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We conduct forward-modeling analysis based on our 2.5 dimensionalmagnetohydrodynamics (MHD) simulation of magnetic flux rope (MFR) formation anderuption driven by photospheric converging motion. The current sheet (CS)evolution during the MFR formation and eruption process in our MHD simulationcan be divided into four stages. The current sheet (CS) evolution during theMFR formation and eruption process in our MHD simulation can be divided intofour stages. The first stage shows the CS forming and gradually lengthening.Resistive instabilities that disrupt the CS mark the beginning of the secondstage. Magnetic islands disappear in the third stage and reappear in the fourthstage. Synthetic images and light curves of the seven Solar DynamicsObservatory/Atmospheric Imaging Assembly (AIA) channels, i.e., 9.4 nm, 13.1 nm,17.1 nm, 19.3 nm, 21.1 nm, 30.4 nm, and 33.5 nm, and the 3-25 keV thermal X-rayare obtained with forward-modeling analysis. The loop-top source and thecoronal sources of the soft X-ray are reproduced in forward modeling. The lightcurves of the seven SDO/AIA channels start to rise once resistive instabilitiesdevelop. The light curve of the 3-25 keV thermal X-ray starts to go up when thereconnection rate reaches one of its peaks. Quasiperiodic pulsations (QPPs)appear twice in the SDO/AIA 17.1 nm, 21.1 nm, and 30.4 nm channels,corresponding to the period of chaotic (re)appearance and CS-guideddisplacements of the magnetic islands. QPPs appear once in the SDO/AIA 9.4 nmand 33.5 nm channels after the disruption of the CS by resistive instabilitiesand in the 19.3 nm channel when the chaotic motion of the magnetic islandsreappears.

Forward Modeling of SDO/AIA and X-Ray Emission from a Simulated Flux Rope Ejection