The recent discovery of switchbacks, localized magnetic deflections in the solar wind, by Parker Solar Probe has spurred investigations into their origin. One prominent theory suggests their formation in the lower corona through a process of magnetic reconnection akin to solar jet formation. To explore this hypothesis, I will present parametric simulations using a three-dimensional numerical magnetohydrodynamic (MHD) model of solar-jet-like events. Within the MHD framework, I examine the influence of varying atmospheric plasma beta on the dynamics of solar-like jets.

Across simulations representing distinct solar atmospheres, similar temporal energy variations were observed. Notably, magnetic energy injection exhibited consistency, with a partial conversion into kinetic energy during jet generation. The parametric study validates this model for initial plasma beta values ranging from 10^-3 to 1, corresponding to different magnetic environments within the solar atmosphere. Common structural characteristics in solar jets, including a dense bulk flow of plasma and a magnetic wavefront propagating at an Alfvénic speed in the atmosphere, were identified. However, the propagation ratio of these structures varied among simulations, revealing intricate influences of atmospheric stratification on jet dynamics.

Overall these simulations unveiled the propagation of magnetic deflections thanks to jet-like events, shedding light on the possible formation processes of switchbacks.