@ -6,10 +6,12 @@ author:
correspond: true correspond: true
affiliation: "My City University" affiliation: "My City University"
address: "Orenomachi, Orenoshi, Orenoken, Japan" address: "Orenomachi, Orenoshi, Orenoken, Japan"
email: "one@myuni.ac.jp"
- number: 2 - number: 2
name: "Author Two" name: "Author Two"
affiliation: "My Other City University" affiliation: "My Other City University"
address: "Hokanomachi, Orenoshi, Orenoken, Japan" address: "Hokanomachi, Orenoshi, Orenoken, Japan"
email: "two@myuni.ac.jp"
email: "xxx@myuni.ac.jp" email: "xxx@myuni.ac.jp"
titleshort: "Paperlighter Example" titleshort: "Paperlighter Example"
authorshort: "Author One et.al." authorshort: "Author One et.al."
@ -19,302 +21,321 @@ linkDir:
appendix: appendix:
- appendix/1 - appendix/1
- appendix/2 - appendix/2
abstract: abstractTex:
Using \LaTeX{} to write papers is concise and convenient. However, for \abstract{To investigate the physical nature of the `nuc\-leated instability' of
writing in life, complicated \LaTeX{} style-files (e.g., elegantpaper) proto giant planets, the stability of layers
are difficult to access, or submission style-files (e.g., journal or in static, radiative gas spheres is analysed on the basis of Baker's
conference) are not free indeed. To tackle these problems and satisfy an standard one-zone model.}
elegant and straightforward scientific writing, {To investigate the physical nature of the `nuc\-leated instability' of
\textbf{paperlighter.sty}, a one-column style-file, is designed. This proto giant planets, the stability of layers
document is edited from icml2022.sty and provides a basic paper in static, radiative gas spheres is analysed on the basis of Baker's
template. Compared to icml2022.sty, paperlighter.sty contain fewer standard one-zone model.}
operations, reducing adjustment while keep graceful. {It is shown that stability depends only upon the equations of state, the opacities and the local
\textbf{\textit{Notably, the paper's main content only describes the format of icml2022.sty. We place the content to show the actual effect of paperlighter.sty.}} 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
$-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.}
{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.}
{}
keywords: giant planet formation -- $\kappa$-mechanism -- stability of gas spheres
acknowledgements:
Part of this work was supported by the German
\emph{Deut\-sche For\-schungs\-ge\-mein\-schaft, DFG\/} project
number Ts~17/2--1.
--- ---
# Introduction
# Format of the Paperlighter
In the \emph{nucleated instability\/} (also called core
Format of paperlighter is defined in this section. instability) hypothesis of giant planet
formation, a critical mass for static core envelope
## Dimensions protoplanets has been found. \citet{langley00} determined
the critical mass of the core to be about $12 \,M_\oplus$
The text of the paper has an overall width of ($M_\oplus=5.975 \times 10^{27}\,\mathrm{g}$ is the Earth mass), which
6.75\textasciitilde{}inches, and height of 9.0\textasciitilde{}inches. is independent of the outer boundary
The left margin should be 0.75\textasciitilde{}inches and the top margin conditions and therefore independent of the location in the
1.0\textasciitilde{}inch (2.54\textasciitilde{}cm). The right and bottom solar nebula. This critical value for the core mass corresponds
margins will depend on whether you print on US letter or A4 paper, but closely to the cores of today's giant planets.
all final versions must be produced for US letter size.
Although no hydrodynamical study has been available many workers
The paper body should be set in 10\textasciitilde{}point type with a conjectured that a collapse or rapid contraction will ensue
vertical spacing of 11\textasciitilde{}points. Please use Times typeface after accumulating the critical mass. The main motivation for
throughout the text. this article
is to investigate the stability of the static envelope at the
## Title critical mass. With this aim the local, linear stability of static
radiative gas spheres is investigated on the basis of Baker's
The paper title should be set in 14\textasciitilde{}point bold type and (\citeyear{mitchell80}) standard one-zone model.
centered between two horizontal rules that are 1\textasciitilde{}point
thick, with 1.0\textasciitilde{}inch between the top rule and the top Phenomena similar to the ones described above for giant planet
edge of the page. Capitalize the first letter of content words and put formation have been found in hydrodynamical models concerning
the rest of the title in lower case. star formation where protostellar cores explode
(Tscharnuter \citeyear{kearns89}, Balluch \citeyear{MachineLearningI}),
## Author Information for Submission whereas earlier studies found quasi-steady collapse flows. The
similarities in the (micro)physics, i.e., constitutive relations of
Use \verb+\lighterauthor{...}+ to specify authors and protostellar cores and protogiant planets serve as a further
\verb+\lighteraddress{...}+ to specify affiliations. (Read the TeX code motivation for this study.
used to produce this document for an example usage.) The author
information will not be printed unless \texttt{accepted} is passed as an
argument to the style file. # Baker's standard one-zone model
## Abstract \begin{figure*}
\centering
The paper abstract should begin in the left column, \caption{Adiabatic exponent $\Gamma_1$.
0.4\textasciitilde{}inches below the final address. The heading $\Gamma_1$ is plotted as a function of
`Abstract’ should be centered, bold, and in 11\textasciitilde{}point $\lg$ internal energy $\mathrm{[erg\,g^{-1}]}$ and $\lg$
type. The abstract body should use 10\textasciitilde{}point type, with a density $\mathrm{[g\,cm^{-3}]}$.}
vertical spacing of 11\textasciitilde{}points, and should be indented \label{FigGam}%
0.25\textasciitilde{}inches more than normal on left-hand and right-hand \end{figure*}
margins. Insert 0.4\textasciitilde{}inches of blank space after the
body. Keep your abstract brief and self-contained, limiting it to one In this section the one-zone model of \citet{DudaHart2nd},
paragraph and roughly 4–6 sentences. Gross violations will require originally used to study the Cephe{\"{\i}}d pulsation mechanism, will
correction at the camera-ready phase. be briefly reviewed. The resulting stability criteria will be
rewritten in terms of local state variables, local timescales and
## Partitioning the Text constitutive relations.
You should organize your paper into sections and paragraphs to help \citet{DudaHart2nd} investigates the stability of thin layers in
readers place a structure on the material and understand its self-gravitating,
contributions. spherical gas clouds with the following properties:
\begin{itemize}
### Sections and Subsections \item hydrostatic equilibrium,
\item thermal equilibrium,
Section headings should be numbered, flush left, and set in \item energy transport by grey radiation diffusion.
11\textasciitilde{}pt bold type with the content words capitalized. \end{itemize}
Leave 0.25\textasciitilde{}inches of space before the heading and For the one-zone-model Baker obtains necessary conditions
0.15\textasciitilde{}inches after the heading. for dynamical, secular and vibrational (or pulsational)
stability (Eqs.\ (34a,\,b,\,c) in Baker \citeyear{DudaHart2nd}). Using Baker's
Similarly, subsection headings should be numbered, flush left, and set notation:
in 10\textasciitilde{}pt bold type with the content words capitalized.
Leave 0.2\textasciitilde{}inches of space before the heading and \noindent
0.13\textasciitilde{}inches afterward. and with the definitions of the \emph{local cooling time\/}
(see Fig.~\ref{FigGam})
Finally, subsubsection headings should be numbered, flush left, and set \begin{equation}
in 10\textasciitilde{}pt small caps with the content words capitalized. \tau_{\mathrm{co}} = \frac{E_{\mathrm{th}}}{L_{r0}} \,,
Leave 0.18\textasciitilde{}inches of space before the heading and \end{equation}
0.1\textasciitilde{}inches after the heading. and the \emph{local free-fall time}
\begin{equation}
Please use no more than three levels of headings. \tau_{\mathrm{ff}} =
\sqrt{ \frac{3 \pi}{32 G} \frac{4\pi r_0^3}{3 M_{\mathrm{r}}}
### Paragraphs and Footnotes }\,,
\end{equation}
Within each section or subsection, you should further partition the Baker's $K$ and $\sigma_0$ have the following form:
paper into paragraphs. Do not indent the first line of a given \begin{eqnarray}
paragraph, but insert a blank line between succeeding ones. \sigma_0 & = & \frac{\pi}{\sqrt{8}}
\frac{1}{ \tau_{\mathrm{ff}}} \\
You can use footnotes\footnote{Footnotes K & = & \frac{\sqrt{32}}{\pi} \frac{1}{\delta}
should be complete sentences.} to provide readers with additional \frac{ \tau_{\mathrm{ff}} }
information about a topic without interrupting the flow of the paper. { \tau_{\mathrm{co}} }\,;
Indicate footnotes with a number in the text where the point is most \end{eqnarray}
relevant. Place the footnote in 9\textasciitilde{}point type at the where $E_{\mathrm{th}} \approx m (P_0/{\rho_0})$ has been used and
bottom of the column in which it appears. Precede the first footnote in \begin{equation}
a column with a horizontal rule of \begin{array}{l}
0.8\textasciitilde{}inches.\footnote{Multiple footnotes can \delta = - \left(
appear in each column, in the same order as they appear in the text, \frac{ \partial \ln \rho }{ \partial \ln T }
but spread them across columns and pages if possible.} \right)_P \\
e=mc^2
\begin{figure}[ht] \end{array}
\vskip 0.2in \end{equation}
\begin{center} is a thermodynamical quantity which is of order $1$ and equal to $1$
\centerline{\includegraphics[width=\columnwidth]{Figure/icml_numpapers.eps}} for nonreacting mixtures of classical perfect gases. The physical
\caption{Historical locations and number of accepted papers for International meaning of $\sigma_0$ and $K$ is clearly visible in the equations
Machine Learning Conferences (ICML 1993 -- ICML 2008) and International above. $\sigma_0$ represents a frequency of the order one per
Workshops on Machine Learning (ML 1988 -- ML 1992). At the time this figure was free-fall time. $K$ is proportional to the ratio of the free-fall
produced, the number of accepted papers for ICML 2008 was unknown and instead time and the cooling time. Substituting into Baker's criteria, using
estimated.} thermodynamic identities and definitions of thermodynamic quantities,
\label{icml-historical} \begin{displaymath}
\end{center} \Gamma_1 = \left( \frac{ \partial \ln P}{ \partial\ln \rho}
\vskip -0.2in \right)_{S} \, , \;
\end{figure} \chi^{}_\rho = \left( \frac{ \partial \ln P}{ \partial\ln \rho}
\right)_{T} \, , \;
## Figures \kappa^{}_{P} = \left( \frac{ \partial \ln \kappa}{ \partial\ln P}
\right)_{T}
You may want to include figures in the paper to illustrate your approach \end{displaymath}
and results. Such artwork should be centered, legible, and separated \begin{displaymath}
from the text. Lines should be dark and at least \nabla_{\mathrm{ad}} = \left( \frac{ \partial \ln T}
0.5\textasciitilde{}points thick for purposes of reproduction, and text { \partial\ln P} \right)_{S} \, , \;
should not appear on a gray background. \chi^{}_T = \left( \frac{ \partial \ln P}
{ \partial\ln T} \right)_{\rho} \, , \;
Label all distinct components of each figure. If the figure takes the \kappa^{}_{T} = \left( \frac{ \partial \ln \kappa}
form of a graph, then give a name for each axis and include a legend { \partial\ln T} \right)_{T}
that briefly describes each curve. Do not include a title inside the \end{displaymath}
figure; instead, the caption should serve this function. one obtains, after some pages of algebra, the conditions for
\emph{stability\/} given
Number figures sequentially, placing the figure number and caption below:
\emph{after} the graphics, with at least 0.1\textasciitilde{}inches of \begin{eqnarray}
space before the caption and 0.1\textasciitilde{}inches after it, as in \frac{\pi^2}{8} \frac{1}{\tau_{\mathrm{ff}}^2}
\cref{icml-historical}. The figure caption should be set in ( 3 \Gamma_1 - 4 )
9\textasciitilde{}point type and centered unless it runs two or more & > & 0 \label{ZSDynSta} \\
lines, in which case it should be flush left. You may float figures to \frac{\pi^2}{\tau_{\mathrm{co}}
the top or bottom of a column, and you may set wide figures across both \tau_{\mathrm{ff}}^2}
columns (use the environment \texttt{figure*} in \LaTeX). Always place \Gamma_1 \nabla_{\mathrm{ad}}
two-column figures at the top or bottom of the page. \left[ \frac{ 1- 3/4 \chi^{}_\rho }{ \chi^{}_T }
( \kappa^{}_T - 4 )
## Algorithms + \kappa^{}_P + 1
\right]
If you are using \LaTeX, please use the & > & 0 \label{ZSSecSta} \\
\texttt{algorithm\textquotesingle{}\textquotesingle{}\ and}algorithmic’’ \frac{\pi^2}{4} \frac{3}{\tau_{ \mathrm{co} }
environments to format pseudocode. These require the corresponding \tau_{ \mathrm{ff} }^2
stylefiles, algorithm.sty and algorithmic.sty, which are supplied with }
this package. \cref{alg:example} shows an example. \Gamma_1^2 \, \nabla_{\mathrm{ad}} \left[
4 \nabla_{\mathrm{ad}}
\begin{algorithm}[tb] - ( \nabla_{\mathrm{ad}} \kappa^{}_T
\caption{Bubble Sort} + \kappa^{}_P
\label{alg:example} )
\begin{algorithmic} - \frac{4}{3 \Gamma_1}
\STATE {\bfseries Input:} data $x_i$, size $m$ \right]
\REPEAT & > & 0 \label{ZSVibSta}
\STATE Initialize $noChange = true$. \end{eqnarray}
\FOR{$i=1$ {\bfseries to} $m-1$}
\IF{$x_i > x_{i+1}$} For a physical discussion of the stability criteria see \citet{DudaHart2nd} or \citet{anonymous}.
\STATE Swap $x_i$ and $x_{i+1}$
\STATE $noChange = false$ We observe that these criteria for dynamical, secular and
\ENDIF vibrational stability, respectively, can be factorized into
\ENDFOR \begin{enumerate}
\UNTIL{$noChange$ is $true$} \item a factor containing local timescales only,
\end{algorithmic} \item a factor containing only constitutive relations and
\end{algorithm} their derivatives.
\end{enumerate}
## Tables The first factors, depending on only timescales, are positive
by definition. The signs of the left hand sides of the
You may also want to include tables that summarize material. Like inequalities~(\ref{ZSDynSta}), (\ref{ZSSecSta}) and (\ref{ZSVibSta})
figures, these should be centered, legible, and numbered consecutively. therefore depend exclusively on the second factors containing
However, place the title \emph{above} the table with at least the constitutive relations. Since they depend only
0.1\textasciitilde{}inches of space before the title and the same after on state variables, the stability criteria themselves are \emph{
it, as in \cref{sample-table}. The table title should be set in functions of the thermodynamic state in the local zone}. The
9\textasciitilde{}point type and centered unless it runs two or more one-zone stability can therefore be determined
lines, in which case it should be flush left. from a simple equation of state, given for example, as a function
of density and
\begin{table}[t] temperature. Once the microphysics, i.e.\ the thermodynamics
\caption{Classification accuracies for naive Bayes and flexible and opacities (see Table~\ref{KapSou}), are specified (in practice
Bayes on various data sets.} by specifying a chemical composition) the one-zone stability can
\label{sample-table} be inferred if the thermodynamic state is specified.
\vskip 0.15in The zone -- or in
\begin{center} other words the layer -- will be stable or unstable in
\begin{small} whatever object it is imbedded as long as it satisfies the
\begin{sc} one-zone-model assumptions. Only the specific growth rates
\begin{tabular}{lcccr} (depending upon the time scales) will be different for layers
\toprule in different objects.
Data set & Naive & Flexible & Better? \\
\midrule \begin{table}
Breast & 95.9$\pm$ 0.2& 96.7$\pm$ 0.2& $\surd$ \\ \caption[]{Opacity sources.}
Cleveland & 83.3$\pm$ 0.6& 80.0$\pm$ 0.6& $\times$\\ \label{KapSou}
Glass2 & 61.9$\pm$ 1.4& 83.8$\pm$ 0.7& $\surd$ \\ $$
Credit & 74.8$\pm$ 0.5& 78.3$\pm$ 0.6& \\ \begin{array}{p{0.5\linewidth}l}
Horse & 73.3$\pm$ 0.9& 69.7$\pm$ 1.0& $\times$\\ \hline
Meta & 67.1$\pm$ 0.6& 76.5$\pm$ 0.5& $\surd$ \\ \noalign{\smallskip}
Pima & 75.1$\pm$ 0.6& 73.9$\pm$ 0.5& \\ Source & T / {[\mathrm{K}]} \\
Vehicle & 44.9$\pm$ 0.6& 61.5$\pm$ 0.4& $\surd$ \\ \noalign{\smallskip}
\bottomrule \hline
\end{tabular} \noalign{\smallskip}
\end{sc} Yorke 1979, Yorke 1980a & \leq 1700^{\mathrm{a}} \\
\end{small}
\end{center} Kr\"ugel 1971 & 1700 \leq T \leq 5000 \\
\vskip -0.1in Cox \& Stewart 1969 & 5000 \leq \\
\noalign{\smallskip}
\hline
\end{array}
$$
\end{table} \end{table}
Tables contain textual material, whereas figures contain graphical We will now write down the sign (and therefore stability)
material. Specify the contents of each row and column in the table’s determining parts of the left-hand sides of the inequalities
topmost row. Again, you may float tables to a column’s top or bottom, (\ref{ZSDynSta}), (\ref{ZSSecSta}) and (\ref{ZSVibSta}) and thereby
and set wide tables across both columns. Place two-column tables at the obtain \emph{stability equations of state}.
top or bottom of the page.
The sign determining part of inequality~(\ref{ZSDynSta}) is
## Theorems and such $3\Gamma_1 - 4$ and it reduces to the
criterion for dynamical stability
The preferred way is to number definitions, propositions, lemmas, etc. \begin{equation}
consecutively, within sections, as shown below. \Gamma_1 > \frac{4}{3}\,\cdot
\end{equation}
\begin{definition} Stability of the thermodynamical equilibrium demands
\label{def:inj} \begin{equation}
A function $f:X \to Y$ is injective if for any $x,y\in X$ different, $f(x)\ne f(y)$. \chi^{}_\rho > 0, \;\; c_v > 0\, ,
\end{definition} \end{equation}
and
Using \cref{def:inj} we immediate get the following result: \begin{equation}
\chi^{}_T > 0
\begin{proposition} \end{equation}
If $f$ is injective mapping a set $X$ to another set $Y$, holds for a wide range of physical situations.
the cardinality of $Y$ is at least as large as that of $X$ With
\end{proposition} \begin{eqnarray}
\begin{proof} \Gamma_3 - 1 = \frac{P}{\rho T} \frac{\chi^{}_T}{c_v}& >& 0\\
Left as an exercise to the reader. \Gamma_1 = \chi_\rho^{} + \chi_T^{} (\Gamma_3 -1)& >& 0\\
\end{proof} \nabla_{\mathrm{ad}} = \frac{\Gamma_3 - 1}{\Gamma_1} & >& 0
\end{eqnarray}
\cref{lem:usefullemma} stated next will prove to be useful. we find the sign determining terms in inequalities~(\ref{ZSSecSta})
and (\ref{ZSVibSta}) respectively and obtain the following form
\begin{lemma} of the criteria for dynamical, secular and vibrational
\label{lem:usefullemma} \emph{stability}, respectively:
For any $f:X \to Y$ and $g:Y\to Z$ injective functions, $f \circ g$ is injective. \begin{eqnarray}
\end{lemma} 3 \Gamma_1 - 4 =: S_{\mathrm{dyn}} > & 0 & \label{DynSta} \\
\begin{theorem} \frac{ 1- 3/4 \chi^{}_\rho }{ \chi^{}_T } ( \kappa^{}_T - 4 )
\label{thm:bigtheorem} + \kappa^{}_P + 1 =: S_{\mathrm{sec}} > & 0 & \label{SecSta} \\
If $f:X\to Y$ is bijective, the cardinality of $X$ and $Y$ are the same. 4 \nabla_{\mathrm{ad}} - (\nabla_{\mathrm{ad}} \kappa^{}_T
\end{theorem} + \kappa^{}_P)
- \frac{4}{3 \Gamma_1} =: S_{\mathrm{vib}}
An easy corollary of \cref{thm:bigtheorem} is the following: > & 0\,.& \label{VibSta}
\end{eqnarray}
\begin{corollary} The constitutive relations are to be evaluated for the
If $f:X\to Y$ is bijective, unperturbed thermodynamic state (say $(\rho_0, T_0)$) of the zone.
the cardinality of $X$ is at least as large as that of $Y$. We see that the one-zone stability of the layer depends only on
\end{corollary} the constitutive relations $\Gamma_1$,
\begin{assumption} $\nabla_{\mathrm{ad}}$, $\chi_T^{},\,\chi_\rho^{}$,
The set $X$ is finite. $\kappa_P^{},\,\kappa_T^{}$.
\label{ass:xfinite} These depend only on the unperturbed
\end{assumption} thermodynamical state of the layer. Therefore the above relations
\begin{remark} define the one-zone-stability equations of state
According to some, it is only the finite case (cf. \cref{ass:xfinite}) that is interesting. $S_{\mathrm{dyn}},\,S_{\mathrm{sec}}$
\end{remark} and $S_{\mathrm{vib}}$. See Fig.~\ref{FigVibStab} for a picture of
$S_{\mathrm{vib}}$. Regions of secular instability are
## Citations and References listed in Table~1.
If you rely on the \LaTeX\{\} bibliographic facility, use \begin{figure}
\texttt{natbib.sty} included in the style-file package to obtain \centering
reference. \caption{Vibrational stability equation of state
$S_{\mathrm{vib}}(\lg e, \lg \rho)$.
Citations within the text should include the authors’ last names and $>0$ means vibrational stability.
year. If the authors’ names are included in the sentence, place only the }
year in parentheses, for example when referencing Arthur Samuel’s \label{FigVibStab}
pioneering work \yrcite{Samuel59}. Otherwise place the entire reference \end{figure}
in parentheses with the authors and year separated by a comma
\cite{Samuel59}. List multiple references separated by semicolons
\cite{kearns89,Samuel59,mitchell80}. Use the `et\textasciitilde{}al.’
construct only for citations with three or more authors or after listing
all authors to a publication in an earlier reference
\cite{MachineLearningI}.
Use an unnumbered first-level section heading for the references, and
use a hanging indent style, with the first line of the reference flush
against the left margin and subsequent lines indented by 10 points. The
references at the end of this document give examples for journal
articles \cite{Samuel59}, conference publications \cite{langley00}, book
chapters \cite{Newell81}, books \cite{DudaHart2nd}, edited volumes
\cite{MachineLearningI}, technical reports \cite{mitchell80}, and
dissertations \cite{kearns89}.
Alphabetize references by the surnames of the first authors, with single
author entries preceding multiple author entries. Order references for
the same authors by year of publication, with the earliest first. Make
sure that each reference includes all relevant information (e.g., page
numbers).
Please put some effort into making references complete, presentable, and # Conclusions
consistent, e.g.~use the actual current name of authors. If using
bibtex, please protect capital letters of names and abbreviations in \begin{enumerate}
titles, for example, use \{B\}ayesian or \{L\}ipschitz in your .bib \item The conditions for the stability of static, radiative
file. layers in gas spheres, as described by Baker's (\citeyear{DudaHart2nd})
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.
\item 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.
\item For solar composition gas the $\kappa$-mechanism is
working in the regions of the ice and dust features
in the opacities, the $\mathrm{H}_2$ 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 Cephe{\"\i}d pulsations.
\end{enumerate}
# Acknowledgements
Acknowledgements is an unnumbered section at the end of the paper.
Typically, this will include thanks to colleagues who contributed to the
ideas, and to funding agencies and corporate sponsors that provided
financial support.
Hasan al Rasyid
3 years ago