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The solar atmosphere hosts many energetic events such as flares, coronal mass ejections (CMEs), jets, etc. varying in temporal, spatial, and energetics scales. When these eruptions are directed toward the Earth, not only do they produce beautiful auroras but also pose a great threat to life in several forms. One of the most accepted theories behind all these events is magnetic reconnection (MR). Reconnections are ubiquitous in astrophysical/space plasmas. It involves the conversion of stored magnetic energy into heat, kinetic energy, and particle acceleration from the reconnection site accompanied by a change in magnetic topology. Being magnetic in nature, it is then imperative to understand the role of magnetic fields, associated currents, and their dynamics in triggering these events. Again, the reconnection process in the solar atmosphere, particularly the onset mechanism and its subsequent dynamics are still intriguing in three dimensions (3Ds). Next, reconnection sites such as magnetic null point (|B|=0), and quasi-separatrix layers (location having a sharp change in magnetic connectivity) play an important role in driving these transients and dictating the pattern of reconnection. However, a reliable and routinely magnetic field measurement is not available for the Sun's atmosphere except for its photosphere and/or chromosphere. Then in order to understand these reconnection driven transients, I have performed numerical modeling of the solar atmosphere by magnetic field extrapolation method and magnetohydrodynamics (MHD) simulations, complemented with observations. In this talk, I will discuss the ONSET of the magnetic reconnection process in a variety of transients like jets and flares, highlighting the role of topologies in guiding the reconnection process in 3D, with a combined observational, and theoretical/numerical modeling approach.