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The disk rotating around its pre-main sequence star exchanges both matter and angular momentum through the existence of the stellar magnetic field (here represented as been dipolar) The coupling is done in the inner part of the disk where the gas is heated and ionized by the stellar radiations. The funneling of the disk material by the magnetic field to form the accretion flows leads to the generation of the polar accretions shocks which radiate in X-ray, Schematic view a classical T Tauri star, p.179, 2016. ,
The infalling accreting material impact the star chromosphere and forms, where its ram pressure is comparable to the local thermal pressure, a shock Temperature produced by this shock are of the order of few millions of kelvins and thus a large amount of X-rays are emitted. These radiations are then reprocessed by the preshock, the postshock and the ambient environment into larger wavelengths which creates the features observed on the TTS spectra, Schematic view of an accretion shock on the stellar surface, p.183, 2016. ,