to 40 MK. All nondetections belong to the weak-wind class. A group of stars exhibit hybrid properties–flarelike behavior superimposed on a constant component with logL_X∼32 ergs/s–which suggest both magnetic activity and wind emission.