Examination of the intensity changes in five outer coronal ''looplike'' transients observed by the Skylab coronagraph shows general tendencies (1) greatest concentration of material at the flanks rather than at the tops of the bright loops that characterize these transients, (2) presence of a large region of depleted density within these loops, and (3) developement of bright legs that contain most of the material in the transient and that display very little lateral motion as the top of the bright loop moves radially outward through the outer corona. These properties of looplike coronal transients provide useful constraints on theoretical models of this phenomenon. In particular, direct comparison of the observed density distributions with those predicted by models of compressional waves initiated by an impulsive energy release in the low corona are a necessary test of these models. These models predict a maximum enhancement at the top of the loop, rather than at the flanks and ''legs'' that move laterally with a significant fraction of the propagation speed of the loop top, in conflict with the observed tendencies. If the observed loops are taken to have the geometry assumed in the compressive wave models (''toroidal symmetry'' about a rotation axis passing through the center of the sun), the predicted density enhancements are several times larger than those inferred from the observations. Agreement cannot be achieved without use of a geometry which conflicts with that used for the model calculations.