Poster abstract

Shapes of disks such as protostellar and protoplanetary disks can reveal fluid flow patterns which in turn can tell us about the physics and some properties of the fluid flow. Analysis of the physics and properties thus reveal why disks can be warped or tilted. We present a model on how accretion disks can warp/tilt that depends on the mass of the compact object, the mass transfer rate, and the speed(s) of the fluid flow but does not depend on magnetic fields or radiation sources.