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Accreting T Tauri stars are observed to be less luminous in X‐rays than non‐accretors, an effect that has been detected in various star‐forming regions. To explain this we have combined, for the first time, a radiative transfer code with an accretion model that considers magnetic fields extrapolated from surface magnetograms obtained from Zeeman–Doppler imaging. Such fields consist of compact magnetic regions close to the stellar surface, with extended field lines interacting with the disc. We study the propagation of coronal X‐rays through the magnetosphere and demonstrate that they are strongly absorbed by the dense gas in accretion columns. The reduction in the observed X‐ray emission depends on the field geometry, which may explain why accreting T Tauri stars show a larger scatter in their observed X‐ray luminosity compared with non‐accreting stars.

Why are accreting T Tauri stars observed to be less luminous in X‐rays than non‐accretors?