  We investigate the escape process of cosmic rays (CRs) from perpendicular
shock regions of a spherical shock propagating to a circumstellar medium with
the Parker-spiral magnetic field. The diffusive shock acceleration in
perpendicular shocks of supernova remnants (SNRs) is expected to accelerate CRs
up to PeV without upstream magnetic field amplification. Red supergiants (RSGs)
and Wolf-Rayet (WR) stars are considered as progenitors in this work. We
perform test particle simulations to investigate the escape process and
escape-limited maximum energy without magnetic field amplification in the
upstream region, where the magnetic field strength and rotation period expected
from observations of RSGs and WR stars are used. We show that particles escape
to the far upstream region while moving along the equator or poles and the
maximum energy is about $10-100~{\rm TeV}$ when SNRs propagate to free wind
regions of RSGs and WR stars. In most cases, the escape-limited maximum energy
is given by the potential difference between the equator and pole. If
progenitors are oblique rotators and SNRs are in the early phase just after the
supernova explosion, the escape-limited maximum energy is limited by the half
wavelength of the wavy current sheet. In addition, for RSGs, we show that the
luminosity of CRs accelerated in the wind region is sufficient to supply the
observed CR flux above $10~{\rm TeV}$ if a strong magnetic field strength is
sustained in most RSGs. In terms of the CR luminosity, SNRs propagating to the
free wind of WR stars can contribute to PeV CRs. As long as no magnetic field
amplification works around SNR shocks, the maximum energy is decided by the
magnetic field strength in the wind region, which depends on the rotation
period, stellar wind, and surface magnetic field of RSGs and WR stars.
Therefore, we need to observe these quantities to understand the origin of CRs.
