[en] The propagation and dissipation of interplanetary shock waves (IPS) generated by coronal mass ejection (CME) or corotating streams of solar flare ejecta are considered. CME shocks interact with the solar wind, resulting in shock fronts which propagate at uneven velocities in different regions. The solar wind may also dampen out the fronts at various locations so that the propagating fronts deviate from the spherical and have holes. The dissipation in the solar wind can degrade the shocks into fast MHD waves. An expression is developed for predicting the probability that a shock wave will disappear at a given distance from the sun. 21 references