The most massive evolved stars (above 50 M⊙) undergo a phase of extreme mass loss, in which their evolution is reversed from a redward to a blueward motion in the H-R diagram. In this phase, the stars are known as Luminous Blue Variables and they are located in the H-R diagram close to the Humphreys-Davidson limit. It is far from understood what causes the strong mass loss or what triggers the so-called giant eruptions, active events in which in a short time a large amount of mass is ejected. Here I present results from a larger project, devoted to better understand LBVs through studying the LBV nebulae. These nebulae are formed as a consequence of the strong mass loss. The analysis concentrates on the morphology and kinematics of these nebulae. Of special concern is the frequently observed bipolar nature of the LBV nebulae. Bipolarity seems to be a general feature and strongly constrains models of the LBV phase, especially of the formation of the nebulae. In addition, we find outflows from LBV nebulae, the first evidence for ongoing instabilities in the nebulae.