  We present high-resolution J-, H-, and K-band observations of the carbon star
IRC+10216. The images were reconstructed from 6 m telescope speckle
interferograms using the bispectrum speckle interferometry method. The H and K
images consist of several compact components within a 0.2" radius and a fainter
asymmetric nebula. The brightest four components are denoted with A to D in the
order of decreasing brightness. A comparison of our images gives - almost like
a movie of five frames - insight to the dynamical evolution of the inner
nebula. For instance, the separation of the two brightest components A and B
increased by almost 40% from 191 mas in 1995 to 265 mas in 1998. At the same
time, component B is fading and the components C and D become brighter. The
X-shaped bipolar structure of the nebula implies an asymmetric mass-loss
suggesting that IRC+10216 is very advanced in its AGB evolution, shortly before
turning into a protoplanetary nebula. The cometary shape of component A
suggests that the core of A is not the central star, but the southern lobe of a
bipolar structure. The position of the central star is probably at or near the
position of component B.
