  The nature of the Vela X-ray "jet", recently discovered by Markwardt &
\"Ogelman (1995), is examined. It is suggested that the "jet" arises along the
interface of domelike deformations of the Rayleigh-Taylor unstable shell of the
Vela supernova remnant; thereby the "jet" is interpreted as a part of the
general shell of the remnant. The origin of deformations as well as the general
structure of the remnant are discussed in the framework of a model based on a
cavity explosion of a supernova star. It is suggested that the shell
deformations viewed at various angles appear as filamentary structures visible
throughout the Vela supernova remnant at radio, optical, and X-ray wavelengths.
A possible origin of the nebula of hard X-ray emission detected by Willmore et
al. (1992) around the Vela pulsar is proposed.
