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+#LyX 1.6.0 created this file. For more info see http://www.lyx.org/
+\lyxformat 345
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\begin_layout Title
Hydrodynamics of giant planet formation
\end_layout
\begin_layout Author
G.
- Wuchterl
+ Wuchterl
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-
+ C.
+ Ptolemy
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+2
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-C.
- Ptolemy
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\begin_layout Offprint
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+wuchterl@amok.ast.univie.ac.at
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-email{wuchterl@amok.ast.univie.ac.at}
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-and
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-email{c.ptolemy@hipparch.uheaven.space}
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\begin_layout Abstract
To investigate the physical nature of the `nuc\SpecialChar \-
leated instability' of proto
- giant planets (Mizuno
-\begin_inset CommandInset citation
-LatexCommand cite
-key "mizuno"
-
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-
-), the stability of layers in static, radiative gas spheres is analysed
- on the basis of Baker's
-\begin_inset CommandInset citation
-LatexCommand cite
-key "baker"
-
-\end_inset
-
- standard one-zone model.
+ giant planets, the stability of layers in static, radiative gas spheres
+ is analysed on the basis of Baker's standard one-zone model.
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
\end_inset
-mechanism is widespread under `cool' conditions.
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-\backslash
-keywords{giant planet formation --
-\backslash
-(
-\backslash
-kappa
-\backslash
-)-mechanism -- stability of gas spheres }
\end_layout
+\begin_layout Keywords
+giant planet formation --
+\begin_inset Formula $\kappa$
\end_inset
-
+-mechanism -- stability of gas spheres
\end_layout
\begin_layout Section
In the
\emph on
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.
\end_inset
), whereas earlier studies found quasi-steady collapse flows.
- The similarities in the (micro)physics, i.e., constitutive relations of protostel
-lar cores and protogiant planets serve as a further motivation for this
- study.
+ The similarities in the (micro)physics, i.
+\begin_inset space \thinspace{}
+\end_inset
+
+g.
+\begin_inset space \space{}
+\end_inset
+
+constitutive relations of protostellar cores and protogiant planets serve
+ as a further motivation for this study.
\end_layout
\begin_layout Section
\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
and with the definitions of the
\emph on
local cooling time
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(see Fig.
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one obtains, after some pages of algebra, the conditions for
\emph on
stability
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given below:
\begin_inset Formula \begin{eqnarray}
.
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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+ Once the microphysics, i.
+\begin_inset space \thinspace{}
+\end_inset
+g.
+\begin_inset space \space{}
\end_inset
the thermodynamics and opacities (see Table
ge\SpecialChar \-
mein\SpecialChar \-
schaft, DFG
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+ project number Ts
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-\begin_layout Plain Layout
+17/2--1.
+\end_layout
+\begin_layout Standard
+\begin_inset Note Note
+status open
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+\begin_layout Plain Layout
+You can alternatively use BibTeX.
+ You must then use the BibTeX style
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+ that is part of the A&A LaTeX-package.
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\end_inset
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- project number Ts
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-17/2--1.
-
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\begin_layout Bibliography
Baker, N.
1966, in Stellar Evolution, ed.
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R.
projects / lyx.git / blobdiff