  We fit an isothermal oscillatory density model to the disk of HD 163296 in
which planets have presumably already formed and they are orbiting at least
within the four observed dark gaps. This 156 AU large axisymmetric disk shows
various physical properties comparable to those of AS 209, HL Tau, and TW Hya
that we have modeled previously; but it compares best to AS 209. The disks of
HD 163296 and AS 209 are comparable in size and they share similar values of
the power-law index $k\approx 0$ (a radial density profile of the form
$\rho(R)\propto R^{-1}$), the rotational parameter $\beta_0$ (to within a
factor of 3); a relatively small inner core radius (although this parameter for
HD 163296 is exceptionally small, $R_1\simeq 0.15$ AU, presumably due to
unresolved planets in the inner 50 AU); the scale length $R_0$ and the Jeans
gravitational frequency $\Omega_J$ (to within factors of 1.4); the equation of
state ($c_0^2/\rho_0$) and the central density $\rho_0$ (to within factors of
2); and the core angular velocity $\Omega_0$ (to within a factor of 4.5). In
the end, we compare all six nebular disks that we have modeled so far.
