Shock-induced magnetic reconnection in the Venusian magnetotail

Venus lacks an intrinsic magnetic field, and its induced magnetosphere differs significantly from Earth's stable dipolar magnetic field. Although magnetic reconnection was detected in the near Venusian magnetotail, the drivers and impacts of magnetic reconnection at Venus remain poorly understood. In this study, we present the global magnetohydrodynamic simulation of Venusian magnetotail reconnection. The results reproduce characteristic reconnection signatures in the Venusian magnetotail and delineate the formation of three-dimensional magnetic structures consistent with reconnection topologies. We demonstrate that reconnection is triggered by the compression of the draped interplanetary magnetic field following an interplanetary shock, a mechanism previously associated with terrestrial dynamics. We further explore the roles of velocity, density and magnetic field of the solar wind in this process. This work highlights new insights into magnetic reconnection in unmagnetized plasma environments.