Jets and outflows from YSO and AGNs affect their environment, and, thus, the formation process of the objects that are launching them. Numerous studies investigate effects of such feedback mechanisms in star and planet formation and galaxy formation. However, a quantitative investigation of how much mass, momentum, or energy from the infall is actually recycled into a high-speed outflow needs to resolve the innermost jet-launching region and to model the physical process of launching directly. According to the current understanding, accretion and ejection are related to each other. One efficient way to remove angular momentum from a disk is to connect it to a magnetized outflow. In this talk, I will present the recent studies of the detailed physics of accretion- ejection structure in the inner part of the disk focusing on launching process of an outflow from a magnetically diffusive accretion disk The main question we address is which kind of disks launch jets and which kind of disks do not? in addition, I will talk about the observed non-axisymmetric structures in the disk-jet structure by extending the model to 3 dimensions and including the companion in the setup.