  The astropause (heliopause for the Sun) is the tangential discontinuity
separating the stellar wind from the interstellar plasma. The global shape of
the heliopause is a matter of debates. Two types of the shape are under
discussion: comet-like and tube-like. In the second type the two-jets oriented
toward the stellar rotation axis are formed by the action of azimuthal
component of the stellar magnetic field. We explore a simplified global
astrosphere in which: (1) the surrounding and moving with respect to the star
circumstellar medium is fully ionized, (2) the interstellar magnetic field is
neglected, (3) the radial component of the stellar magnetic field is neglected
as compared with the azimuthal component, (4) the stellar wind outflow is
spherically symmetric and supersonic. We present the results of numerical 3D
MHD modelling and explore how the global structure depends on the gas-dynamic
Mach number of the interstellar flow, $M_\infty$, and the Alfvenic Mach number
in the stellar wind. It is shown that the astropause has a tube-like shape for
small values of $M_\infty$. The wings of the tube are distorted toward the tail
as larger as larger the Mach number is. The new (to our knowledge) result is
the reverse interstellar flow in the vicinity of the astropause in the tail.
The larger the interstellar Mach number is the narrower the reverse flow is. At
some values of the Mach number the stellar wind overcomes the reverse
interstellar flow and moves out in downwind. In this regime the astropause
changes its topology from tube-like to sheet-like.
