  The bright-rimmed cloud SFO 22 was observed with the 45 m telescope of
Nobeyama Radio Observatory in the ^{12}CO (J = 1-0), ^{13}CO (J = 1-0), and
C^{18}O (J = 1-0) lines, where well-developed head-tail structure and small
line widths were found. Such features were predicted by radiation-driven
implosion models, suggesting that SFO 22 may be in a quasi-stationary
equilibrium state. We compare the observed properties with those from numerical
models of a photo-evaporating cloud, which include effects of magnetic pressure
and heating due to strong far-ultraviolet (FUV) radiation from an exciting
star. The magnetic pressure may play a more important role in the density
structures of bright-rimmed clouds, than the thermal pressure that is enhanced
by the FUV radiation. The FUV radiation can heat the cloud surface to near 30
K, however, its effect is not enough to reproduce the observed density
structure of SFO 22. An initial magnetic field of 5 \mu G in our numerical
models produces the best agreement with the observations, and its direction can
affect the structures of bright-rimmed clouds.
