Abstract
In the previous chapter, the idealized case of the spherically symmetric collapsing protostar was discussed. However it was clear that observations of most protostars are not consistent with such a simple model, and additional effects must be included. This chapter considers the effects of rotation. The angular momentum problem was introduced in Chap. 1: even the relatively small-scale molecular cloud cores have far too much angular momentum to be able to collapse to stellar dimensions.
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