\abstract{To investigate the physical nature of the `nuc\-leated instability' of
\abstract{To investigate the physical nature of the `nuc\-leated instability' of
proto giant planets, the stability of layers
proto giant planets, the stability of layers in static, radiative gas spheres is analysed on the basis of Baker's standard one-zone model.}
in static, radiative gas spheres is analysed on the basis of Baker's
standard one-zone model.}
{To investigate the physical nature of the `nuc\-leated instability' of
{To investigate the physical nature of the `nuc\-leated instability' of
proto giant planets, the stability of layers
proto giant planets, the stability of layers in static, radiative gas spheres is analysed on the basis of Baker's standard one-zone model.}
in static, radiative gas spheres is analysed on the basis of Baker's
{It is shown that stability depends only upon the equations of state, the opacities and the local thermodynamic state in the layer. Stability and instability can therefore be expressed in the form of stability equations of state which are universal for a given composition.}
standard one-zone model.}
{The stability equations of state are calculated for solar composition and are displayed in the domain $-14 \leq \lg \rho / \mathrm{[g\, cm^{-3}]} \leq 0 $, $ 8.8 \leq \lg e / \mathrm{[erg\, g^{-1}]} \leq 17.7$. These displays may be used to determine the one-zone stability of layers in stellar or planetary structure models by directly reading off the value of the stability equations for the thermodynamic state of these layers, specified by state quantities as density $\rho$, temperature $T$ or specific internal energy $e$. Regions of instability in the $(\rho,e)$-plane are described and related to the underlying microphysical processes.}
{It is shown that stability depends only upon the equations of state, the opacities and the local
{Vibrational instability is found to be a common phenomenon at temperatures lower than the second He ionisation zone. The $\kappa$-mechanism is widespread under `cool' conditions.}
thermodynamic state in the layer. Stability and instability can
therefore be expressed in the form of stability equations of state
which are universal for a given composition.}
{The stability equations of state are
calculated for solar composition and are displayed in the domain