= Solution
In a static spherical star, <hydrostatic equilibrium> and the <Poisson equation> give
$$
\boxed{\frac{dp}{dr}=-\rho g,
\qquad
g=\frac{d\Phi}{dr}=\frac{Gm(r)}{r^2},
\qquad
\frac{dm}{dr}=4\pi r^2\rho},
$$
or equivalently $r^{-2}d(r^2g)/dr=4\pi G\rho$.
Let $\boldsymbol\xi$ be the fluid <displacement field>, so the velocity perturbation is $\delta\mathbf u=\partial_t\boldsymbol\xi$. Linearizing the ideal-fluid momentum equation about the static state and cancelling the background hydrostatic terms gives
$$
\boxed{\rho\frac{\partial^2\boldsymbol\xi}{\partial t^2}
=-\rho\nabla\delta\Phi-\delta\rho\nabla\Phi-\nabla\delta p}.
$$
Conservation of mass says that the Lagrangian density perturbation is $\Delta_L\rho=-\rho\nabla\cdot\boldsymbol\xi$. The relation between <Eulerian and Lagrangian fluid perturbations> and adiabatic compression gives, with $\Delta=\nabla\cdot\boldsymbol\xi$,
$$
\boxed{\delta\rho=-\rho\Delta-\boldsymbol\xi\cdot\nabla\rho,
\qquad
\delta p=-\gamma p\Delta-\boldsymbol\xi\cdot\nabla p},
$$
while linearized self-gravity gives $\boxed{\nabla^2\delta\Phi=4\pi G\delta\rho}$.
For the stated <spherical harmonic> displacement, the radial divergence is $r^{-2}d(r^2\widetilde\xi_r)/dr$, while $\nabla\widetilde\xi_h$ is radial and orthogonal to the angular gradient of $Y_l^m$. Hence
$$
\boxed{\widetilde\Delta
=\frac1{r^2}\frac d{dr}(r^2\widetilde\xi_r)
-k_h^2\widetilde\xi_h,
\qquad
k_h^2=\frac{l(l+1)}{r^2}}.
$$
Equating the radial and horizontal coefficients of $Y_l^m$ and $\nabla Y_l^m$, and applying the separated <Laplacian in spherical coordinates> to $\widetilde{\delta\Phi}(r)Y_l^m$, gives
$$
\boxed{-\rho\omega^2\widetilde\xi_r
=-\rho\frac{d\widetilde{\delta\Phi}}{dr}
-g\widetilde{\delta\rho}
-\frac{d\widetilde{\delta p}}{dr}},
$$
$$
\boxed{-\rho\omega^2\widetilde\xi_h
=-\rho\widetilde{\delta\Phi}-\widetilde{\delta p}},
$$
$$
\boxed{\widetilde{\delta\rho}
=-\rho\widetilde\Delta-\widetilde\xi_r\frac{d\rho}{dr},
\qquad
\widetilde{\delta p}
=-\gamma p\widetilde\Delta-\widetilde\xi_r\frac{dp}{dr}},
$$
$$
\boxed{\frac1{r^2}\frac d{dr}
\left(r^2\frac{d\widetilde{\delta\Phi}}{dr}\right)
-k_h^2\widetilde{\delta\Phi}=4\pi G\widetilde{\delta\rho}}.
$$
Define the <stellar buoyancy frequency> by
$$
\boxed{N^2=g\left(
\frac1{\gamma p}\frac{dp}{dr}
-\frac1\rho\frac{d\rho}{dr}\right)}.
$$
Eliminating $\widetilde\Delta$ between the density and pressure perturbations gives
$$
\widetilde{\delta\rho}
=\frac{\rho}{\gamma p}\widetilde{\delta p}
+\frac{\rho N^2}{g}\widetilde\xi_r.
$$
Substitution in the radial equation, followed by use of $dp/dr=-\rho g$, yields
$$
\boxed{(\omega^2-N^2)\widetilde\xi_r
=\frac d{dr}\left(
\widetilde{\delta\Phi}+\frac{\widetilde{\delta p}}\rho\right)
-\frac{N^2\widetilde{\delta p}}{g\rho}}.
$$
Regular spherical profiles near the center have $\rho=\rho_c+O(r^2)$ and $p=p_c+O(r^2)$, while $m(r)=4\pi\rho_cr^3/3+O(r^5)$ and hence $g=O(r)$. Both logarithmic gradients in the definition of $N^2$ are $O(r)$, so $N^2=Ar^2+O(r^4)$. A Sun-like radiative central stratification is stable, making $A>0$.
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