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G.
Wuchterl
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and
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C.
Ptolemy
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Just to show the usage of the elements in the author field
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17, A-1180 Vienna
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email{wuchterl@amok.ast.univie.ac.at}
and
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University of Alexandria, Department of Geography, ...
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email{c.ptolemy@hipparch.uheaven.space}
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The university of heaven temporarily does not accept e-mails
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-mechanism is widespread under `cool' conditions.
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kappa
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)-mechanism -- stability of gas spheres }
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In the
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nucleated instability
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(also called core instability) hypothesis of giant planet formation, a
critical mass for static core envelope protoplanets has been found.
Mizuno (
Baker's standard one-zone model
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Adiabatic exponent
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In this section the one-zone model of Baker (
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\noindent
For the one-zone-model Baker obtains necessary conditions for dynamical,
secular and vibrational (or pulsational) stability (Eqs.
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(34a,
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b,
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c) in Baker
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and with the definitions of the
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local cooling time
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(see Fig.\SpecialChar ~
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one obtains, after some pages of algebra, the conditions for
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stability
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given below:
\begin_inset Formula \begin{eqnarray}
\frac{\pi ^{2}}{8}\frac{1}{\tau _{\mathrm{ff}}^{2}}(3\Gamma _{1}-4) & > & 0\label{ZSDynSta} \\
The one-zone stability can therefore be determined from a simple equation
of state, given for example, as a function of density and temperature.
Once the microphysics, i.e.
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the thermodynamics and opacities (see Table\SpecialChar ~
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different for layers in different objects.
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Yorke 1979, Yorke 1980a
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Krügel 1971
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Cox & Stewart 1969
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This is footnote a
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We will now write down the sign (and therefore stability) determining parts
of the left-hand sides of the inequalities (
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1.
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Vibrational stability equation of state
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Conclusions
ge\SpecialChar \-
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schaft, DFG
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project number Ts\SpecialChar ~
17/2--1.
Baker, N.
1966, in Stellar Evolution, ed.
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R.
F.
Stein,& A.