We interpret the observed X-ray morphology of the central part of the Crab Nebula ( torus +  jets ) in terms of the standard theory by Kennel and Coroniti ( 1984 ) .
The only new element is the inclusion of anisotropy in the energy flux from the pulsar in the theory .
In the standard theory of relativistic winds , the Lorentz factor of the particles in front of the shock that terminates the pulsar relativistic wind depends on the polar angle as \gamma = \gamma _ { 0 } + \gamma _ { m } \sin ^ { 2 } \theta , where \gamma _ { 0 } \sim 200 and \gamma _ { m } \sim 4.5 \times 10 ^ { 6 } .
The plasma flow in the wind is isotropic .
After the passage of the pulsar wind through the shock , the flow becomes subsonic with a roughly constant ( over the plerion volume ) pressure P = { 1 \over 3 } n \epsilon , where n is the plasma particle density and \epsilon is the mean particle energy .
Since \epsilon \sim \gamma mc ^ { 2 } , a low-density region filled with the most energetic electrons is formed near the equator .
A bright torus of synchrotron radiation develops here .
Jet-like regions are formed along the pulsar rotation axis , where the particle density is almost four orders of magnitude higher than that in the equatorial plane , because the particle energy there is four orders of magnitude lower .
The energy of these particles is too low to produce detectable synchrotron radiation .
However , these quasi-jets become comparable in brightness to the torus if additional particle acceleration takes place in the plerion .
We also present the results of our study of the hydrodynamic interaction between an anisotropic wind and the interstellar medium .
We compare the calculated and observed distributions of the volume intensity of X-ray radiation .

Key words : plasma astrophysics , hydrodynamics and shock waves .