Model Article for the preprint style elsart
S.A.M. Pepping
Elsevier Science, P.O. Box 103, 1000 AC Amsterdam, Netherlands
Abstract
This article discusses several features of preparing preprints with the elsart document style.
Key words: preprint style, elsart, LATEX style, model article, guide lines
PACS: 01.30.−y
1
Introduction
This article discusses several features of preparing preprints with the elsart
document style. For more general information about LATEX, see the LATEX
manual written by Lamport [1] or the booklet Preparing Articles with LATEX,
which is part of Elsevier Science’s LATEX package (see below).
All macro packages recommended in this document can be obtained from one
of the servers of the Comprehensive TeX Archive Network (CTAN). CTAN
is a mirrored network of the FTP servers ftp.tex.ac.uk, ftp.dante.de
and ctan.tug.org, which are widely mirrored (see ftp://ctan.tug.org/
tex-archive/README.mirrors) and hold up-to-date copies of all the publicdomain versions of TEX, LATEX, Metafont and ancillary programs.
Elsevier Science has prepared a LATEX package for authors, which contains the
following files:
• ascii.tab (ASCII table),
• elsart.cls (use this file if you are using LATEX 2ε , the current version of
LATEX),
Email address: s.pepping@elsevier.nl (S.A.M. Pepping).
URL: www.elsevier.com/locate/latex (S.A.M. Pepping).
Preprint submitted to Elsevier Science
17 September 2001
• elsart.sty and elsart12.sty (use these two files if you are using LATEX2.09,
the now obsolete version of LaTeX),
• instraut.dvi and/or instraut.ps (instruction booklet),
• readme.
The package is freely available from Elsevier Science’s Web servers
http://www.elsevier.com/locate/latex, and from CTAN in the directory
/tex-archive/macros/latex/contrib/supported/elsevier.
2
Options
There is an option to obtain double line spacing, as is sometimes required for
copies submitted for review. It is called doublespacing or reviewcopy.
3
Frontmatter
The elsart document class has a separate frontmatter environment for the
title, authors, addresses, abstract and keywords.
• \title: As in standard LATEX, e.g. \title{Model}.
• \author: Different from standard LATEX, the \author command contains
only one author and no address. Multiple authors go into multiple \author
commands, separated from each other by commas. The address goes into a
separate \address command. Example: \author{D.E. Knuth}.
• \address: Here goes the address, e.g. \address{CERN, Geneva}.
• \thanks and \thanksref: These provide footnotes to the title, authors and
addresses. The \thanksref command takes a label: \thanksref{label} to
relate it to the \thanks command with the same label: \thanks[label].
There can be several references to a single \thanks command. Example:
\title{Model\thanksref{titlefn}} and
\thanks[titlefn]{Supported by grants.}
• \corauth and \corauthref: These provide footnotes to mark the corresponding author and the correspondence address. They are used in the
same manner as \thanks and \thanksref. Example:
\author{A. Name\corauthref{cor}} and
\corauth[cor]{Corresponding author. Address: ... .}
• \ead: This command should be used for the email address or the URL of the
author. It refers to the ‘current author’, i.e., the author last mentioned before
the command. When it holds a URL, this should be indicated by setting
the optional argument to ‘url’. Example: \ead{s.pepping@elsevier.nl},
\ead[url]{www.elsevier.com/locate/latex}.
2
It is not necessary to give a \maketitle command. The title, authors and
addresses are printed as soon as TEX sees them.
The authors and addresses can be combined in one of two ways:
• The simplest way lists the authors of one address, followed by the address,
and so on for all addresses.
• The other way first lists all authors, and then all addresses. The authors
and addresses are related to each other by labels: \author[label1]{Name1}
corresponds to \address[label1]{Address1}.
\author[South]{T.R. Marsh},
\author[Oxford]{S.R. Duck}
\address[South]{University of Southampton, UK}
\address[Oxford]{University of Oxford, UK}
See the examples in figs. 1, 2, 3, 4.
If you put the frontmatter in an included file, that file should contain the
whole frontmatter, including its begin and end commands. Otherwise, the
labels of the frontmatter will remain undefined.
4
Abstract
The abstract should be self-contained. Therefore, do not refer to the list of
references. Instead, quote the reference in full, as follows: Wettig & Brown
(1996, NewA, 1, 17).
5
Keywords
In electronic publications a proper classification is more important than ever.
Elsevier Science’s physics journals use several keyword schemes:
Keywords: Uncontrolled keywords.
PACS: The PACS scheme, developed and maintained by the AIP, covers
the whole field of Physics. See http://www.aip.org/pacs/pacs.html or
http://www.elsevier.com/locate/pacs.
MSC: The MSC scheme, developed and maintained by the AMS, covers the
whole field of Mathematics. See http://www.ams.org/msc or http://www.
elsevier.com/locate/msc.
3
\documentclass{elsart}
\usepackage{graphicx,amssymb}
\journal{New Astronomy}
\begin{document}
\begin{frontmatter}
\title{Stroboscopic Doppler tomography of FO Aqr}
\author[South]{T.R. Marsh\corauthref{cor}},
\corauth[cor]{Corresponding author.}
\ead{trm@astro.soton.ac.uk}
\author[Oxford]{S.R. Duck\thanksref{now}}
\thanks[now]{Present address: Systems Engineering and Assessment Ltd.,
Beckington Castle, PO Box 800, Bath BA3 6TB, UK.}
\ead{srd@sea.co.uk}
\address[South]{University of Southampton, Department of Physics,
Highfield, Southampton SO17 1BJ, UK}
\address[Oxford]{University of Oxford, Department of Physics, Nuclear
Physics Laboratory, Keble Road, Oxford, OX1 3RH, UK}
\begin{abstract}
FO Aqr is a close binary star in
which a magnetic white dwarf accretes from a cool companion. Light
curves and spectra show variations on the orbital frequency, the
white dwarf’s spin frequency and combinations of the two.
\end{abstract}
\begin{keyword}
Accretion, accretion disks \sep Line: profiles \sep
Binaries: close \sep Novae, cataclysmic variables
\PACS 97.10.Gz \sep 97.30.Qt \sep 97.80.Gm
\end{keyword}
\end{frontmatter}
\section{Introduction}
FO Aqr is a member of the
are close binary stars in
a late-type main-sequence
recently been reviewed in
DQ~Her class of stars which
which a magnetic white dwarf accretes from
secondary star. These stars have most
Ref. \cite{Patterson94}.
Fig. 1. Article opening with explicit links (input)
4
Stroboscopic Doppler tomography of FO Aqr
T.R. Marsha,∗ , S.R. Duckb,1
a University
of Southampton, Department of Physics,
Highfield, Southampton SO17 1BJ, UK
b University of Oxford, Department of Physics, Nuclear Physics
Laboratory, Keble Road, Oxford, OX1 3RH, UK
Abstract
FO Aqr is a close binary star in which a magnetic white dwarf accretes from a
cool companion. Light curves and spectra show variations on the orbital frequency,
the white dwarf’s spin frequency and combinations of the two.
Key words: Accretion, accretion disks, Line: profiles, Binaries: close, Novae, cataclysmic variables
PACS: 97.10.Gz, 97.30.Qt, 97.80.Gm
Introduction
FO Aqr is a member of the DQ Her class of stars which are close binary stars
in which a magnetic white dwarf accretes from a late-type main-sequence
secondary star. These stars have most recently been reviewed in Ref. [1].
∗
Corresponding author.
Present address: Systems Engineering and Assessment Ltd., Beckington Castle,
PO Box 800, Bath BA3 6TB, UK.
Email addresses: trm@astro.soton.ac.uk (T.R. Marsh), srd@sea.co.uk (S.R.
Duck).
1
Preprint submitted to New Astronomy
21 August 1997
Fig. 2. Article opening with explicit links (output)
5
\documentclass{elsart}
\begin{document}
\begin{frontmatter}
\title{Integrability in
random matrix models\thanksref{talk}}
\thanks[talk]{Expanded version of a talk
presented at the Singapore Meeting on
Particle Physics (Singapore, August 1990).}
\author{L. Alvarez-Gaum\’{e}\corauthref{cor}}
\address{Theory Division, CERN,
CH-1211 Geneva 23, Switzerland}
\ead{lag@cern.ch}
\author{C. Gomez\corauthref{cor}\thanksref{SNSF}}
\address{D\’{e}partment de Physique Th\’{e}orique,
Universit\’{e} de Gen\‘{e}ve,
CH-1211 Geneva 4, Switzerland}
\ead{cg@ug.ch}
\author{J. Lacki}
\address{School of Natural Sciences,
Institute for Advanced Study,
Princeton, NJ 08540, USA}
\ead[url]{www.ias.edu/~jl}
\thanks[SNSF]{Supported by the
Swiss National Science Foundation}
\begin{abstract}
We prove the equivalence between the recent matrix
model formulation of 2D gravity and lattice
integrable models. For even potentials this
system is the Volterra hierarchy.
\end{abstract}
\end{frontmatter}
\section{Introduction}
Some aspects of the recently discovered
non-perturbative solutions to non-critical strings
\cite{Patterson94} can be better understood and
clarified directly in terms of the integrability
properties of the random matrix model.
...
Fig. 3. Article opening with implicit links (input)
6
Integrability in random matrix models?
L. Alvarez-Gaumé∗
Theory Division, CERN, CH-1211 Geneva 23, Switzerland
C. Gomez∗,1
Départment de Physique Théorique, Université de Genève, CH-1211 Geneva 4,
Switzerland
J. Lacki
School of Natural Sciences, Institute for Advanced Study, Princeton, NJ 08540,
USA
Abstract
We prove the equivalence between the recent matrix model formulation of 2D
gravity and lattice integrable models. For even potentials this system is the Volterra
hierarchy.
1. Introduction
Some aspects of the recently discovered non-perturbative solutions to noncritical strings [1] can be better understood and clarified directly in terms of
the integrability properties of the random matrix model.
...
Fig. 4. Article opening with implicit links (output)
7
Keywords are entered below the abstract in the following way:
\begin{keyword}
Keyword \sep Keyword
\PACS PACS code \sep PACS code
\MSC MSC code \sep MSC code
\end{keyword}
6
Cross-references
In electronic publications articles may be internally hyperlinked. Hyperlinks
are generated from proper cross-references in the article.
For example, the words Fig. 1 will never be more than simple text, whereas
the proper cross-reference \ref{mapfigure} may be turned into a hyperlink
to the figure itself.
In the same way, the words Ref. [1] will fail to turn into a hyperlink; the proper
cross-reference is \cite{Gea97}.
Cross-referencing is possible in LATEX for sections, subsections, formulae, figures, tables, and literature references.
7
PostScript figures
LATEX and PostScript have had a long and successful relationship. In the
current version of LATEX, LATEX 2ε , there are three packages for including
PostScript figures:
• graphics. This simple package provides the command
\includegraphics*[][]{file}. The * is optional; it
enables the PostScript feature of clipping. In its simplest form,
\includegraphics{file}, it includes the figure in the PostScript file file
without resizing.
• graphicx. This package provides the command
\includegraphics*[key--value list]{file}. The * is optional; it enables the PostScript feature of clipping. Often used keys are:
– scale=.40 to scale the size of the figure with 40%,
– width=25pc, height=15pc to set the width or height of the figure,
– angle=90 to rotate the figure over 90◦ .
8
\begin{figure}
\begin{center}
\includegraphics*[width=5cm]{name.eps}
\end{center}
\caption{An example of a figure.}
\label{fig:exmp}
\end{figure}
Fig. 5. An example of a figure.
• epsfig. This package is really the graphicx package, but it allows one
to include PostScript figures using the familiar commands from the earlier
packages epsfig and psfig.
For detailed information, see the documentation of the graphics packages, in
particular the file grfguide.tex.
8
Mathematical symbols
Many physics authors require more mathematical symbols than the few that
are provided in standard LATEX. A useful package for additional symbols is
the amssymb package, developed by the American Mathematical Society. This
package includes such oft used symbols as \lesssim for ., \gtrsim for & or
\hbar for ~. Note that your TEX system should have the msam and msbm fonts
installed. If you need only a few symbols, such as \Box for , you might try
the package latexsym.
In the elsart document class vectors are preferably coded as \vec{a} instead
of \bf{a} or \pol{a}.
9
The Bibliography
In LATEX literature references are listed in the thebibliography environment.
Each reference is a \bibitem; each \bibitem is identified by a label, by which
it can be cited in the text: \bibitem{ESG96} is cited as \cite{ESG96}.
Version 2.16 of elsart introduces the subbibitems environment. The references in a subbibitems environment have the same major reference number,
and are counted by letters a, b, etc. The subbibitems environment has a label
of its own: \begin{subbibitems{label}. It can therefore be referred to as
\cite{label}, which produces a citation like [7a–c]. A short citation like [7]
9
can be produced by adding :s to the label: \cite{label:s}. Example: See
Refs. [6a–b], or in short form, see Refs. [6].
Version 2.16 of elsart also introduces the possibility to insert notes into the
bibliography, by using the \note command. In a subbibitems environment it
must be the last item. Example: See Refs. [5,7].
10
Template article
There is a template article templat-num.tex, which you can use as a skeleton
for your own article.
References
[1] Leslie Lamport: LATEX, A document preparation system, 2nd edition, AddisonWesley (Reading, Massachusetts, 1994).
[2] Wettig, T., & Brown, G.E., The evolution of relativistic binary pulsars, 1996,
NewA, 1, 17-34.
[3] Elson, R.A.W., Santiago, B.X., & Gilmore, G.F., Halo stars, starbursts, and
distant globular clusters: A survey of unresolved objects in the Hubble Deep
Field, 1996, NewA, 1, 1-16.
[4] Governato, F., Moore, B., Cen, R., Stadel, J., Lake, G., & Quinn, T., The Local
Group as a test of cosmological models, 1997, NewA 2, 91-106.
[5] We consider an exactly solvable two-band model of electrons moving in one
dimension and interacting with a δ-function spin-exchange potential.
[6a] N. Nagaosa and P. A. Lee, Phys. Rev. Lett. 79, 3755 (1997).
[6b] C. Pépin and P. A. Lee, Phys. Rev. Lett. 81, 2779 (1998).
[7] K. Gorny, O. M. Vyasilev, J. A. Marindale, V. A. Nandor, C. H. Pennington,
P. C. Hammel, W. L. Hults, J. L. Smith, P. L. Kuhns, A. P. Reyes and
W. G. Moulton, Phys. Rev. Lett. 82, 177 (1999).
These references demonstrate that for some high-Tc compounds the gap does not
seem to depend on the magnetic field.
10
