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#LyX 2.4 created this file. For more info see https://www.lyx.org/
\lyxformat 620
\begin_document
\begin_header
\save_transient_properties true
\origin /systemlyxdir/examples/Articles/
\textclass aa
\use_default_options true
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\language english
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\secnumdepth 3
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\end_header
\begin_body
\begin_layout Title
\begin_inset Note Note
status open
\begin_layout Plain Layout
\family roman
\series medium
\size normal
This is an example \SpecialChar LyX
file for articles to be submitted to the Journal of Astronomy & Astrophysics (A&A).
How to install the A&A \SpecialChar LaTeX
class to your \SpecialChar LaTeX
system is explained in
\begin_inset Flex URL
status open
\begin_layout Plain Layout
https://wiki.lyx.org/Layouts/Astronomy-Astrophysics
\end_layout
\end_inset
.
\begin_inset Newline newline
\end_inset
Depending on the submission state and the abstract layout,
you need to use different document class options that are listed in the aa manual.
\family default
\begin_inset Newline newline
\end_inset
\family roman
\series default
Note:
\series medium
If you use accented characters in your document,
you must use the predefined document class option
\series default
latin9
\series medium
in the document settings.
\end_layout
\end_inset
\end_layout
\begin_layout Title
Hydrodynamics of giant planet formation
\end_layout
\begin_layout Subtitle
I.
Overviewing the
\begin_inset Formula $\kappa$
\end_inset
-mechanism
\end_layout
\begin_layout Author
G.
Wuchterl
\begin_inset Flex institutemark
status open
\begin_layout Plain Layout
1
\end_layout
\end_inset
\begin_inset ERT
status collapsed
\begin_layout Plain Layout
\backslash
and
\end_layout
\end_inset
C.
Ptolemy
\begin_inset Flex institutemark
status collapsed
\begin_layout Plain Layout
2
\end_layout
\end_inset
\begin_inset ERT
status collapsed
\begin_layout Plain Layout
\backslash
fnmsep
\end_layout
\end_inset
\begin_inset Foot
status collapsed
\begin_layout Plain Layout
Just to show the usage of the elements in the author field
\end_layout
\end_inset
\begin_inset Note Note
status collapsed
\begin_layout Plain Layout
\backslash
fnmsep is only needed for more than one consecutive notes/marks
\end_layout
\end_inset
\end_layout
\begin_layout Offprint
G.
Wuchterl
\end_layout
\begin_layout Address
Institute for Astronomy (IfA),
University of Vienna,
Türkenschanzstrasse 17,
A-1180 Vienna
\begin_inset Newline newline
\end_inset
\begin_inset Flex Email
status open
\begin_layout Plain Layout
wuchterl@amok.ast.univie.ac.at
\end_layout
\end_inset
\begin_inset ERT
status collapsed
\begin_layout Plain Layout
\backslash
and
\end_layout
\end_inset
University of Alexandria,
Department of Geography,
...
\begin_inset Newline newline
\end_inset
\begin_inset Flex Email
status collapsed
\begin_layout Plain Layout
c.ptolemy@hipparch.uheaven.space
\end_layout
\end_inset
\begin_inset Foot
status collapsed
\begin_layout Plain Layout
The university of heaven temporarily does not accept e-mails
\end_layout
\end_inset
\end_layout
\begin_layout Date
Received September 15,
1996;
accepted March 16,
1997
\end_layout
\begin_layout Abstract (unstructured)
To investigate the physical nature of the `nuc\SpecialChar softhyphen
leated instability' of proto 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 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
\begin_inset Formula $-14\leq\lg\rho/[\mathrm{g}\,\mathrm{cm}^{-3}]\leq0$
\end_inset
,
\begin_inset Formula $8.8\leq\lg e/[\mathrm{erg}\,\mathrm{g}^{-1}]\leq17.7$
\end_inset
.
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
\begin_inset Formula $\rho$
\end_inset
,
temperature
\begin_inset Formula $T$
\end_inset
or specific internal energy
\begin_inset Formula $e$
\end_inset
.
Regions of instability in the
\begin_inset Formula $(\rho,e)$
\end_inset
-plane are described and related to the underlying microphysical processes.
Vibrational instability is found to be a common phenomenon at temperatures lower than the second He ionisation zone.
The
\begin_inset Formula $\kappa$
\end_inset
-mechanism is widespread under `cool' conditions.
\begin_inset Note Note
status open
\begin_layout Plain Layout
Citations are not allowed in A&A abstracts.
\end_layout
\end_inset
\begin_inset Note Note
status open
\begin_layout Plain Layout
This is the unstructured abstract type,
an example for the structured abstract is in the
\family sans
aa.lyx
\family default
template file that comes with \SpecialChar LyX
.
\end_layout
\end_inset
\end_layout
\begin_layout Keywords
giant planet formation –
\begin_inset Formula $\kappa$
\end_inset
-mechanism – stability of gas spheres
\end_layout
\begin_layout Section
Introduction
\end_layout
\begin_layout Standard
In the
\emph on
nucleated instability
\emph default
(also called core instability) hypothesis of giant planet formation,
a critical mass for static core envelope protoplanets has been found.
Mizuno (
\begin_inset CommandInset citation
LatexCommand cite
key "Eisenstein2005"
literal "true"
\end_inset
) determined the critical mass of the core to be about
\begin_inset Formula $12\,M_{\oplus}$
\end_inset
(
\begin_inset Formula $M_{\oplus}=5.975\,10^{27}\,\mathrm{g}$
\end_inset
is the Earth mass),
which is independent of the outer boundary conditions and therefore independent of the location in the solar nebula.
This critical value for the core mass corresponds closely to the cores of today's giant planets.
\end_layout
\begin_layout Standard
Although no hydrodynamical study has been available many workers conjectured that a collapse or rapid contraction will ensue after accumulating the critical mass.
The main motivation for this article is to investigate the stability of the static envelope at the critical mass.
With this aim the local,
linear stability of static radiative gas spheres is investigated on the basis of Baker's (
\begin_inset CommandInset citation
LatexCommand cite
key "Abernethy2003"
literal "true"
\end_inset
) standard one-zone model.
\end_layout
\begin_layout Standard
Phenomena similar to the ones described above for giant planet formation have been found in hydrodynamical models concerning star formation where protostellar cores explode (Tscharnuter
\begin_inset CommandInset citation
LatexCommand cite
key "Cotton1999"
literal "true"
\end_inset
,
Balluch
\begin_inset CommandInset citation
LatexCommand cite
key "Mena2000"
literal "true"
\end_inset
),
whereas earlier studies found quasi-steady collapse flows.
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
Baker's standard one-zone model
\end_layout
\begin_layout Standard
\begin_inset Float figure
placement document
alignment document
wide true
sideways false
status open
\begin_layout Plain Layout
\begin_inset Caption Standard
\begin_layout Plain Layout
\begin_inset CommandInset label
LatexCommand label
name "fig:FigGam"
\end_inset
Adiabatic exponent
\begin_inset Formula $\Gamma_{1}$
\end_inset
.
\begin_inset Formula $\Gamma_{1}$
\end_inset
is plotted as a function of
\begin_inset Formula $\lg$
\end_inset
internal energy
\begin_inset Formula $[\mathrm{erg}\,\mathrm{g}^{-1}]$
\end_inset
and
\begin_inset Formula $\lg$
\end_inset
density
\begin_inset Formula $[\mathrm{g}\,\mathrm{cm}^{-3}]$
\end_inset
\end_layout
\end_inset
\end_layout
\end_inset
In this section the one-zone model of Baker (
\begin_inset CommandInset citation
LatexCommand cite
key "Abernethy2003"
literal "true"
\end_inset
),
originally used to study the Cepheïd pulsation mechanism,
will be briefly reviewed.
The resulting stability criteria will be rewritten in terms of local state variables,
local timescales and constitutive relations.
\end_layout
\begin_layout Standard
Baker (
\begin_inset CommandInset citation
LatexCommand cite
key "Abernethy2003"
literal "true"
\end_inset
) investigates the stability of thin layers in self-gravitating,
spherical gas clouds with the following properties:
\end_layout
\begin_layout Itemize
hydrostatic equilibrium,
\end_layout
\begin_layout Itemize
thermal equilibrium,
\end_layout
\begin_layout Itemize
energy transport by grey radiation diffusion.
\end_layout
\begin_layout Standard
\noindent
For the one-zone-model Baker obtains necessary conditions for dynamical,
secular and vibrational (or pulsational) stability (Eqs.
\begin_inset space \space{}
\end_inset
(34a,
\begin_inset space \thinspace{}
\end_inset
b,
\begin_inset space \thinspace{}
\end_inset
c) in Baker
\begin_inset CommandInset citation
LatexCommand cite
key "Abernethy2003"
literal "true"
\end_inset
).
Using Baker's notation:
\end_layout
\begin_layout Standard
\align left
\begin_inset Formula
\begin{eqnarray*}
M_{r} & & \textrm{mass internal to the radius }r\\
m & & \textrm{mass of the zone}\\
r_{0} & & \textrm{unperturbed zone radius}\\
\rho_{0} & & \textrm{unperturbed density in the zone}\\
T_{0} & & \textrm{unperturbed temperature in the zone}\\
L_{r0} & & \textrm{unperturbed luminosity}\\
E_{\textrm{th}} & & \textrm{thermal energy of the zone}
\end{eqnarray*}
\end_inset
\end_layout
\begin_layout Standard
\noindent
and with the definitions of the
\emph on
local cooling time
\emph default
(see Fig.
\begin_inset space ~
\end_inset
\begin_inset CommandInset ref
LatexCommand ref
reference "fig:FigGam"
nolink "false"
\end_inset
)
\begin_inset Formula
\begin{equation}
\tau_{\mathrm{co}}=\frac{E_{\mathrm{th}}}{L_{r0}}\,,
\end{equation}
\end_inset
and the
\emph on
local free-fall time
\emph default
\begin_inset Formula
\begin{equation}
\tau_{\mathrm{ff}}=\sqrt{\frac{3\pi}{32G}\frac{4\pi r_{0}^{3}}{3M_{\mathrm{r}}}}\,,
\end{equation}
\end_inset
Baker's
\begin_inset Formula $K$
\end_inset
and
\begin_inset Formula $\sigma_{0}$
\end_inset
have the following form:
\begin_inset Formula
\begin{eqnarray}
\sigma_{0} & = & \frac{\pi}{\sqrt{8}}\frac{1}{\tau_{\mathrm{ff}}}\\
K & = & \frac{\sqrt{32}}{\pi}\frac{1}{\delta}\frac{\tau_{\mathrm{ff}}}{\tau_{\mathrm{co}}}\,;
\end{eqnarray}
\end_inset
where
\begin_inset Formula $E_{\mathrm{th}}\approx m(P_{0}/{\rho_{0}})$
\end_inset
has been used and
\begin_inset Formula
\begin{equation}
\begin{array}{l}
\delta=-\left(\frac{\partial\ln\rho}{\partial\ln T}\right)_{P}\\
e=mc^{2}
\end{array}
\end{equation}
\end_inset
is a thermodynamical quantity which is of order
\begin_inset Formula $1$
\end_inset
and equal to
\begin_inset Formula $1$
\end_inset
for nonreacting mixtures of classical perfect gases.
The physical meaning of
\begin_inset Formula $\sigma_{0}$
\end_inset
and
\begin_inset Formula $K$
\end_inset
is clearly visible in the equations above.
\begin_inset Formula $\sigma_{0}$
\end_inset
represents a frequency of the order one per free-fall time.
\begin_inset Formula $K$
\end_inset
is proportional to the ratio of the free-fall time and the cooling time.
Substituting into Baker's criteria,
using thermodynamic identities and definitions of thermodynamic quantities,
\begin_inset Formula
\[
\Gamma_{1}=\left(\frac{\partial\ln P}{\partial\ln\rho}\right)_{S}\,,\;\chi_{\rho}^{}=\left(\frac{\partial\ln P}{\partial\ln\rho}\right)_{T}\,,\;\kappa_{P}^{}=\left(\frac{\partial\ln\kappa}{\partial\ln P}\right)_{T}
\]
\end_inset
\begin_inset Formula
\[
\nabla_{\mathrm{ad}}=\left(\frac{\partial\ln T}{\partial\ln P}\right)_{S}\,,\;\chi_{T}^{}=\left(\frac{\partial\ln P}{\partial\ln T}\right)_{\rho}\,,\;\kappa_{T}^{}=\left(\frac{\partial\ln\kappa}{\partial\ln T}\right)_{T}
\]
\end_inset
one obtains,
after some pages of algebra,
the conditions for
\emph on
stability
\emph default
given below:
\begin_inset Formula
\begin{eqnarray}
\frac{\pi^{2}}{8}\frac{1}{\tau_{\mathrm{ff}}^{2}}(3\Gamma_{1}-4) & > & 0\label{ZSDynSta}\\
\frac{\pi^{2}}{\tau_{\mathrm{co}}\tau_{\mathrm{ff}}^{2}}\Gamma_{1}\nabla_{\mathrm{ad}}\left[\frac{1-3/4\chi_{\rho}^{}}{\chi_{T}^{}}(\kappa_{T}^{}-4)+\kappa_{P}^{}+1\right] & > & 0\label{ZSSecSta}\\
\frac{\pi^{2}}{4}\frac{3}{\tau_{\mathrm{co}}\tau_{\mathrm{ff}}^{2}}\Gamma_{1}^{2}\,\nabla_{\mathrm{ad}}\left[4\nabla_{\mathrm{ad}}-(\nabla_{\mathrm{ad}}\kappa_{T}^{}+\kappa_{P}^{})-\frac{4}{3\Gamma_{1}}\right] & > & 0\label{ZSVibSta}
\end{eqnarray}
\end_inset
For a physical discussion of the stability criteria see Baker (
\begin_inset CommandInset citation
LatexCommand cite
key "Abernethy2003"
literal "true"
\end_inset
) or Cox (
\begin_inset CommandInset citation
LatexCommand cite
key "Parkin2005"
literal "true"
\end_inset
).
\end_layout
\begin_layout Standard
We observe that these criteria for dynamical,
secular and vibrational stability,
respectively,
can be factorized into
\end_layout
\begin_layout Enumerate
a factor containing local timescales only,
\end_layout
\begin_layout Enumerate
a factor containing only constitutive relations and their derivatives.
\end_layout
\begin_layout Standard
The first factors,
depending on only timescales,
are positive by definition.
The signs of the left hand sides of the inequalities
\begin_inset space ~
\end_inset
(
\begin_inset CommandInset ref
LatexCommand ref
reference "ZSDynSta"
nolink "false"
\end_inset
),
(
\begin_inset CommandInset ref
LatexCommand ref
reference "ZSSecSta"
nolink "false"
\end_inset
) and (
\begin_inset CommandInset ref
LatexCommand ref
reference "ZSVibSta"
nolink "false"
\end_inset
) therefore depend exclusively on the second factors containing the constitutive relations.
Since they depend only on state variables,
the stability criteria themselves are
\emph on
functions of the thermodynamic state in the local zone
\emph default
.
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.
\begin_inset space \thinspace{}
\end_inset
g.
\begin_inset space \space{}
\end_inset
the thermodynamics and opacities (see Table
\begin_inset space ~
\end_inset
\begin_inset CommandInset ref
LatexCommand ref
reference "tab:KapSou"
nolink "false"
\end_inset
),
are specified (in practice by specifying a chemical composition) the one-zone stability can be inferred if the thermodynamic state is specified.
The zone – or in other words the layer – will be stable or unstable in whatever object it is imbedded as long as it satisfies the one-zone-model assumptions.
Only the specific growth rates (depending upon the time scales) will be different for layers in different objects.
\end_layout
\begin_layout Standard
\begin_inset Float table
placement document
alignment document
wide false
sideways false
status open
\begin_layout Plain Layout
\begin_inset Caption Standard
\begin_layout Plain Layout
\begin_inset CommandInset label
LatexCommand label
name "tab:KapSou"
\end_inset
Opacity sources
\end_layout
\end_inset
\end_layout
\begin_layout Plain Layout
\align center
\begin_inset Tabular
<lyxtabular version="3" rows="4" columns="2">
<features tabularvalignment="middle">
<column alignment="left" valignment="top" width="0pt">
<column alignment="left" valignment="top" width="0pt">
<row>
<cell alignment="center" valignment="top" topline="true" usebox="none">
\begin_inset Text
\begin_layout Plain Layout
Source
\end_layout
\end_inset
</cell>
<cell alignment="center" valignment="top" topline="true" usebox="none">
\begin_inset Text
\begin_layout Plain Layout
\begin_inset Formula $T/[\textrm{K}]$
\end_inset
\end_layout
\end_inset
</cell>
</row>
<row>
<cell alignment="center" valignment="top" topline="true" usebox="none">
\begin_inset Text
\begin_layout Plain Layout
Yorke 1979,
Yorke 1980a
\end_layout
\end_inset
</cell>
<cell alignment="center" valignment="top" topline="true" usebox="none">
\begin_inset Text
\begin_layout Plain Layout
\begin_inset Formula $\leq1700^{\textrm{a}}$
\end_inset
\end_layout
\end_inset
</cell>
</row>
<row>
<cell alignment="center" valignment="top" usebox="none">
\begin_inset Text
\begin_layout Plain Layout
Krügel 1971
\end_layout
\end_inset
</cell>
<cell alignment="center" valignment="top" usebox="none">
\begin_inset Text
\begin_layout Plain Layout
\begin_inset Formula $1700\leq T\leq5000$
\end_inset
\end_layout
\end_inset
</cell>
</row>
<row>
<cell alignment="center" valignment="top" bottomline="true" usebox="none">
\begin_inset Text
\begin_layout Plain Layout
Cox & Stewart 1969
\end_layout
\end_inset
</cell>
<cell alignment="center" valignment="top" bottomline="true" usebox="none">
\begin_inset Text
\begin_layout Plain Layout
\begin_inset Formula $5000\leq$
\end_inset
\end_layout
\end_inset
</cell>
</row>
</lyxtabular>
\end_inset
\end_layout
\begin_layout Plain Layout
\begin_inset Formula $^{\textrm{a}}$
\end_inset
This is footnote a
\end_layout
\end_inset
We will now write down the sign (and therefore stability) determining parts of the left-hand sides of the inequalities (
\begin_inset CommandInset ref
LatexCommand ref
reference "ZSDynSta"
nolink "false"
\end_inset
),
(
\begin_inset CommandInset ref
LatexCommand ref
reference "ZSSecSta"
nolink "false"
\end_inset
) and (
\begin_inset CommandInset ref
LatexCommand ref
reference "ZSVibSta"
nolink "false"
\end_inset
) and thereby obtain
\emph on
stability equations of state
\emph default
.
\end_layout
\begin_layout Standard
The sign determining part of inequality
\begin_inset space ~
\end_inset
(
\begin_inset CommandInset ref
LatexCommand ref
reference "ZSDynSta"
nolink "false"
\end_inset
) is
\begin_inset Formula $3\Gamma_{1}-4$
\end_inset
and it reduces to the criterion for dynamical stability
\begin_inset Formula
\begin{equation}
\Gamma_{1}>\frac{4}{3}\,\cdot
\end{equation}
\end_inset
Stability of the thermodynamical equilibrium demands
\begin_inset Formula
\begin{equation}
\chi_{\rho}^{}>0,\;\;c_{v}>0\,,
\end{equation}
\end_inset
and
\begin_inset Formula
\begin{equation}
\chi_{T}^{}>0
\end{equation}
\end_inset
holds for a wide range of physical situations.
With
\begin_inset Formula
\begin{eqnarray}
\Gamma_{3}-1=\frac{P}{\rho T}\frac{\chi_{T}^{}}{c_{v}} & > & 0\\
\Gamma_{1}=\chi_{\rho}^{}+\chi_{T}^{}(\Gamma_{3}-1) & > & 0\\
\nabla_{\mathrm{ad}}=\frac{\Gamma_{3}-1}{\Gamma_{1}} & > & 0
\end{eqnarray}
\end_inset
we find the sign determining terms in inequalities
\begin_inset space ~
\end_inset
(
\begin_inset CommandInset ref
LatexCommand ref
reference "ZSSecSta"
nolink "false"
\end_inset
) and (
\begin_inset CommandInset ref
LatexCommand ref
reference "ZSVibSta"
nolink "false"
\end_inset
) respectively and obtain the following form of the criteria for dynamical,
secular and vibrational
\emph on
stability
\emph default
,
respectively:
\begin_inset Formula
\begin{eqnarray}
3\Gamma_{1}-4=:S_{\mathrm{dyn}}> & 0\label{DynSta}\\
\frac{1-3/4\chi_{\rho}^{}}{\chi_{T}^{}}(\kappa_{T}^{}-4)+\kappa_{P}^{}+1=:S_{\mathrm{sec}}> & 0\label{SecSta}\\
4\nabla_{\mathrm{ad}}-(\nabla_{\mathrm{ad}}\kappa_{T}^{}+\kappa_{P}^{})-\frac{4}{3\Gamma_{1}}=:S_{\mathrm{vib}}> & 0\,.\label{VibSta}
\end{eqnarray}
\end_inset
The constitutive relations are to be evaluated for the unperturbed thermodynamic state (say
\begin_inset Formula $(\rho_{0},T_{0})$
\end_inset
) of the zone.
We see that the one-zone stability of the layer depends only on the constitutive relations
\begin_inset Formula $\Gamma_{1}$
\end_inset
,
\begin_inset Formula $\nabla_{\mathrm{ad}}$
\end_inset
,
\begin_inset Formula $\chi_{T}^{},\,\chi_{\rho}^{}$
\end_inset
,
\begin_inset Formula $\kappa_{P}^{},\,\kappa_{T}^{}$
\end_inset
.
These depend only on the unperturbed thermodynamical state of the layer.
Therefore the above relations define the one-zone-stability equations of state
\begin_inset Formula $S_{\mathrm{dyn}},\,S_{\mathrm{sec}}$
\end_inset
and
\begin_inset Formula $S_{\mathrm{vib}}$
\end_inset
.
See Fig.
\begin_inset space ~
\end_inset
\begin_inset CommandInset ref
LatexCommand ref
reference "fig:VibStabEquation"
nolink "false"
\end_inset
for a picture of
\begin_inset Formula $S_{\mathrm{vib}}$
\end_inset
.
Regions of secular instability are listed in Table
\begin_inset space ~
\end_inset
1.
\end_layout
\begin_layout Standard
\begin_inset Float figure
placement document
alignment document
wide false
sideways false
status open
\begin_layout Plain Layout
\begin_inset Caption Standard
\begin_layout Plain Layout
\begin_inset CommandInset label
LatexCommand label
name "fig:VibStabEquation"
\end_inset
Vibrational stability equation of state
\begin_inset Formula $S_{\mathrm{vib}}(\lg e,\lg\rho)$
\end_inset
.
\begin_inset Formula $>0$
\end_inset
means vibrational stability
\end_layout
\end_inset
\end_layout
\end_inset
\end_layout
\begin_layout Section
Conclusions
\end_layout
\begin_layout Enumerate
The conditions for the stability of static,
radiative layers in gas spheres,
as described by Baker's (
\begin_inset CommandInset citation
LatexCommand cite
key "Abernethy2003"
literal "true"
\end_inset
) standard one-zone model,
can be expressed as stability equations of state.
These stability equations of state depend only on the local thermodynamic state of the layer.
\end_layout
\begin_layout Enumerate
If the constitutive relations – equations of state and Rosseland mean opacities – are specified,
the stability equations of state can be evaluated without specifying properties of the layer.
\end_layout
\begin_layout Enumerate
For solar composition gas the
\begin_inset Formula $\kappa$
\end_inset
-mechanism is working in the regions of the ice and dust features in the opacities,
the
\begin_inset Formula $\mathrm{H}_{2}$
\end_inset
dissociation and the combined H,
first He ionization zone,
as indicated by vibrational instability.
These regions of instability are much larger in extent and degree of instability than the second He ionization zone that drives the Cepheïd pulsations.
\end_layout
\begin_layout Acknowledgments
Part of this work was supported by the German
\emph on
Deut\SpecialChar softhyphen
sche For\SpecialChar softhyphen
schungs\SpecialChar softhyphen
ge\SpecialChar softhyphen
mein\SpecialChar softhyphen
schaft,
DFG
\emph default
project number Ts
\begin_inset space ~
\end_inset
17/2–1.
\end_layout
\begin_layout Standard
\begin_inset CommandInset bibtex
LatexCommand bibtex
btprint "btPrintAll"
bibfiles "../biblioExample"
options "aa"
\end_inset
\begin_inset Note Note
status open
\begin_layout Plain Layout
\series bold
Note:
\series default
If you cannot see the bibliography in the output,
assure that you have given the full path to the Bib\SpecialChar TeX
style file
\family sans
aa.bst
\family default
that is part of the A&A \SpecialChar LaTeX
-package.
\end_layout
\end_inset
\end_layout
\end_body
\end_document
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