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We present the investigation of accretion/ejection properties of young stellar objects (YSOs), combining multi-band observations, numerical simulations, and laboratory experiments: from the Gaia-ESO Survey (GES) spectroscopic optical data of the NGC 2264 cluster (Bonito et al. 2020), to the laser experiments of stellar jets and accretion shocks young stars (e.g. Burdonov et al. 2020, 2021; Revet et al. 2021), to numerical simulations in the UV and X-ray band of accretion shocks, also in the context of next generation telescopes as Athena X-ray Observatory (Bonito et al. in preparation). The analysis of the Hα emission line profile in the GES context, provides us with information on the accretion/ejection activity of young stars, even when the nebular contribution is strong. We have developed a tool, the OHaNA method, to handle the strong nebular contribution and spectra with spurious profiles of the Hα and forbidden emission lines (e.g. [SII] and [NII] doublets). In this case, the mass accretion rate can be related to the full width at zero intensity (FWZI) of the emission line, whose measurement is more robust with respect to any value derived from the peak (e.g. Hα10%) possibly altered by the nebular contribution. The laser experiments of jets and accretion shocks in YSOs will be discussed, focusing on the effect of the local absorption on the detectability of their emission and on the role of the magnetic field on the collimation of jets. For the high energy emission, we will present the new simulations comparing the UV and X-ray shock emission from the models and the observations, taking into account also the local absorption effect and investigating the detectability of the Doppler shift in the line profiles. Future perspectives with next generation instruments, as the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) and the implication on the study of young stellar objects and their variability will be also discussed.