  We present two simple analytical methods for computing the gravity wave
contribution to the cosmic background radiation (CBR) anisotropy in
inflationary models; one method uses a time-dependent transfer function, the
other method uses an approximate gravity-wave mode function which is a simple
combination of the lowest order spherical Bessel functions. We compare the CBR
anisotropy tensor multipole spectrum computed using our methods with the
previous result of the highly accurate numerical method, the ``Boltzmann''
method. Our time-dependent transfer function is more accurate than the
time-independent transfer function found by Turner, White, and Lidsey; however,
we find that the transfer function method is only good for $l \la 120$. Using
our approximate gravity-wave mode function, we obtain much better accuracy; the
tensor multipole spectrum we find differs by less than 2\% for $l \la 50$, less
than 10\% for $l \la 120$, and less than 20\% for $l \leq 300$ from the
``Boltzmann'' result. Our approximate graviton mode function should be quite
useful in studying tensor perturbations from inflationary models.
