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Flares from the Sun and other stars are most prominently observed in the softX-ray band. Most of the radiated energy, however, is released at optical/UVwavelengths. In spite of decades of investigation, the physics of flares is notfully understood. Even less is known about the powerful flares routinelyobserved from pre-main sequence stars, which might significantly influence theevolution of circumstellar disks. Observations of the NGC2264 star formingregion were obtained in Dec. 2011, simultaneously with three telescopes,Chandra (X-rays), CoRoT (optical), and Spitzer (mIR), as part of the"Coordinated Synoptic Investigation of NGC2264" (CSI-NGC2264). Shorter Chandraand CoRoT observations were also obtained in March 2008. We analyzed thelightcurves to detect X-ray flares with an optical and/or mIR counterpart.Basic flare properties from the three datasets, such as emitted energies andpeak luminosities, were then compared to constrain the spectral energydistribution of the flaring emission and the physical conditions of theemitting regions. Flares from stars with and without circumstellar disks werealso compared to establish any difference that might be attributed to thepresence of disks. Seventy-eight X-ray flares with an optical and/or mIRcounterpart were detected. Their optical emission is found to correlate wellwith, and to be significantly larger than, the X-ray emission. The slopes ofthe correlations suggest that the difference becomes smaller for the mostpowerful flares. The mIR flare emission seems to be strongly affected by thepresence of a circumstellar disk: flares from stars with disks have a strongermIR emission with respect to stars without disks. This might be attributed tothe reprocessing of the optical (and X-ray) flare emission by the innercircumstellar disk, providing evidence for flare-induced disk heating.

A multi-wavelength view of magnetic flaring from PMS stars