Origin of X-ray emission from intermediate-mass pre-main-sequence stars

Determine the physical origin of X-ray emission from intermediate-mass pre-main-sequence stars, distinguishing among wind-driven shocks, magnetic activity intrinsic to Herbig Ae/Be stars, and unresolved active companions.

Background

The paper investigates whether X-ray emission is associated with angular-momentum loss in intermediate-mass pre-main-sequence stars in Trumpler 14. Unlike low-mass pre-main-sequence stars, these stars are not generally expected to possess strong surface magnetic fields once on the main sequence, so their X-rays may arise from several competing mechanisms.

The unresolved origin of the X-rays limits the interpretation of the observed tendency for X-ray-detected objects to rotate more slowly. Establishing whether the emission traces intrinsic magnetic activity, wind shocks, or unresolved companions is therefore necessary to determine whether X-ray-related magnetic braking contributes to the formation of slow rotators.