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                        GCVS  Variability  Types

                                  and

          Distribution Statistics of Designated Variable Stars

                According to their Types of Variability

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                    I.    GCVS  Variability  Types.



An improved system of variability classification is used in the fourth

edition of the GCVS, based on recent developments in classification

principles and taking into account the suggestions of a number of

specialists.  Variability types are grouped according to the major

astrophysical reasons for variability, viz.,



1. eruptive (FU, GCAS, I, IA, IB, IN, INA, INB, INT, IT, IN(YY), IS, ISA,

           ISB, RCB, RS, SDOR, UV, UVN, WR),

2. pulsating (ACYG, BCEP, BCEPS, CEP, CEP(B), CW, CWA, CWB, DCEP, DCEPS,

           DSCT, DSCTC, L, LB, LC, M, PVTEL, RR, RR(B), RRAB, RRC, RV,

           RVA, RVB, SR, SRA, SRB, SRC, SRD, SXPHE, ZZ, ZZA, ZZB),

3. rotating (ACV, ACVO, BY, ELL, FKCOM, PSR, SXARI),

4. cataclysmic (explosive and novalike) variables (N, NA, NB, NC, NL, NR,

           SN, SNI, SNII, UG, UGSS, UGSU, UGZ, ZAND),

5. eclipsing binary systems (E, EA, EB, EW, GS, PN, RS, WD, WR, AR, D, DM,

           DS, DW, K, KE, KW, SD),

6. intense variable X-ray sources (X, XB, XF, XI, XJ, XND, XNG, XP, XPR,

            XPRM, XM),

7. other symbols (BLLAC, CST, GAL, L:, QSO, S, *, +).



All of these classes include objects of a dissimilar nature that belong

to different types of light variability.  On the other hand, an object

may be variable because of almost all of the possible reasons or because

of any combination of them.  If a variable belongs to several types of

variability, the types are joined in the data field by a "+" sign, e.g.,

E+UG, UV+BY.



Despite considerable success in understanding stellar variability pro-

cesses, the classification adopted in the Catalogue is far from perfect.

This is especially the case for explosive, symbiotic and novalike

variables; X-ray sources; and peculiar objects.



The new variability types (ZZO, AM, R, BE, LBV, BLBOO, EP, SRS, LPB)

have been added in the Name-Lists 67- 77 and in the GCVS vol.V.



ZZO    ZZ Cet type variables of the DO spectral type showing HeII and

       and CIV absorbtion lines in their spectra.



AM     AM Her type variables; close binary systems consisting of a

       dK-dM type dwarf and of a compact object with strong magnetic

       field, characterized by variable linear and circular polarization

       of light. The total range of light variations may reach 4-5 mag V.



R      Close binary systems characterized by the presence of strong

       reflection (re-radiation) of the light of the hot star

       illuminating the surface of the cooler companion.  Light curves

       are sinusoidal with the period equal to Porb, maximum brightness

       coinciding with the passage of the hot star in front of the

       companion.  The eclipse may be absent.  The range of light

       variation is about 0.5-1.0mag V (KV Vel).



BE     It becomes more and more clear that, although the majority of Be

       stars are photometrically variable, not all of them could be

       properly called GCAS variables.  Quite a number of them show

       small-scale variations not necessarily related to shell events; in

       some cases the variations are quasi-periodic.  By now we are not

       able to present an elaborated system of classification for Be

       variables, but we adopt a decision that in the cases when a Be

       variable cannot be readily described as a GCAS star we give simply

       BE for the type of variability.



EP     Stars showing eclipses by their planets. Prototype: V0376 Peg.



SRS    Semiregular pulsating red giants with short period (several days

       to month), probably high-overtone pulsators. Prototype: AU Ari.



LPB    For comparatively long-period pulsating B stars (periods exceeding

(LBV)  one day).



BLBOO  The so-called "anomalous Cepheids", i.e. stars with periods

       characteristic of comparatively long-period RRAB variables, but

       considerably brighter by luminosity (BL Boo = NGC 5466 V19).





                       1. Eruptive Variable Stars



       Eruptive variables are stars varying in brightness because of

       violent processes and flares occurring in their chromospheres

       and coronae. The light changes are usually accompanied by shell

       events or mass outflow in the form of stellar winds of variable

       intensity and/or by interaction with the surrounding interstellar

       medium. This class includes the following types:



FU     Orion variables of the FU Orionis type. Characterized by

       gradual increases in brightness by about 6 mag in several months,

       followed by either almost complete constancy at maximum that is

       sustained for long periods of time or slow decline by 1-2 mag.

       Spectral types at maximum are in the range Ae(alpha) - Gpe(alpha).

       After an outburst, a gradual development of an emission spectrum

       is observed and the spectral type becomes later. These variables

       probably mark one of the evolutionary stages of T Tauri-type Orion

       variables (INT), as evidenced by an outburst of one member, V1057

       Cyg, but its decline (2.5 mag in 11 years) commenced immediately

       after maximum brightness was attained. All presently known FU Ori

       variables are coupled with reflecting cometary nebulae.



GCAS   Eruptive irregular variables of the Gamma Cas type. These

       are rapidly rotating B III-IVe stars with mass outflow from their

       equatorial zones. The formation of equatorial rings or disks is

       often accompanied by temporary fading. Light amplitudes may reach

       1.5 mag in V.



I      Poorly studied irregular variables with unknown features of light

       variations and spectral types. This is a very inhomogeneous group

       of objects.



IA     Poorly studied irregular variables of early (O-A) spectral type.



IB     Poorly studied irregular variables of intermediate (F-G) to

       late (K-M) spectral type.



IN     Orion variables. Irregular, eruptive variables connected with

       bright or dark diffuse nebulae or observed in the regions of these

       nebulae. Some of them may show cyclic light variations caused by

       axial rotation. In the Spectrum-Luminosity diagram, they are

       found in the area of the main sequence and subgiants. They are

       probably young objects that, during the course of further

       evolution, will become light-constant stars on the zero-age main

       sequence (ZAMS). The range of brightness variations may reach

       several magnitudes. In the case of rapid light variations having

       been observed (up to 1 mag in 1-10 days), the letter "S" is added

       to the symbol for the type (INS). This type may be divided into

       the following subtypes:



INA    Orion variables of early spectral types (B-A or Ae). They are often

       characterized by occasional abrupt Algol-like fadings (T Ori);



INB    Orion variables of intermediate and late spectral types, F-M or

       Fe-Me (BH Cep, AH Ori). F-type stars may show Algol-like fadings

       similar to those of many INA stars; K-M stars may produce flares

       along with irregular light variations;



INT,IT Orion variables of the T Tauri type. Stars are assigned to

       this type on the basis of the following (purely spectroscopic)

       criteria:  spectral types are in the range Fe-Me. The spectra of

       most typical stars resemble the spectrum of the solar

       chromosphere. The feature specific to the type is the presence of

       the flourescent emission lines Fe II 4046, 4132 A (anomalously

       intense in the spectra of these stars), emission lines [Si II] and

       [O I], as well as the absorption line Li I 6707 A. These variables

       are usually observed only in diffuse nebulae. If it is not

       apparent that the star is associated with a nebula, the letter "N"

       in the symbol for the type may be omitted, e.g., IT (RW AUR);



IN(YY) Some Orion variables (YY Ori) show the presence of absorption

       components on the redward sides of emission lines, indicating the

       infall of matter toward the stars' surfaces. In such cases, the

       symbol for the type may be accompanied by the symbol "YY".



IS     Rapid irregular variables having no apparent connection with diffuse

       nebulae and showing light changes of about 0.5 - 1.0 mag within

       several hours or days. There is no strict boundary between rapid

       irregular and Orion variables. If a rapid irregular star is

       observed in the region of a diffuse nebula, it is considered an

       Orion variable and designated by the symbol INS. To attribute

       a variable to the IS type, it is necessary to take much care to be

       certain that its light changes are really not periodic. Quite a

       number of the stars assigned to this type in the third edition of

       the GCVS turned out to be eclipsing binary systems, RR Lyrae

       variables, and even extragalactic BL Lac objects.



ISA    Rapid irregular variables of the early spectral types, B-A or Ae;



ISB    Rapid irregular variables of the intermediate and late spectral

       types, F-M and Fe-Me.



RCB    Variables of the R Coronae Borealis type. These are hydrogen-poor,

       carbon- and helium-rich, high-luminosity stars belonging to the

       spectral types Bpe-R, which are simultaneously eruptive and

       pulsating variables. They show slow nonperiodic fadings by 1-9

       mag in V lasting from a month or more to several hundred days.

       These changes are superposed on cyclic pulsations with amplitudes

       up to several tenths of a magnitude and periods in the range

       30-100 days.



RS     Eruptive variables of the RS Canum Venaticorum type. This type is

       ascribed to close binary systems with spectra showing Ca II H and

       K in emission, their components having enhanced chromospheric

       activity that causes quasi-periodic light variability. The period

       of variation is close to the orbital one, and the variability

       amplitude is usually as great as 0.2 mag in V (UX Ari). They are

       X-ray sources and rotating variables. RS CVn itself is also an

       eclipsing system (see below).



SDOR   Variables of the S Doradus type. These are eruptive,

       high-luminosity Bpec-Fpec stars showing irregular (sometimes

       cyclic) light changes with amplitudes in the range 1-7 mag in V.

       They belong to the brightest blue stars of their parent galaxies.

       As a rule, these stars are connected with diffuse nebulae and

       surrounded by expanding envelopes (P Cyg, Eta Car).



UV     Eruptive variables of the UV Ceti type, these are K Ve-M Ve stars

       sometimes displaying flare activity with amplitudes from

       several tenths of a magnitude up to 6 mag in V. The amplitude is

       considerably greater in the ultraviolet spectral region. Maximum

       light is attained in several seconds or dozens of seconds after

       the beginning of a flare; the star returns to its normal

       brightness in several minutes or dozens of minutes.



UVN    Flaring Orion variables of spectral types Ke-Me. These are

       phenomenologically almost identical to UV Cet variables observed

       in the solar neighborhood. In addition to being related to

       nebulae, they are normally characterized by being of earlier

       spectral type and greater luminosity, with slower development of

       flares (V389 Ori). They are possibly a specific subgroup of INB

       variables with irregular variations superimposed by flares.



WR     Eruptive Wolf-Rayet variables. Stars with broad emission features

       of He I and He II as well as C II-C IV, O II-O IV, and N III-N V.

       They display irregular light changes with amplitudes up to 0.1 mag

       in V, which are probably caused by physical processes, in

       particular, by nonstable mass outflow from their atmospheres.



                          2. Pulsating Variable Stars



       Pulsating variables are stars showing periodic expansion and

       contraction of their surface layers. The pulsations may be radial

       or nonradial. A radially pulsating star remains spherical in

       shape, while in the case of nonradial pulsations the star's shape

       periodically deviates from a sphere, and even neighboring zones of

       its surface may have opposite pulsation phases.



       Depending on the period value, on the mass and evolutionary status

       of the star, and on the scale of pulsational phenomena, the

       following types of pulsating variables may be distinguished:



ACYG   Variables of the Alpha Cygni type, which are nonradially pulsating

       supergiants of Bep-AepIa spectral types. The light changes with

       amplitudes of the order of 0.1 mag often seem irregular, being

       caused by the superposition of many oscillations with close

       periods. Cycles from several days to several weeks are observed.



BCEP   Variables of the Beta Cephei type (Beta Cep, Beta CMa), which are

       pulsating O8-B6 I-V stars with periods of light and

       radial-velocity variations in the range of 0.1 - 0.6 days and light

       amplitudes from 0.01 to 0.3 mag in V. The light curves are similar

       in shape to average radial-velocity curves but lag in phase by a

       quarter of the period, so that maximum brightness corresponds to

       maximum contraction, i.e., to minimum stellar radius. The

       majority of these stars probably show radial pulsations, but some

       (V649 Per) display nonradial pulsations; multiperiodicity is

       characteristic of many of these stars.



BCEPS  A short-period group of Beta Cep variables. The spectral types are

       B2-B3 IV-V; periods and light amplitudes are in the ranges 0.02 -

       0.04 days and 0.015 - 0.025 days, respectively, i.e., an order of

       magnitude smaller than the normally observed ones.



CEP    Cepheids. Radially pulsating, high luminosity (classes Ib-II) vari-

       ables with periods in the range of 1-135 days and amplitudes from

       several hundredths to 2 mag in V (in the B band, the amplitudes

       are greater). Spectral type at maximum light is F; at minimum,

       the types are G-K. The longer the period of light variation,

       the later is the spectral type. The maximum of the surface-layer

       expansion velocity almost coinciding with maximum light.



CEP(B) Cepheids (TU Cas, V 367 Sct) displaying the presence of two or

       more simultaneously operating pulsation modes (usually the

       fundamental tone with the period P0 and the first overtone P1).

       The periods P0 are in the range from 2 to 7 days, with the ratio

       P1/P0 approx. 0.71.



CW     Variables of the W Virginis type. These are pulsating variables of

       the galactic spherical component (old disk) population with

       periods of approximately 0.8 to 35 days and amplitudes from 0.3 to

       1.2 mag in V. They obey a period-luminosity relation different

       from that for Delta Cep variables (see DCEP). For an equal period

       value, the W Vir variables are fainter than the Delta Cep stars by

       0.7 - 2 mag. The light curves of W Vir variables for some period

       intervals differ from those of Delta Cep variables for

       corresponding periods either by amplitudes or by the presence of

       humps on their descending branches, sometimes turning into broad

       flat maxima. W Vir variables are present in globular clusters and

       at high galactic latitudes. They may be separated into the

       following subtypes:



CWA    W Vir variables with periods longer than 8 days (W Vir);



CWB    W Vir variables with periods shorter than 8 days (BL Her).



DCEP   These are the classical cepheids, or Delta Cep-type variables. Com-

       paratively young objects that have left the main sequence and

       evolved into the instability strip of the Hertzsprung-Russell

       (H-R) diagram, they obey the well-known Cepheid period-luminosity

       relation and belong to the young disk population. DCEP stars are

       present in open clusters. They display a certain relation between

       the shapes of their light curves and their periods.



DCEPS  These are Delta Cep variables having light amplitudes <0.5 mag in

       V (<0.7 mag in B) and almost symmetrical light curves (M-m

       approx. 0.4 - 0.5 periods); as a rule, their periods do not exceed

       7 days. They are probably first-overtone pulsators and/or are in

       the first transition across the instability strip after leaving

       the main sequence (SU Cas).



       Traditionally, both Delta Cep and W Vir stars are quite often called

       Cepheids because it is often impossible to discriminate between

       them on the basis of the light curves for periods in the range 3 -

       10 days. However, these are distinct groups of entirely different

       objects in different evolutionary stages. One of the significant

       spectral differences between W Vir stars and Cepheids is the

       presence, during a certain phase interval, of hydrogen-line

       emission in the former and of Ca II H and K emission in the

       latter.



DSCT   Variables of the Delta Scuti type. These are pulsating variables of

       spectral types A0-F5 III-V displaying light amplitudes from 0.003

       to 0.9 mag in V (usually several hundredths of a magnitude) and

       periods from 0.01 to 0.2 days. The shapes of the light curves,

       periods, and amplitudes usually vary greatly. Radial as well as

       nonradial pulsations are observed. The variability of some

       members of this type appears sporadically and sometimes completely

       ceases, this being a consequence of strong amplitude modulation

       with the lower value of the amplitude not exceeding 0.001 mag

       in some cases. The maximum of the surface layer expansion does not

       lag behind the maximum light for more than 0.1 periods. DSCT stars are

       representatives of the galactic disk (flat component) and are

       phenomenologically close to the SX Phe variables.



DSCTC  Low amplitude group of Delta Sct variables (light amplitude <0.1

       mag in V). The majority of this type's representatives are stars

       of luminosity class V; objects of this subtype generally are

       representative of the Delta Sct variables in open clusters.



L      Slow irregular variables. The light variations of these stars show no

       evidence of periodicity, or any periodicity present is very poorly

       defined and appears only occasionally. Like for the type I, stars are

       often attributed to this type because of being insufficiently studied.

       Many type L variables are really semiregulars or belong to other types.



LB     Slow irregular variables of late spectral types (K, M, C, S); as a

       rule, they are giants (CO Cyg). This type is also ascribed, in

       the GCVS, to slow red irregular variables in the case of unknown

       spectral types and luminosities.



LC     Irregular variable supergiants of late spectral types having amplitudes

       of about 1 mag in V (TZ Cas).



M      Mira (Omicron) Ceti-type variables. These are long-period variable

       giants with characteristic late-type emission spectra (Me, Ce, Se) and

       light amplitudes from 2.5 to 11 mag in V. Their periodicity is

       well pronounced, and the periods lie in the range between 80 and

       1000 days. Infrared amplitudes are usually less than in the

       visible and may be <2.5 mag. For example, in the K band they

       usually do not exceed 0.9 mag. If the amplitudes exceed 1 - 1.5

       mag , but it is not certain that the true light amplitude exceeds 2.5

       mag, the symbol "M" is followed by a colon, or the star is

       attributed to the semiregular class with a colon following the

       symbol for that type (SR).



PVTEL  Variables of the PV Telescopii type. These are helium supergiant

       Bp stars with weak hydrogen lines and enhanced lines of He and C.

       They pulsate with periods of approximately 0.1 to 1 days, or vary

       in brightness with an amplitude of 0.1 mag in V during a time

       interval of about a year.



RR     Variables of the RR Lyrae type, which are radially-pulsating giant A-F

       stars having amplitudes from 0.2 to 2 mag in V. Cases of variable

       light-curve shapes as well as variable periods are known. If

       these changes are periodic, they are called the "Blazhko effect."



       Traditionally, RR Lyrae stars are sometimes called short-period

       Cepheids or cluster-type variables. The majority of these stars belong

       to the spherical component of the Galaxy; they are present, sometimes in

       large numbers, in some globular clusters, where they are known as

       pulsating horizontal-branch stars. Like Cepheids, maximum

       expansion velocities of surface layers for these stars practically

       coincide with maximum light.



RR(B)  RR Lyrae variables showing two simultaneously operating pulsation

       modes, the fundamental tone with the period P0 and the first

       overtone, P1 (AQ Leo). The ratio P1/P0 is approximately 0.745;



RRAB   RR Lyrae variables with asymmetric light curves (steep ascending

       branches), periods from 0.3 to 1.2 days, and amplitudes from 0.5

       to 2 mag in V;



RRC    RR Lyrae variables with nearly symmetric, sometimes sinusoidal, light

       curves, periods from 0.2 to 0.5 days, and amplitudes not greater

       than 0.8 mag in V (SX UMa).



RV     Variables of the RV Tauri type. These are radially pulsating

       supergiants having spectral types F-G at maximum light and K-M at

       minimum. The light curves are characterized by the presence of

       double waves with alternating primary and secondary minima that

       can vary in depth so that primary minima may become secondary and

       vice versa. The complete light amplitude may reach 3-4 mag in V.

       Periods between two adjacent primary minima (usually called formal

       periods) lie in the range 30-150 days (these are the periods

       appearing in the Catalogue). Two subtypes, RVA and RVB, are

       recognized:



RVA    RV Tauri variables that do not vary in mean magnitude (AC Her);



RVB    RV Tauri variables that periodically (with periods from 600 to

       1500 days and amplitudes up to 2 mag in V) vary in mean

       magnitude (DF Cyg, RV Tau).



SR     Semiregular variables, which are giants or supergiants of intermediate

       and late spectral types showing noticeable periodicity in their

       light changes, accompanied or sometimes interrupted by various

       irregularities. Periods lie in the range from 20 to >2000 days,

       while the shapes of the light curves are rather different and

       variable, and the amplitudes may be from several hundredths to

       several magnitudes (usually 1-2 mag in V).



SRA    Semiregular late-type (M, C, S or Me, Ce, Se) giants displaying

       persistent periodicity and usually small (<2.5 mag in V) light

       amplitudes (Z Aqr). Amplitudes and light-curve shapes generally

       vary and periods are in the range of 35-1200 days. Many of these

       stars differ from Miras only by showing smaller light amplitudes;



SRB    Semiregular late-type (M, C, S or Me, Ce, Se) giants with poorly

       defined periodicity (mean cycles in the range of 20 to 2300 days)

       or with  alternating intervals of periodic and slow irregular changes,

       and even with light constancy intervals (RR CrB, AF Cyg). Every star

       of this type may usually be assigned a certain mean period

       (cycle), which is the value given in the Catalogue. In a number

       of cases, the simultaneous presence of two or more periods of

       light variation is observed;



SRC    Semiregular late-type (M, C, S or Me, Ce, Se) supergiants (Mu Cep) with

       amplitudes of about 1 mag and periods of light variation from 30 days to

       several thousand days;



SRD    Semiregular variable giants and supergiants of F, G, or K spectral

       types, sometimes with emission lines in their spectra. Amplitudes

       of light variation are in the range from 0.1 to 4 mag, and the range of

       periods is from 30 to 1100 days (SX Her, SV UMa).



SXPHE  Phenomenologically, these resemble DSCT (Delta Sct) variables and

       are pulsating subdwarfs of the spherical component, or old disk

       galactic population, with spectral types in the range A2-F5. They

       may show several simultaneous periods of oscillation, generally in

       the range 0.04-0.08 days, with variable-amplitude light changes

       that may reach 0.7 mag in V. These stars are present in globular

       clusters.



ZZ     ZZ Ceti variables. These are nonradially pulsating white dwarfs that

       change their brightnesses with periods from 30 s to 25 min and

       amplitudes from 0.001 to 0.2 mag in V. They usually show several

       close period values. Flares of 1 mag are sometimes observed;

       however, these may be explained by the presence of close UV Ceti

       companions.



       These variables are divided into the following subtypes:



ZZA    ZZ Cet-type variables of DA spectral type (ZZ Cet) having only

       hydrogen absorption lines in their spectra;



ZZB    ZZ Cet-type variables of DB spectral type having only helium

       absorption lines in their spectra.



                           3. Rotating Variable Stars



       Variable stars with nonuniform surface brightness and/or

       ellipsoidal shapes, whose variability is caused by axial rotation

       with respect to the observer. The nonuniformity of surface

       brightness distributions may be caused by the presence of spots or

       by some thermal or chemical inhomogeneity of the atmosphere caused

       by a magnetic field whose axis is not coincident with the rotation

       axis. These stars are subdivided into the following types:



ACV    Alpha2 Canum Venaticorum variables. These are main-sequence stars

       with spectral types B8p-A7p and displaying strong magnetic fields.

       Spectra show abnormally strong lines of Si, Sr, Cr, and rare

       earths whose intensities vary with rotation. They exhibit magnetic

       field and brightness changes (periods of 0.5-160 days or more). The

       amplitudes of the brightness changes are usually withine 0.01-0.1 mag

       in V.



ACVO   Rapidly oscillating Alpha2 CVn variables. These are nonradially

       pulsating, rotating magnetic variables of Ap spectral type (DO

       Eri). Pulsation periods are in the range of 6-12 mmag (0.004-0.01

       days), while amplitudes of light variation caused by the pulsation

       are about 0.01 mag in V. The pulsational variations are superposed

       on those caused by rotation.



BY     BY Draconis-type variables, which are emission-line dwarfs of dKe-dMe

       spectral type showing quasiperiodic light changes with periods

       from a fraction of a day to 120 days and amplitudes from several

       hundredths to 0.5 mag in V. The light variability is caused by

       axial rotation of a star with a variable degree of nonuniformity

       of the surface brightness (spots) and chromospheric activity.

       Some of these stars also show flares similar to those of UV Cet

       stars, and in those cases they also belong to the latter type and

       are simultaneously considered eruptive variables.



ELL    Rotating ellipsoidal variables (b Per, Alpha Vir). These are close

       binary systems with ellipsoidal components, which change combined

       brightnesses with periods equal to those of orbital motion because

       of changes in emitting areas toward an observer, but showing no

       eclipses. Light amplitudes do not exceed 0.1 mag in V.



FKCOM  FK Comae Berenices-type variables. These are rapidly rotating

       giants with nonuniform surface brightnesses, which have G-K spectral

       types with broad H and K Ca II emission and sometimes Halpha.

       They may also be spectroscopic binary systems. Periods of light

       variation (up to several days) are equal to rotational periods,

       and amplitudes are several tenths of a magnitude. It is not

       excluded that these objects are the product of further evolution

       of EW (W UMa) close binary systems (see below).



PSR    Optically variable pulsars (CM Tau), which are rapidly rotating

       neutron stars with strong magnetic fields, radiating in the radio,

       optical, and X-ray regions. Pulsars emit narrow beams of

       radiation, and periods of their light changes coincide with

       rotational periods (from 0.004 to 4 s), while amplitudes of the

       light pulses reach 0.8 mag.



SXARI  SX Arietis-type variables. These are main-sequence B0p-B9p stars

       with variable-intensity He I and Si III lines and magnetic fields.

       They are sometimes called helium variables. Periods of light and

       magnetic field changes (about 1 day) coincide with rotational

       periods, while amplitudes are approximately 0.1 mag in V. These

       stars are high-temperature analogs of the ACV variables.



               4. Cataclysmic (Explosive and Novalike) Variables



       These are variable stars showing outbursts caused by thermonuclear

       burst processes in their surface layers (novae) or deep in their

       interiors (supernovae). We use the term "novalike" for

       variables that show novalike outbursts caused by rapid energy

       release in the surrounding space (UG-type stars - see

       below) and also for objects not displaying outbursts but

       resembling explosive variables at minimum light by their spectral

       (or other) characteristics. The majority of explosive and

       novalike variables are close binary systems, their components

       having strong mutual influence on the evolution of each star. It

       is often observed that the hot dwarf component of the system is

       surrounded by an accretion disk formed by matter lost by the

       other, cooler, and more extended component. This category is

       subdivided into the following types:



N      Novae. Close binary systems with orbital periods from 0.05 to 230

       days. One of the components of these systems is a hot dwarf star

       that suddenly, during a time interval from one to several dozen or

       several hundred days, increases its brightness by 7-19 mag in V,

       then returns gradually to its former brightness over several

       months, years, or decades. Small changes at minimum light may be

       present. Cool components may be giants, subgiants, or dwarfs of

       K-M type. The spectra of novae near maximum light resemble A-F

       absorption spectra of luminous stars at first. Then broad

       emission lines (bands) of hydrogen, helium, and other elements

       with absorption components indicating the presence of a rapidly

       expanding envelope appear in the spectrum. As the light

       decreases, the composite spectrum begins to show forbidden lines

       characteristic of the spectra of gas nebulae excited by hot

       stars. At minimum light, the spectra of novae are generally

       continuous or resemble the spectra of Wolf-Rayet stars. Only

       spectra of the most massive systems show traces of cool

       components.



       Some novae reveal pulsations of hot components with periods of

       approximately 100 s and amplitudes of about 0.05 mag in V after an

       outburst. Some novae eventually turn out to be eclipsing

       systems. According to the features of their light variations,

       novae are subdivided into fast (NA), slow (NB), very slow (NC),

       and recurrent (NR) categories.



NA     Fast novae displaying rapid light increases and then, having achieved

       maximum light, fading by 3 mag in 100 or fewer days (GK Per);



NB     Slow novae that fade after maximum light by 3 mag in >= 150 days (RR

       Pic). Here the presence of the well-known "dip" in the light

       curves of novae similar to T Aur and DQ Her is not taken into

       account:  The rate of fading is estimated on the basis of a smooth

       curve, its parts before and after the "dip" being a direct

       continuation of one another;



NC     Novae with a very slow development and remaining at maximum light for

       more than a decade, then fading very slowly. Before an outburst

       these objects may show long-period light changes with amplitudes

       of 1-2 mag in V (RR Tel); cool components of these systems are

       probably giants or supergiants, sometimes semiregular variables,

       and even Mira variables. Outburst amplitudes may reach 10 mag.

       High excitation emission spectra resemble those of planetary

       nebulae, Wolf-Rayet stars, and symbiotic variables. The

       possibility that these objects are planetary nebulae in the

       process of formation is not excluded;



NL     Novalike variables, which are insufficiently studied objects

       resembling novae by the characteristics of their light changes or

       by spectral features. This type includes, in addition to

       variables showing novalike outbursts, objects with no bursts ever

       observed; the spectra of novalike variables resemble those of old

       novae, and small light changes resemble those typical for old

       novae at minimum light. However, quite often a detailed

       investigation makes it possible to reclassify some representatives

       of this highly inhomogeneous group of objects into other types;



NR     Recurrent novae, which differ from typical novae by the fact that two

       or more outbursts (instead of a single one) separated by 10-80

       years have been observed (T CrB).



SN     Supernovae (B Cas, CM Tau). Stars that increase, as a result of an

       outburst, their brightnesses by 20 mag and more, then fade slowly.

       The spectrum during an outburst is characterized by the presence

       of very broad emission bands, their widths being several times

       greater than those of the bright bands observed in the spectra of

       novae. The expansion velocities of SN envelopes are in the

       thousands of km/s. The structure of a star after outburst alters

       completely. An expanding emission nebula results and a (not

       always observable) pulsar remains at the position of the original

       star. According to the light curve shape and the spectral

       features, supernovae are subdivided into types I and II.



SNI    Type I supernovae. Absorption lines of Ca II, Si, etc., but no

       hydrogen lines are present in the spectra. The expanding envelope

       almost lacks hydrogen. During 20-30 days following maximum light,

       the brightness decreases by approximately 0.1 mag per day, then

       the rate of fading slows and reaches a constant value of

       0.014/day;



SNII   Type II supernovae. Lines of hydrogen and other elements are

       apparent in their spectra. The expanding envelope consists mainly

       of H and He. Light curves show greater diversity than those of

       type I supernovae. Usually after 40-100 days since maximum light,

       the rate of fading is 0.1 mag per day.



UG     U Geminorum-type variables, quite often called dwarf novae. They are

       close binary systems consisting of a dwarf or subgiant K-M star

       that fills the volume of its inner Roche lobe and a white dwarf

       surrounded by an accretion disk. Orbital periods are in the range

       0.05-0.5 days. Usually only small, in some cases rapid, light

       fluctuations are observed, but from time to time the brightness of

       a system increases rapidly by several magnitudes and, after an

       interval of from several days to a month or more, returns to the

       original state. Intervals between two consecutive outbursts for a

       given star may vary greatly, but every star is characterized by a

       certain mean value of these intervals, i.e., a mean cycle that

       corresponds to the mean light amplitude. The longer the cycle,

       the greater the amplitude. These systems are frequently sources

       of X-ray emission. The spectrum of a system at minimum is

       continuous, with broad H and He emission lines. At maximum these

       lines almost disappear or become shallow absorption lines. Some

       of these systems are eclipsing, possibly indicating that the

       primary minimum is caused by the eclipse of a hot spot that

       originates in the accretion disk from the infall of a gaseous

       stream from the K-M star. According to the characteristics of the

       light changes, U Gem variables may be subdivided into three types:

       SS Cyg, SU UMa, and Z Cam.



UGSS   SS Cygni-type variables (SS Cyg, U Gem). They increase in

       brightness by 2-6 mag in V in 1-2 days and in several subsequent

       days return to their original brightnesses. The values of the

       cycle are in the range 10 days to several thousand;



UGSU   SU Ursae Majoris-type variables. These are characterized by the

       presence of two types of outbursts called "normal" and

       "supermaxima". Normal, short outbursts are similar to those of

       UGSS stars, while supermaxima are brighter by 2 mag, are more than

       five times longer (wider), and occur several times less frequently.

       During supermaxima the light curves show superposed periodic

       oscillations (superhumps), their periods being close to the

       orbital ones and amplitudes being about 0.2-0.3 mag in V. Orbital

       periods are shorter than 0.1 days; companions are of dM spectral

       type;



UGZ    Z Camelopardalis-type stars. These also show cyclic outbursts,

       differing from UGSS variables by the fact that sometimes after an

       outburst they do not return to the original brightness, but during

       several cycles retain a magnitude between maximum and minimum.

       The values of cycles are from 10 to 40 days, while light

       amplitudes are from 2 to 5 mag in V.



ZAND   Symbiotic variables of the Z Andromedae type. They are close

       binaries consisting of a hot star, a star of late type, and an

       extended envelope excited by the hot star's radiation. The

       combined brightness displays irregular variations with amplitudes

       up to 4 mag in V. A very inhomogeneous group of objects.



                       5. Close Binary Eclipsing Systems



       We adopt a triple system of classifying eclipsing binary systems:

       according to the shape of the combined light curve, as well as to

       physical and evolutionary characteristics of their components.

       The classification based on light curves is simple, traditional,

       and suits the observers; the second and third classification

       methods take into account positions of the binary-system

       components in the (MV ,B-V) diagram and the degree of inner Roche

       lobe filling. Estimates are made by applying the simple criteria

       proposed by Svechnikov and Istomin (1979). The symbols for the

       types of eclipsing binary systems that we use are given below.



            a) Classification based on the shape of the light curve



E      Eclipsing binary systems. These are binary systems with orbital planes

       so close to the observer's line of sight (the inclination i of the

       orbital plane to the plane orthogonal to the line of sight is

       close to 90 deg) that the components periodically eclipse each other.

       Consequently, the observer finds changes of the apparent combined

       brightness of the system with the period coincident with that of the

       components' orbital motion.



EA     Algol (Beta Persei)-type eclipsing systems. Binaries with spherical

       or slightly ellipsoidal components. It is possible to specify, for

       their light curves, the moments of the beginning and end of the

       eclipses. Between eclipses the light remains almost constant or

       varies insignificantly because of reflection effects, slight

       ellipsoidality of components, or physical variations. Secondary

       minima may be absent. An extremely wide range of periods is

       observed, from 0.2 to >= 10000 days. Light amplitudes are also

       quite different and may reach several magnitudes.



EB     Beta Lyrae-type eclipsing systems. These are eclipsing systems having

       ellipsoidal components and light curves for which it is impossible

       to specify the exact times of onset and end of eclipses because of

       a continuous change of a system's apparent combined brightness

       between eclipses; secondary minimum is observed in all cases, its

       depth usually being considerably smaller than that of the primary

       minimum; periods are mainly longer than 1 day. The components

       generally belong to early spectral types (B-A). Light amplitudes

       are usually <2 mag in V.



EW     W Ursae Majoris-type eclipsing variables. These are eclipsers with

       periods shorter than 1 days, consisting of ellipsoidal components

       almost in contact and having light curves for which it is

       impossible to specify the exact times of onset and end of

       eclipses. The depths of the primary and secondary minima are

       almost equal or differ insignificantly. Light amplitudes are

       usually <0.8 mag in V. The components generally belong to

       spectral types F-G and later.



            b) Classification according to the components' physical

                                characteristics



GS     Systems with one or both giant and supergiant components; one of the

       components may be a main sequence star.



PN     Systems having, among their components, nuclei of planetary nebulae

       (UU Sge).



RS     RS Canum Venaticorum-type systems. A significant property of these

       systems is the presence in their spectra of strong Ca II H and K

       emission lines of variable intensity, indicating increased

       chromospheric activity of the solar type. These systems are also

       characterized by the presence of radio and X-ray emission. Some

       have light curves that exhibit quasi sine waves outside eclipses,

       with amplitudes and positions changing slowly with time. The

       presence of this wave (often called a distortion wave) is

       explained by differential rotation of the star, its surface being

       covered with groups of spots; the period of the rotation of a spot

       group is usually close to the period of orbital motion (period of

       eclipses) but still differs from it, which is the reason for the

       slow change (migration) of the phases of the distortion wave

       minimum and maximum in the mean light curve. The variability of

       the wave's amplitude (which may be up to 0.2 mag in V) is

       explained by the existence of a long-period stellar activity cycle

       similar to the 11-year solar activity cycle, during which the

       number and total area of spots on the star's surface vary.



WD     Systems with white-dwarf components.



WR     Systems having Wolf-Rayet stars among their components (V 444 Cyg).



        c) Classification based on the degree of filling of inner Roche

                                     lobes



AR     Detached systems of the AR Lacertae type. Both components are

       subgiants not filling their inner equipotential surfaces.



D      Detached systems, with components not filling their inner Roche lobes.



DM     Detached main-sequence systems. Both components are main-sequence

       stars and do not fill their inner Roche lobes.



DS     Detached systems with a subgiant. The subgiant also does not fill its

       inner critical surface.



DW     Systems similar to W UMa systems in physical properties (KW, see

       below), but not in contact.



K      Contact systems, both components filling their inner critical surfaces.



KE     Contact systems of early (O-A) spectral type, both components being

       close in size to their inner critical surfaces.



KW     Contact systems of the W UMa type, with ellipsoidal components of F0-K

       spectral type. Primary components are main-sequence stars and

       secondaries lie below and to the left of the main sequence in the

       (MV,B-V) diagram.



SD     Semidetached systems in which the surface of the less massive com-

       ponent is close to its inner Roche lobe.



       The combination of the above three classification systems for

       eclipsers results in the assignment of multiple classifications

       for object types. These are separated by a solidus ("/") in the

       data field. Examples are:  E/DM, EA/DS/RS, EB/WR, EW/KW, etc.



         6. Optically Variable Close Binary Sources of Strong, Variable

                        X-ray Radiation (X-ray Sources)



X      Close binary systems that are sources of strong, variable X-ray emis-

       sion and which do not belong to or are not yet attributed to any

       of the above types of variable stars. One of the components of

       the system is a hot compact object (white dwarf, neutron star, or

       possibly a black hole). X-ray emission originates from the infall

       of matter onto the compact object or onto an accretion disk

       surrounding the compact object. In turn, the X-ray emission is

       incident upon the atmosphere of the cooler companion of the

       compact object and is reradiated in the form of optical

       high-temperature radiation (reflection effect), thus making that

       area of the cooler companion's surface an earlier spectral type.

       These effects lead to quite a peculiar complex character of

       optical variability in such systems. These objects may be

       subdivided into the following types:



XB     X-ray bursters. Close binary systems showing X-ray and optical

       bursts, their duration being from several seconds to ten minutes,

       with amplitudes of about 0.1 mag in V (V 801 Ara, V 926 Sco);



XF     Fluctuating X-ray systems showing rapid variations of X-ray (Cygnus

       X-1 = V1357 Cyg) and optical (V821 Ara) radiation on time scales

       of dozens of milliseconds;



XI     X-ray irregulars. Close binary systems consisting of a hot compact

       object surrounded by an accretion disk and a dA - dM-type dwarf.

       These display irregular light changes on time scales of minutes

       and hours, and amplitudes of about 1 mag in V. Superposition of a

       periodic variation because of orbital motion is possible (V818

       Sco);



XJ     X-ray binaries characterized by the presence of relativistic jets

       evident at X-ray and radio wavelengths, as well as in the optical

       spectrum in the form of emission components showing periodic

       displacements with relativistic velocities (V1343 Aql);



XND    X-ray, novalike (transient) systems containing, along with a hot

       compact object, a dwarf or subgiant of G-M spectral type. These

       systems occasionally rapidly increase in brightness by 4-9 mag

       in V, in the visible simultaneously with the X-ray range, with no

       envelope ejected. The duration of the outburst may be up to

       several months (V616 Mon);



XNG    X-ray, novalike (transient) systems with an early-type supergiant or

       giant primary component and a hot compact object as a companion.

       Following the main component's outburst, the material ejected by

       it falls onto the compact object and causes, with a significant

       delay, the appearance of X rays. The amplitudes are about 1-2 mag

       in V (V725 Tau);



XP     X-ray pulsar systems. The primary component is usually an ellipsoidal

       early-type supergiant. The reflection effect is very small and

       light variability is mainly caused by the ellipsoidal primary

       component's rotation. Periods of light changes are between 1 and

       10 days; the period of the pulsar in the system is from 1 s to 100

       min. Light amplitudes usually do not exceed several tenths of a

       magnitude (Vela X-1 = GP Vel);



XPR    X-ray pulsar systems featuring the presence of the reflection effect.

       They consist of a dB-dF-type primary and an X-ray pulsar, which

       may also be an optical pulsar. The mean light of the system is

       brightest when the primary component is irradiated by X rays; it

       is faintest during a low state of the X-ray source. The total

       light amplitude may reach 2-3 mag in V (HZ Her);



XPRM,  X-ray systems consisting of a late-type dwarf (dK-dM) and a pulsar

XM     with a strong magnetic field. Matter accretion on the compact

       object's magnetic poles is accompanied by the appearance of

       variable linear and circular polarization; hence, these systems

       are sometimes known as "polars". The amplitudes of the light

       changes are usually about 1 mag in V but, provided that the

       primary component is irradiated by X rays, the mean brightness of

       a system may increase by 3 mag in V. The total light amplitude may

       reach 4-5 mag in V (AM Her, AN UMa).



       If the beam of X-ray emission originating at the magnetic poles of

       the rotating hot compact object does not pass through the

       observer's position and the system is not observed as a pulsar,

       the letter "P" in the above symbols for X-ray- system types is not

       used. If an X-ray system is also an eclipsing or an ellipsoidal

       variable, the X-ray symbol is preceded by "E" or "ELL" joined with

       the X-ray symbol by a "+" sign (e.g., E+X, ELL+X).



                            7. Other Symbols



       In addition to the variable-star types described above, certain

       other symbols that need to be explained will be found in the

       Type data field:



BLLAC  Extragalactic BL Lacertae-type objects. These are compact

       quasistellar objects showing almost continuous spectra with weak

       emission and absorption lines and relatively rapid irregular light

       changes with amplitudes up to 3 mag in V or more. Sources of

       strong X-ray radiation and radio waves, their emission displays

       strong and variable linear polarization in the visible and

       infrared spectral regions. Some objects of this type, considered

       erroneously to be variable stars and designated in the GCVS

       system, will probably sometimes be included in the main table of

       the Catalogue in the future, too.



CST    Nonvariable stars, formerly suspected to be variable and hastily

       designated. Further observations have not confirmed their

       variability.



GAL    Optically variable quasistellar extragalactic objects (active

       galactic nuclei [AGNs]) considered to be variable stars by

       mistake.



L:     Unstudied variable stars with slow light changes.



QSO    Optically variable quasistellar extragalactic sources (quasars) that

       earlier were erroneously considered to be variable stars.



S      Unstudied variable stars with rapid light changes.



*      Unique variable stars outside the range of the classifications de-

       scribed above. These probably represent either short stages of

       transition from one variability type to another or the earliest

       and latest evolutionary stages of these types, or they are

       insufficiently studied members of future new types of variables.



+      If a variable star belongs to several types of light variability

       simultaneously, the types are joined in the Type field by a "+"

       sign (e.g., E+UG, UV+BY).





       II.  Distribution Statistics of Designated Variable Stars

                According to their Types of Variability

                    (GCVS I-III and NL 67 - 77).

    Type      Numb. Stars

|          |     525

|*         |      70

|ACV       |     330

|ACV+DSCT: |       1

|ACV+DSCTC |       1

|ACV:      |      81

|ACVO      |      31

|ACVO:     |       3

|ACYG      |      59

|ACYG:     |      62

|AM        |      11

|AM/XRM+E  |       1

|AM:       |       3

|BCEP      |      95

|BCEP(B)   |       2

|BCEP+E    |       1

|BCEP+E:   |       4

|BCEP+EA/D |       1

|BCEP+ELL: |       1

|BCEP:     |      36

|BCEPS     |       3

|BE        |     193

|BE:       |      43

|BLLAC     |       4

|BY        |     259

|BY+UV     |      14

|BY+UV:    |       1

|BY:       |     138

|BY:+E:    |       1

|CEP       |     125

|CEP(B)    |      14

|CEP:      |      48

|CST       |      69

|CST:      |      88

|CW:       |       2

|CWA       |      95

|CWA:      |      18

|CWB       |      50

|CWB:      |      16

|DCEP      |     458

|DCEP(B)   |       1

|DCEP:     |       9

|DCEPS     |      47

|DCEPS(B)  |       1

|DCEPS:    |       3

|DSCT      |     108

|DSCT(B)   |       1

|DSCT(B:)  |       1

|DSCT:     |      26

|DSCTC     |     289

|DSCTC(B)  |       1

|DSCTC+E   |       1

|DSCTC+E:  |       1

|DSCTC+ELL |       1

|DSCTC:    |      42

|E         |     497

|E+ACYG+XP |       1

|E+AM      |       1

|E+AM:     |       1

|E+BE      |       1

|E+IS:     |       1

|E+LPB:    |       1

|E+NC      |       1

|E+NL      |       3

|E+UG      |       1

|E+UV      |       3

|E+WR      |       1

|E+X       |       2

|E+XI      |       1

|E+XJ      |       1

|E+XM      |       5

|E+XP      |       1

|E+XPM     |       1

|E+XPRM    |       1

|E+XR      |       1

|E+XRM     |       1

|E/D       |       5

|E/D/WR    |       1

|E/D:      |       1

|E/DM      |       9

|E/DM:     |       1

|E/DS      |       4

|E/DS:     |       4

|E/DW      |       2

|E/GS+GCAS |       1

|E/KE      |       9

|E/KE:     |       1

|E/KW      |       1

|E/KW:     |       9

|E/PSR     |       1

|E/RS      |       6

|E/RS:     |       1

|E/SD      |      79

|E/SD:     |     101

|E/WD      |       1

|E/WD+NL   |       1

|E/WR      |       3

|E/WR+E:   |       1

|E:        |     274

|E:+DSCTC: |       1

|E:+NL     |       1

|E:+SXARI  |       1

|E:/GS     |       1

|E:/GS+SR  |       1

|E:/GS:    |       1

|E:/PN     |       1

|E:/RS     |       2

|E:/RS:    |       2

|E:/SD:    |       6

|E:/WR     |       5

|EA        |    1181

|EA+ACV:   |       1

|EA+ACYG   |       1

|EA+BCEP:  |       1

|EA+DSCT   |       2

|EA+DSCT:  |       1

|EA+DSCTC  |       2

|EA+NL     |       2

|EA+NL:    |       1

|EA+RPHS   |       1

|EA+UG:    |       1

|EA+UGSU:  |       1

|EA+UV+BY  |       1

|EA+XM     |       1

|EA+ZAND   |       1

|EA/AR     |       6

|EA/AR/RS  |       8

|EA/AR:    |       6

|EA/AR:/RS |       2

|EA/D      |     114

|EA/D+BY   |       1

|EA/D/RS   |       6

|EA/D/RS+X |       1

|EA/D/WD   |       1

|EA/D/WR   |       1

|EA/D:     |      16

|EA/D:/PN  |       1

|EA/D:/RS  |       1

|EA/D:/RS: |       1

|EA/DM     |     252

|EA/DM+ACV:|       1

|EA/DM+UV  |       1

|EA/DM/RS  |       2

|EA/DM:    |      40

|EA/DS     |     136

|EA/DS/RS  |       3

|EA/DS:    |      39

|EA/DW     |       7

|EA/DW/RS  |       2

|EA/DW/RS: |       1

|EA/DW:    |       1

|EA/GS     |      27

|EA/GS+SR  |       1

|EA/GS+SRC |       1

|EA/GS+ZAND|       1

|EA/GS/D   |       5

|EA/GS/RS  |       4

|EA/GS/RS: |       1

|EA/GS/WD  |       1

|EA/GS:    |      12

|EA/K:     |       2

|EA/KE     |      45

|EA/KE:    |      64

|EA/KW     |       1

|EA/KW:    |       1

|EA/PN     |       1

|EA/RS     |       7

|EA/RS:    |       4

|EA/SD     |     979

|EA/SD/RS  |       3

|EA/SD/RS: |       1

|EA/SD:    |     397

|EA/WD     |       2

|EA/WD+NL  |       4

|EA/WD+NL: |       1

|EA/WR     |       4

|EA:       |     115

|EA:/GS    |       1

|EA:/PN    |       1

|EA:/SD    |       1

|EA:/SD:   |       4

|EB        |     306

|EB/AR     |       3

|EB/AR/RS  |       1

|EB/AR:    |       3

|EB/D      |      15

|EB/D/GS   |       1

|EB/D:     |       5

|EB/DM     |      70

|EB/DM/WR  |       1

|EB/DM:    |      11

|EB/DS     |       4

|EB/DW     |       7

|EB/DW/RS  |       1

|EB/DW:    |       1

|EB/GS     |      13

|EB/GS+ACYG|       1

|EB/GS+SRD |       1

|EB/GS/D   |       1

|EB/GS/K   |       1

|EB/GS/RS  |       1

|EB/GS/SD: |       1

|EB/GS:    |       1

|EB/K      |       2

|EB/K:     |       1

|EB/KE     |     171

|EB/KE:    |      33

|EB/KW     |      10

|EB/KW:    |       6

|EB/SD     |      51

|EB/SD:    |      28

|EB/WR     |       1

|EB:       |      69

|EB:/D:    |       1

|EB:/DM    |       1

|EB:/DM:   |       1

|EB:/DS:   |       1

|EB:/GS    |       1

|EB:/GS:   |       1

|EB:/KE    |       2

|EB:/KE:   |       3

|EB:/KW:   |       1

|EB:/SD    |       2

|ELL       |      49

|ELL+BCEP  |       1

|ELL+BCEP: |       2

|ELL+E:    |       1

|ELL+RS    |       1

|ELL+X     |       1

|ELL+XF    |       1

|ELL+XP    |       1

|ELL+XPNG: |       1

|ELL/DM    |       2

|ELL/DW:   |       1

|ELL/KE    |       1

|ELL/PN    |       1

|ELL/RS    |       1

|ELL/WR+*  |       1

|ELL:      |      63

|ELL:+BCEP |       1

|ELL:+NL:  |       1

|ELL:+WR   |       1

|EP        |       1

|EW        |     309

|EW  :     |       1

|EW/D      |       1

|EW/D:     |       1

|EW/DM     |       1

|EW/DM:    |       2

|EW/DW     |      15

|EW/DW/RS  |       1

|EW/DW:    |       6

|EW/K      |       4

|EW/KE     |      67

|EW/KE:    |      21

|EW/KW     |     357

|EW/KW/RS  |       1

|EW/KW:    |       8

|EW/SD:    |       2

|EW:       |      77

|EW:/KE    |       3

|EW:/KE:   |       6

|EW:/KW    |       4

|EW:/KW:   |       9

|FKCOM     |       9

|FKCOM:    |       5

|FU        |       4

|FU:       |       8

|GAL       |       8

|GAL:      |       1

|GCAS      |     121

|GCAS+BCEP |       1

|GCAS+ELL  |       1

|GCAS+UV:  |       1

|GCAS+XP   |       1

|GCAS:     |      35

|GCAS:+XP  |       1

|GDOR      |      12

|GDOR:     |      10

|I         |     171

|I:        |      47

|IA        |      33

|IA:       |      23

|IB        |       7

|IB:       |      10

|IN        |     460

|IN(YY)    |       3

|IN:       |      66

|INA       |      61

|INA:      |       3

|INAT      |       1

|INB       |     163

|INB+BY    |       1

|INB:      |       7

|INS       |     261

|INS:      |      96

|INSA      |      16

|INSA:     |       3

|INSB      |     105

|INSB(YY)  |       2

|INSB:     |       6

|INST      |      44

|INST(YY)  |      10

|INT       |     126

|INT(YY)   |       7

|INT:      |       3

|IS        |      58

|IS:       |      88

|ISA       |      12

|ISA(YY)   |       1

|ISA:      |      11

|ISB       |      30

|ISB:      |      27

|IT        |      55

|IT:       |       3

|L         |     585

|L:        |     157

|LB        |    1907

|LB+E:     |       1

|LB:       |     979

|LBV       |       1

|LBV:      |       3

|LC        |      84

|LC+E:     |       1

|LC:       |      21

|LPB       |      95

|LPB:      |      40

|M         |    6004

|M+NB:     |       1

|M+ZAND    |       1

|M:        |    1237

|N         |      50

|N+UG:+EA  |       1

|N:        |      29

|NA        |     140

|NA+E+X    |       1

|NA+E:     |       1

|NA+EA     |       2

|NA+XP     |       1

|NA:       |       5

|NAB       |       1

|NB        |      37

|NB+EA     |       2

|NB:       |       1

|NC        |       6

|NC+M      |       2

|NC:       |       3

|NL        |      67

|NL+E      |       1

|NL+EA+X   |       1

|NL+X      |       2

|NL+ZZ:    |       2

|NL:       |      19

|NR        |       6

|NR:       |       2

|PSR       |       1

|PVTEL     |      11

|PVTEL:    |       3

|QSO       |       6

|R         |       7

|R/PN      |       1

|R:        |       2

|R:+E:     |       1

|R:/PN     |       1

|RCB       |      28

|RCB:      |      14

|RPHS      |      21

|RPHS+ELL  |       1

|RR        |    1524

|RR(B)     |       5

|RR:       |     318

|RRA       |       1

|RRAB      |    4352

|RRAB:     |      29

|RRC       |     449

|RRC:      |      63

|RS        |     132

|RS+DSCT:  |       1

|RS+E      |       1

|RS:       |      41

|RV        |      43

|RV:       |      47

|RVA       |      24

|RVB       |      14

|RVB+EA    |       1

|RVB:      |       1

|S:        |     183

|SDOR      |      13

|SDOR:     |       6

|SN        |       2

|SN+PSR    |       1

|SNI       |       3

|SNI:      |       1

|SR        |    1266

|SR+ZAND   |       1

|SR:       |    1341

|SR:+E     |       1

|SRA       |     934

|SRA+EA    |       1

|SRA:      |      36

|SRB       |    1193

|SRB:      |     189

|SRC       |      61

|SRC:      |      11

|SRD       |     150

|SRD+E:    |       1

|SRD+EA    |       1

|SRD:      |      62

|SRS       |       8

|SRS:      |       2

|SXARI     |      23

|SXARI:    |      10

|SXPHE     |      13

|SXPHE(B)  |       2

|SXPHE:    |      11

|UG        |     142

|UG+E      |       2

|UG+EA     |       1

|UG:       |      87

|UG:+E     |       1

|UG:+EW/WD |       1

|UGSS      |      81

|UGSS+E    |       1

|UGSS+E/WD |       1

|UGSS+EA   |       1

|UGSS+XM   |       1

|UGSS+ZZ:  |       1

|UGSU      |      31

|UGSU+E    |       4

|UGSU+E+ZZ |       1

|UGSU+EA   |       1

|UGSU:     |       7

|UGSU:+E   |       1

|UGZ       |      27

|UGZ+E     |       1

|UGZ+ZZ    |       1

|UGZ:      |      14

|UV        |    1001

|UV+BY     |      13

|UV+BY:    |       5

|UV:       |      29

|UVN       |     533

|UVN(YY)   |       1

|UVN:      |      16

|WR        |      32

|X         |       2

|X+BE      |       1

|X+E       |       1

|XB        |       7

|XB+E:     |       1

|XBI       |       1

|XBN+E     |       1

|XBND      |       1

|XBP       |       1

|XBPR      |       1

|XF        |       1

|XFND      |       1

|XFPNG     |       1

|XI        |       7

|XI+E:     |       1

|XI+RS     |       1

|XM        |      30

|XM+E      |       2

|XM+EA     |       2

|XN        |       4

|XN+XP     |       1

|XND       |       9

|XND+E:    |       1

|XND+ELL   |       1

|XND+ELL:  |       2

|XNDB      |       1

|XNDR+E:   |       1

|XNG       |       1

|XNGP      |       2

|XP        |       8

|XP:       |       1

|XPM       |       3

|XPM+ELL   |       1

|XPR       |       3

|XPR+E     |       1

|XRM+E     |       1

|ZAND      |      37

|ZAND+E    |       1

|ZAND+M    |       1

|ZAND+SR   |       1

|ZAND:     |      19

|ZZ        |       7

|ZZ+UV:    |       1

|ZZ:       |       2

|ZZA       |      34

|ZZB       |       9

|ZZB:      |       1

|ZZO       |       8

---------------------

 Total         38624

========================================================================

(End)  N.N. Samus [Moscow Inst. Astron.], O.V. Durlevich [Sternberg

Astron. Inst., Moscow] 16-Feb-2004

