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\paperID{P2-36}
%%%% ID=P2-36
\title{Information System on Binary Stars}
%\titlemark{ }
\author{Oleg Yu.\ Malkov, Elena Yu.\ Kilpio}
\affil{Institute of Astronomy, Moscow, Russia}

\author{Ekaterina A.\ Snegireva}
\affil{Physical Department, Ural State University, Ekaterinbourg, Russia}

\author{Maxim S.\ Tuchin}
\affil{Physical Department, Moscow State University, Moscow, Russia}

\contact{Oleg Malkov}
\email{malkov@inasan.ru}

\paindex{Malkov, O. Yu.}
\aindex{Kilpio, E. Yu.}
\aindex{Snegireva, E.}
\aindex{Tuchin, M.}

\authormark{Malkov, Kilpio, Snegireva \& Tuchin}
\keywords{information: system, catalogs, binary stars}

\begin{abstract}          % Leave intact
We present a project of an Information system on binary stars (ISBS).
The main goal of the system is to collect information on masses and
other astrophysical parameters of components of binary/mul\-ti\-ple
systems. A first version of ISBS will contain astronomical data
catalogues, related to observations of eclipsing binary stars. An
interface will provide access to the summary description of the
catalogues either by GCVS identifier or by evolutionary type. The ISBS
will allow user to make statistical investigations as well as to
obtain data on a particular binary system. The majority of the
included catalogues are presented in machine readable form for the
first time. It is likely that ISBS will be merged naturally into the
Russian Virtual Observatory and into the Besancon database on binaries.
\end{abstract}

\section{Introduction}

Eclipsing binaries represent one of the most numerous type of
binaries. Independent stellar mass and luminosity determination is
possible only for components of eclipsing binaries, with the spectrum
lines of the two components. They represent only some 5\% of all known
eclipsing binaries. So, for statistical investigations it would be
advisable to estimate fundamental parameters (such as mass and radius)
for eclipsing binaries with unknown spectroscopic elements.

That was a goal of authors of early catalogues (Brancewicz 
\& Dworak 1980, Svechnikov \& Kuznetsova 1990).
But the number of known eclipsing binaries increases constantly;
current version of the General Catalogue of Variable Stars, GCVS
(Kholopov et al. 1985-1988;
see also http://www.sai.msu.su/groups/clus\-ter/gcvs/gcvs/ for living edition)
contains about 6250 eclipsing binaries, in comparison with some 5000
systems in the 1988 version (this statistics does not
include variables discovered in large surveys, like OGLE).
Observational data is collected in a number of other catalogues,
devoted to various types of eclipsing binaries.

In this paper we present a project of an information system on binary
stars.
Our main goal is to collect information on masses and other
astrophysical parameters of components of binary systems.
ISBS will allow user to make statistical investigations as well as
to obtain data on a particular binary system.
A first version of the system
will include data on eclipsing binaries. 
Future versions will include
data on visual,
spectroscopic and other types of binaries (allowing to determine
astrophysical stellar parameters of components), particularly,
data on evolved close binary systems (Cherepashchuk et al., 1996).

\section{Classification of eclipsing binaries}

Primaries in close binary stars can undergo Roche lobe overflow during
various stages of their evolution. Cases A and B indicate systems
where mass transfer starts at core hydrogen burning stage and at
hydrogen shell burning stage, respectively.
Fig.~\ref{P2-36:fig1} illustrates mass transfer cases on the 
mass --- separation diagram. 

\begin{figure}
\epsscale{.50}
\plotone{P2-36_f1.eps}
\caption{Close binaries evolutionary scheme.
$m_1$ - initial mass of more massive component, in solar mass; $a$
- initial semi-major axis, in solar radius; $m_2$ is adopted to be
approximately equal to $m_1$. The figure is taken from
Yungelson \& Massevich (1982)}
\label{P2-36:fig1}
\end{figure}

Eclipsing binaries in the ISBS are classified according to the
following scheme, introduced by Svechnikov (1986):

DM --- detached main sequence systems, where both components are main
sequence stars, which do not fill their inner Roche lobes

SD --- semi-detached systems, where the more massive component is a main
sequence star, and the less massive secondary component is a subgiant which
fills (or nearly fills) its Roche lobe

DS --- detached systems with a subgiant secondary, where the less
massive subgiant component distinctly does not fill its Roche lobe

AR --- detached systems with two subgiant components, where both stars
do not fill their Roche lobe (AR Lac-type systems)

CE --- contact systems of early spectra, both components are close to
their Roche lobes, and the spectrum of the more massive component is not later
than about F0

CW --- contact systems of W UMa-type with %FO the 
   periods shorter than 0.5
days and where the spectrum of the more massive component is
later than about F0

DW --- systems, similar to W UMa-stars, where both components do not
fill their Roche lobes, and their physical characteristics are similar
to those of CW-systems (short-period RS CVn-type systems)

GS --- systems with at least one supergiant or late type giant.

\medskip\noindent %% FO
We assume that, depending on age, separation between components and %% their 
masses, % a system of Case A mass transfer can be observed
mass transfer in a system of Case A can be observed
as a DW-, CW- or CE-type system, 
while in a system of Case B mass transfer
can be observed as a AR-, DS- or SD-type system (a few exceptions are
possible). GS-type systems can
undergo Roche lobe overflow during
helium burning stage (Case C, not shown in Fig~\ref{P2-36:fig1}).
DM-type systems do not (yet) undergo Roche lobe overflow and,
during their evolution and
depending on separation between components and their masses, can
belong to any of the three cases.

\section{Catalogues of binaries}

The first version of the ISBS will include catalogues of eclipsing
binary stars and will give access to the summary description of the
catalogues and to catalogue data. Stars from the following catalogues
will be included in the first version of ISBS:
%
Catalog of orbital elements, masses and luminosities of close double
stars (Svechnikov \& Bessonova 1984);
%
The catalogue of approximate photometric and absolute elements of
eclipsing variable stars (Svechnikov \& Kuznetsova 1990);
%
The catalogue of orbital elements, masses and luminosities of
detached main-sequence eclipsing variable stars with known photometric
and spectroscopic elements (Svechnikov \& Perevozkina 1999);
%
The catalogue of orbital elements, masses and luminosities of
detached main-sequence eclipsing variable stars with known elements of
photometric orbit and unknown spectroscopic elements (Perevozkina \&
Svechnikov 1999);
%
The catalogue of photometric, geometrical and absolute elements of
semidetached eclipsing binary systems with known spectroscopic orbits
(Surkova \& Svechnikov 2004a);
%
The catalogue of photometric, geometrical and absolute elements of
semidetached eclipsing binary systems with known photometric orbits
and unknown spectroscopic orbits (Surkova \& Svechnikov 2004b);
%
The catalogue of photometric, geometrical and absolute elements of
contact binary stars of the early spectral type (Bondarenko \&
Perevozkina 1996);
%
Massive close binaries with early-type components of main sequence
catalogue. Observed characteristics (Polushina 2004);
%
Catalogue of pre-contact, short-period RS CVn-type systems 
(Dryomova 2004);
%
Catalogue of astrophysical parameters of binary systems
(Malkov 1993);
%
Stellar mass catalogue (Belikov 1995);
%
Age and metallicity estimates of intermediate mass stars in
eclipsing binaries (Kovaleva 2001).

It is likely that ISBS will be merged naturally into the
Russian Virtual Observatory (Dluzhnevskaya et al. 2003)
and into the Besancon database on binaries
(Oblak \& Debray 2004).

\begin{references}

\reference Belikov A. N. 1995, Bull. Inf. CDS 47, 9

\reference Bondarenko I. I. \& Perevozkina E. L. 1996,
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\reference Brancewicz H. K. \& Dworak T. Z. 1980, Acta 
Astron. 30, 502

\reference Cherepashchuk A., Katysheva N., Khruzina T., 
Shugarov S. 1996, Catalog of Evolved Close Binary Stars,
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parts 1 and 2.

\reference Dluzhnevskaya O., Malkov O., Kovaleva D., Kilpio A., Kilpio E.
2003, Astronomical and Astrophysical Transactions 22, 375

\reference Dryomova G. N. 2004,
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Ekaterinbourg, Ural University, in press

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\reference Kovaleva D. A. 2001, Astronomy Reports 45, 972

\reference Malkov O. Yu. 1993, Bull. Inf. CDS 42, 27

\reference Oblak E. \& Debray B. 2004, \adassxiii, \paperref{P2-31}

\reference Perevozkina E. L. \& Svechnikov M. A. 1999,
The catalogue of orbital elements, masses and luminosities of
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photometric orbit and unknown spectroscopic elements,
Ekaterinbourg, Ural University, p.122

\reference Polushina T. S. 2004,
Astronomical and Astrophysical Transactions, in press

\reference Surkova L. P. \& Svechnikov M. A. 2004a,
The catalogue of photometric, geometrical and absolute elements of
semidetached eclipsing binary systems with known spectroscopic orbits,
Ekaterinbourg, Ural University, in press

\reference Surkova L. P. \& Svechnikov M. A. 2004b,
The catalogue of photometric, geometrical and absolute elements of
semidetached eclipsing binary systems with known photometric orbits
and unknown spectroscopic orbits,
Ekaterinbourg, Ural University, in press

\reference Svechnikov M. A. 1986, The catalogue of orbital elements, masses
and luminosities of close binary stars, Irkutsk, Irkutsk Univ. Publ.

\reference Svechnikov M. A. \& Bessonova L. A. 1984, CDS Bull 26, 99

\reference Svechnikov M. A. \& Kuznetsova Eh. F. 1990,
Catalogue of approximate photometric and absolute elements of
eclipsing variable stars,
Vols. 1--2, Sverdlovsk, Ural University

\reference Svechnikov M. A. \& Perevozkina E. L. 1999,
The catalogue of orbital elements, masses and luminosities of
detached main-sequence eclipsing variable stars with known photometric
and spectroscopic elements,
Ekaterinbourg, Ural University, p.5

\reference Yungelson L. R. \& Massevich A. G. 1982, 
Itogi Nauki i Tekhniki 21, 27.

\end{references}

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