  The detection of the pulsed $\sim 1 $~TeV gamma-ray emission from the Crab
pulsar reported by MAGIC and VERITAS collaborations demands a substantial
revision of existing models of particle acceleration in the pulsar
magnetosphere. In this regard model independent restrictions on the possible
production site of the VHE photons become an important issue. In this paper, we
consider limitations imposed by the process of conversion of VHE gamma rays
into $e^{\pm}$ pairs in the magnetic field of the pulsar magnetosphere. Photons
with energies exceeding 1~TeV are effectively absorbed even at large distances
from the surface of the neutron star. Our calculations of magnetic absorption
in the force-free magnetosphere show that the twisting of the magnetic field
due to the pulsar rotation makes the magnetosphere more transparent compared to
the dipole magnetosphere. The gamma-ray absorption appears stronger for photons
emitted in the direction of rotation than in the opposite direction. There is a
small angular cone inside which the magnetosphere is relatively transparent and
photons with energy $1.5$~TeV can escape from distances beyond $0.1$~light
cylinder radius ($R_{\rm{lc}}$). The emission surface from where photons can be
emitted in the observer's direction further restricts the sites of VHE
gamma-ray production. For the observation angle $57^{\circ}$ relative to the
Crab pulsar axis of rotation and the orthogonal rotation, the emission surface
in the open field line region is located as close as $0.4\,R_{\rm{lc}}$ from
the stellar surface for a dipole magnetic field, and $0.1\,R_{\rm{lc}}$ for a
force-free magnetic field.
