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{ISSN 0236-2457}
{\large\bf
\centerline{ASTRONOMICHESKII TSIRKULYAR}}
\medskip
\large
\centerline{Published by the Bureau of Astronomical Communications}
\centerline{of the Russian Academy of Sciences}
\centerline{and Sternberg Astronomical Institute}
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\hrule
\medskip
\centerline{No.15xx, 1996 September 5}
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\hrule
\bigskip
\centerline{\bf TITLE OF THE ARTICLE IN RUSSIAN}
\centerline{\bf (ALL CAPITAL CHARACTERS)}
\medskip
\centerline{\bf Title of the Article in English}
\centerline{\bf (Capitalize All the Words,}
\centerline{\bf except for Prepositions and Articles)}
\medskip
{\bf Abstract.} This text contains Instructions for
our Authors; at the same time, it shows the general layout of
a contribution to the Astronomicheskii Tsirkulyar as it will appear
published in the electronic form or printed on paper. See the source
file `sample.ltx', stored in this directory, to get an idea
on how we got this text. Place your abstract here, it must not exceed
ten lines. It is in English, if the article itself is in Russian, and
{\it vice versa.}
\bigskip
The text of your article starts here.
We accept articles in all branches of astronomy. Preference
is given to short notes containing information that should
be distributed as soon as possible (e.g., discoveries of supernovae,
novae, comets; important novel theoretical results, etc.)
Articles submitted should be accompanied by a recommendation from
a seminar specialized in the given branch of astronomy; please
justify in brief the necessity of rapid publication.
The Editors will greatly appreciate if you submit your contribution
in the form suitable for electronic publication and subsequent
printing on paper.
It is envisaged that the notes accepted by the Editors will be placed
in our WWW server (temporary address:
{\bf http://comet.sai.msu.su/ac/})
and thus will become available to all the WWW
users. From this moment on, the paper receives its reference with No.
and page(s) of the Astronomicheskii Tsirkulyar. The electronic version
will be distributed also via e-mail to all libraries and institutions
that possess facilities necessary to process the electronic version.
When a certain number of the contributions are accumulated, a
traditional paper version wll be printed and distributed via snailmail
according to our mailing list.
The volume of the contribution normally should not exceed 4 kilobytes
of the text with minimum number of figures and tabular material.
Please compose in \LaTeX, using our stylefile `atsirk.sty' and the file
`sample.ltx' (input file for the present text) as a template.
Submit your article
by e-mail to {\bf gmr@sai.msu.su} (if in Russian, please uuencode it, to
avoid problems with noncompatible cyrillic keyboards).
{\it However, if you have difficulties with computer equipment, e-mail
communication, or \LaTeX, we, for the time being, accept articles
in usual form (see Astronomicheskii Tsirkulyar No. 1543--1548,
Information for Authors), text taped and figures drawn on paper.
In this case, send your article by conventional mail to the address
given at the end of this text.}
Below we give you some examples of how to compose equations and tables
and to insert figures (which can be sent as uuencoded gif format files).
Evident inequalities:
$$
\pi\ga3.141\mbox{ and } \pi\la3.142
$$
\noindent(this formula is not numbered).
Here is the Saha equation
\begin{equation}
n_e\frac{n^+}{n_1}=\frac{g^+}{g_1}\frac{2(2\pi mkT)^{3/2}}{h^3}
\exp\left(-\frac{\chi_1}{kT}\right),
\end{equation}
\noindent
where $n^+$ is the number of ionized atoms in the ground state
(cm$^{-3}$), $g^+$ is the statistical weight of this state, $n_e$ is
number density of free electrons (cm$^{-3}$).
Equation of radiative transfer in spherical coordinates:
\begin{equation}
\cos\vartheta\frac{\partial I}{\partial r}
-\frac{\sin\vartheta}{r}\frac{\partial I}{\partial\vartheta}=
-\alpha I+\varepsilon,
\end{equation}
\noindent
where $\varepsilon$ is volume emissivity.
In cylindrical coordinates, the gravitational potential of a body
with arbitrary distribution of density $\sigma$ is:
\begin{equation}
U(r,\varphi,z)=G\int\!\!\int\limits_V\!\!\int
{\frac{\sigma(\rho,\psi,\zeta)\rho\,d\rho\,d\psi\,d\zeta}
{\sqrt{\rho^2+r^2-2\rho r\cos(\varphi-\psi)+(z-\zeta)^2}}},
\end{equation}
\noindent
where the integration is carried out over the entire volume $V$
of the body.
An example of an illustration:
\begin{figure}[h]
\vspace*{3cm}
\caption{Plot of stellar magnitudes {\it vs} time}
\end{figure}
\begin{table}[t]
\begin{center}
\caption{An example of a small table. Four brightest stars}
\medskip
\begin{tabular}{|l|l|c|c||c|c||c|}
\hline
& &\multicolumn{2}{|c||}{Other Names}&
\multicolumn{2}{|c||}{J2000}& \\
\cline{3-6}
Star & Name & & & & & $m_V$ \\
& & BD, CPD & HD & $\alpha$ & $\delta$ & (mag) \\
\hline
& & & & & & \\
$\alpha$ CMa & Sirius & $-$16\deg1591 & ~48915 & $06^{\rm h}\!45^{\rm m}\!
10\fs762$ &
$-16\deg41\arcmin57\farcs82$ & $-1\fmagn46$ \\
$\alpha$ Car & Canopus & $-$52\deg~914 & ~45348 & 06 23 57.005 &
$-$52 41 45.55 & $-$0.57 \\
$\alpha$ Boo & Arcturus & $+$19\deg2777 & 124897 & 14 15 43.458 &
$+$19 12 36.73 & $-$0.05 \\
$\alpha$ Lyr & Vega & $+$38\deg3238 & 172167 & 18 36 55.377 &
$+$38 46 46.78 & $+$0.03 \\
& && & & & \\
\hline
\end{tabular}
\end{center}
{\bf Notes to Table 1.} Here you can insert some comments
to the above Table.
\end{table}
\newpage
References should be given in parentheses (Kippenhahn R. and Thomas H.-C.,
A\&A, 1983, 124, 206). Use the abbreviations accepted
now in astronomy journals (see, e.g., the Astrophysical Journal):\\
AZh for Astronomicheskii Zhurnal \\
PAZh for Pis'ma v Astronomicheskii Zhurnal \\
ApJ for Astrophysical Journal \\
AJ for Astronomical Journal \\
A\&A for Astronomy and Astrophysics \\
MNRAS for Monthly Notices of the Royal Astronomical Society \\
etc.
At the end, please indicate author's name(s) and affiliation(s):
\medskip
\noindent
Sternberg Astron. Inst. \hspace{8cm} ç.í.òÕÄÎÉÃËÉÊ \\ \\
13 Universitetskij prosp.\hspace{8cm} G.M.Rudnitskij \\
Moscow, 119899 Russia \\
{\it gmr@sai.msu.su} \\
Received September 5, 1996
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