Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.inasan.rssi.ru/~malkov/CEV/contrad.txt Äàòà èçìåíåíèÿ: Mon Nov 25 14:17:46 2013 Äàòà èíäåêñèðîâàíèÿ: Sat Jun 28 03:52:44 2014 Êîäèðîâêà: IBM-866 Ïîèñêîâûå ñëîâà: magnitude

CN And CWA_CB According to lc from Jassur & Khodadadi [352] it is
a CBV system because of asymmetry (primary
maximum is greater than secondary) and large dA, but
according to lc solution it is CWA overcontact system
with components in poor termal contact. But according
to van Hamme et al. [319] and their lc solution
(with two spots) it is semidetached system with
components in marginal contact, the decreasing period
is consistent with this suggestion (and in this case
mass transfer from more massive primary to less
massive and smaller secondary exists).

EE Aqr CBV___: According to Wronka et al. [320] it is semi-detached
system with more massive primary almost filling its
critical lobe and less massive secondary filling
Roche lobe. there is no any asymmetry on lc, but
minima of different depth. So it may be CB or CBF,
not CBV.

V802 Aql CWA Classified as CWW by Samec et al. [105], secondary
spectra is later than usual.

V1713 Aql System will belong to CB or CW if subdwarf are
components of these classes. There is no individual
investigations. Confirmation of spectra is needed.

V883 Ara Period is not suitable for any of the classes, there
is no individual investigations, system is
chemically peculiar and on eccentric orbit.

TU Boo CWW_CWA The primary minimum of lc is a transit so system may
be classified as A-subtype, but Niarchos et al. [485]
have solved the lc with WD method and have stressed
that some physical characteristics are typical for
W-subtype systems. Moreover, their solution with spots
have given secondary (less massive and smaller) is
being some hotter than primary. This is typical for
W-subtype too. According to Coughlin et al. [354] is
a marginal contact system with both components almost
fill their critical lobes, light curve asymmetric, so
authors use hot spot on the primary to solve light
curves. They supposed the mass transfer from secondary
to primary which is supported by increasing period.
The shape of the lc corresponds to A-subtype, but q is
greater than 0.4 and components are only in marginal
contact like the typical W-subtype system. So it
rather CB of V subclass?

DU Boo CWA___: According to Pribulla et al. [276] to explain both
photometric and spectroscopic observations several
phenomena are required: (i) large heated areas, most
probably on the secondary component and very likely
resulting from the mass and energy ÿìÂow heating the
hemisphere facing the observer around phase 0.25,
(ii) additional matter close to the neck connecting
the component producing òÀÜbumpsòÀÝ in the BFs observed
around the ÿìÁrst quadrature, (iii) streams of matter
most probably approaching the observer before the
primary minimum (making the proÿìÁle of the primary
being wider before the primary minimum), or
(iv) deviations from the Roche model. But the mass
transfer from the more to the less massive component
would result in period decrease in the system which
is not observed. Fill-out factor is large so system
is in deep contact. Their analysis clearly showed that
the complications in DU Boo cannot be explained by
dark/hot surface areas only. In fact, without BFs,
photometry does not require any additional
phenomena. Additional source of light seen in BFs in
DU Boo is visible only around ÿìÁrst quadrature
(phase 0.25) and its RV corresponds to the neck area
connecting the components. In other quadrature the
systems look more like detached or semidetached. So
It may be the CW system. To determine subclass more
investigation are needed.

IQ Cam DW The spectral type of secondary is earlier than for
for other DW. IQ Cam is one of the best SN Ia
progenitor candidates known today. Eclipsing nature
is not known exactly.

AD Cap SC There is no enough data to classify this system
properly. Pojmanski [93] gives magnitude range 9.65
(0.33) in V band and minII=minI (ASAS-3 light curve).
This values are smaller than for other SC systems,
and period is smaller as compared with other SC.
Also in Antonopoulou [397] spectral type is equals to
K4V+K5V.AD Cap is chromospheric active system of
RS CVn type. More observations and investigations
are needed.

AO Cas CE Too large P for CE systems, possible it is a CG
system, but too small A1 in this case. Ell
configuration is possible. In most studies the
system is found to be a semidetached and the primary
while less massive is more luminous than secondary.
According to Gies & Wiggs [321] and
Bagnuolo & Gies [199] the system is semidetached,
less massive secondary is subgiant which fills its
Roche lobe and more massive primary is a MS star and
doesn't fill its Roche lobe. Then SH type is more
suitable? But too early Sp2 for typical SH type.

V570 Cas A1 is large, may belong to SA, but all SA have EA or
EB light curves, not E:. Period is given according
to Alfonso-Garzon et al. [413], but as can be seen,
their light curve is very strange and does not
resemble ones for eclipsing variables. So
eclipsing nature must be confirmed firstly.

V731 Cas S2C P is larger than for other S2C systems (<=0.25d for
others except V Sge which has period bout 0.5d).
According to Downes et al. [90] cataclysmic status
is uncertain. More investigations are needed.

V741 Cas May belong to SA class, but primary spectra is some
early, for SC both spectra is not appropriate.
According to Duemmler et al. [322] system is detached,
but primary is close to contact. So is this system in
intermediate state?

SV Cen CE It is a CE type system rather because of period,
Sp types, masses and luminosity of both stars. But
A1 is large. Magnitudes in CEV agree with values
which are given in GCVS, different investigations
and light curves from VSX.

V748 Cen According to van Genderen et al. [323] secondary is
M4III star, filling its Roche lobe, primary is a hot
small star. Probably system is symbiotic and may
belong to D2S class, but to know it exactly primary
spectra should be determined properly. Also Large A1,
is included to list of symbiotic stars of
Belczynski et al.[167].

V1133 Cen May be classified as CB only, but luminosity class
for secondaries of CB is IV-V, not III. There is no
publications, so system is needed to be investigated.

ZZ Cep DM Too large A1, far from line M for DM systems (see
Fig.1 in Malkov et al. [324]). The binary is the
brigther star of the triple system ADS 16252.
Spectral class of the system were derived by
Herbig [258]. Analysys of the V light curve was
firstly performed by Kandpal & Srivastava [259] and
by Cester et al. [142]. The system is detached.
Derived absolute dimensions of the secondary component
contradicts to spectral type of Herbig. The secondary
component lies far above the MS band as would a
subgiant star. The nature of the system remains
unclear.

BE Cep CWW System was studied recently by Dai et al. [488] who
supposed system to be marginal contact W-type W UMa
binary, while Samec et al. [489] have predicted
near-contact configuration. The dA value (i.e. A1-A2)
is larger than for other CWW systems and spectral type
is unknown.

DY Cet CWA System was classified as A-subtype of U UMa class by
Rucinski et al. [454] based on RV curve, later this
class was confirmed by Deb & Singh [343] (according
to solution of ASAS light curve). But our algorithm
recognizes it as near-contact system because of
late type secondary. Secondary spectra is not
appropriates to CWA configuration but we used data
of Pourbaix et al. [11]. Primary spectra was
determined by [454] based on color indexes and seem
to be right while secondary spectra may be uncorrect.
So data of Pourbaix must be proven.

GO Cyg CB Sp2 is earlier than for other CB systems.
Near-contact system according to Ulas et al. [325],
in which the primary (massive and hotter) component is
slightly greater than its Roche lobe, while the cool
component is slightly smaller than it. GO Cyg is an
unevolved system with both its components very close
to the ZAMS. GO Cyg has the most massive components
among the known CB systems. Light curves are
symmetric, so it is not CBV system.

V729 Cyg CG Was denoted as CB system in old version of CEV and
in Csizmadia & Klagyivik [120], but period is
greater and spectral type is earlier than for other
CB systems. We changed ev. class to CG and spectral
type according to Rauw et al.[198]. The masses of
the components equal to (38-55)M and (10-15)M for
primary and secondary respectively [198].

V1329 Cyg D2S A1 in GCVS and therefore in CEV for B band is around
6 mag. According to Chochol et al. [326] magnitude
range is around 11.7-14.2, so A1=2.5. And mean
brightness slowly decreases (see their lc).

AV Del SA According to Mader et al. [272] it is semidetached
system and may belong to SC ev. class. Sp class for
secondary is unknown, Sp type for primary equals to
F8 and is too early for SC. Also period value, A2
value and mass of the primary (more massive and
hotter) are smaller than for other SC systems.
There is no chromospherical activity (see [272]) on
both light curves and spectra. So SC status is not
proofed properly.

BI Del DG System is included to the Catalogue of
Chromospherically Active Binaries of Eker et al. [50]
but without type designation. Spectral type not known
exactly, lies with DR systems on the Sp1-logP and
A1-A2 planes, differs from other DG systems. May be
DR? Need more investigations for confirmation. A1 is
larger than 0.75.

BV Eri CBF Period is smaller than for other CBF systems.
According to Gu et al. [327] value of period is valid.
It is CB according to Gu [328], light curves resembles
the CBF ones. So system may be the CBF with the
smallest period.

SV Gem SH Large A1 according to GCVS, but ASAS gives
10.55-10.62 in V band, and Guilbault et al. [329] and
remarks in VSX (by Otero): it stopped eclipsing around
1940. Reflection variability with the orbital period
is seen in survey data between 1989 and 2009. Also
small amplitude ellipsoidal variations superposed
causing a small secondary minimum at phase 0.5. Period
constant over the last 102 years. Is system Ell or
not eclipsing?

MT Her CB_S__: Denoted as SA in Shaw [330] but Budding & Murad [331]
have given detached solution of their lc. Why system
is CB?

V772 Her DM Triple system, see Boyd et al. [332] for details.

RS Ind CBF___: Denoted as possible CBF by Shaw [330].
Marton et al. [212] have solved lc for the several
possible configurations, their results partly
support CB configuration.

RY Ind SA_CB CB type is according to Shaw [330], while
Lapasset & Claria [333] have found the system is
semidetached algol-like binary (via Russell & Merrill
method)

RT Lac SA Too large A2. RT Lac is among the most peculiar
stars of RS CVn type systems. While most of this type
binary has equal-mass components, the RT Lac
components have unequal masses. Ibanoglu et al. [262]
has reported that brightness of the system at three
phases, i.e., mid-primary and quadratures, shows
quasi-periodic changes. The brightness at the primary
eclipse (phase 0.0) shows the largest variation
with a maximum amplitude of about 0.3 mag in the B
and V filter. The light variations at second maximum
(phase 0.75) resemble those at primary eclipse but
with a maximum amplitude of about 0.2 mag, while the
variations at first maximum (phase 0.25) are
generally in the opposite sense, but with a lower
amplitude (about 0.1 mag). In addition, although not
strictly periodic, the average cycle of the light
variations is almost the same for both second
maximum and primary eclipse. Such a significant
out-of-eclipse variations may be lead to large A2
value. In CEV we use photometric data from [262]
obtained in 1992 because of the smallest difference
Max1-Max2 in that observational period. According to
[262] more massive, smaller and hotter component is
mostly responsible for the change in the light
curve because of its chromospheric activity. More
over Ibanoglu et al. [195] have shown that The less
massive, larger star fills its own lobe. Therefore,
a gas stream from the larger, less massive star to
the more massive one will be expected. It may also
belongs to SC ev. class, but its period is smaller
than for other SC systems. It spectral type is later
than for SA.

VY Lac SA_CB According to Semeniuk & Kaluzny [299] system is
semidetached, but Shaw [330] have included it in his
list of CB systems

UV Leo CB_DM Giuricin et al. [334] have solved lc and confirmed the
earlier hypotesis about detached status, but have
stressed that the less massive component looks like
more evolved star. Solution of Frederik & Etzel [335]
confirms of detached status with possible magnetic
activity for one of the components, so system may be
the DR? But period is much longer compared to other
DR systems. Looks like typical CB.

RT LMi CWW_CWA Niarchos et al. [336] have classified it as CWW based
on lc solution. Rucinski et al. [301] have derived RV
curve and classified system as CWA. Later
Qian et al. [337] have shown than lc of binary is
variable and primary minimum was an occultation in
1994 while it is a transit in 2003. Based on their lc
system is CWA, but solution of these lc have given
CWW type! Qian et al. have concluded that RT LMi could
not be uniquely assigned a subtype based on
BinnendijkòÀÙs classiÿìÁcation.

RR Lep SA_CB Vyas & Abhyankar [338] have supposed system to be
semi-detached algol-like, but Shaw [330] has included
it in the list of CB systems.

TT Lyr SH A1 is larger than 2, secondary spectra is K0 (Liao &
Qian [213]), but why it is SH?

V361 Lyr CBV According to Hilditch et al. [114] this star is a
typical CBV system with asymetrical light curve.
More massive and hotter primary fills its Roche
lobe, while cooler and smaller secondary is detached.
However Hilditch stressed out that this system is a
rare because of its small period and significant
difference in eclipse depth as compared with other
CBV binaries. In CEV we use magnitude in secondary
maximum (around 0.75P).

IT Nor C Had a CG type in old CEV version, but too low period
and late Sp as compared with other CG systems. Value
of P is not known exactly. According to VSX P equals
to P=1.754145, but in GCVS, [1] and in CEV now
P=0.6357943. According to Shaw [330] P=0.3509, Sp=A0.
According to Brancewicz & Dworak [339] system is
semidetached, both components close to fill their
Roche lobe. CB?

V2610 Oph Tas & Evren [340] have investigated this system based
on light curves and classified it as CWA, but later
Pribulla et al.[286] have pointed out that system is
quadruple and also noted that lc solution of
Tas & Evren is completely inapplicable because of
multiplicity of V2610 Oph. When they have corrected
the observed photometric amplitude for the
contribution of secondary pair, they have obtained the
full amplitude of the binary as 0.41, indicating a
high orbital inclination angle. So new light curve
analysis is needed to classify this system.

FR Ori SA_CB Shaw [330] included it in his list of CB systems,
while detached in Brancewicz & Dworak catalogue [339].
Zakirov [341] has suggested that system is SA with MS
primary and pre-MS secondary filling its critical
obe. One of these hypotesis must be proven.

V357 Peg CWA System was classified as CWA by Rucinski et al. [284]
who have given also primary spectra, this result was
confirmed by Deb & Singh [343] and by
Ekmekci et al. [289] but secondary spectra (G5V)
which is given by Pourbaix et al. [11] is not suitable
for CWA class but for CB only. On the other side
Ekmekci et al. [289] have supposed F3IV spectral type
for secondary. So secondary spectra must be determined
properly to classify V357 Peg.

AI Phe DR Period is long for DR class. Don't belong to
long-period RS CVn systems, but active according to
Karatas et al. [125].

VZ Psc CB_CWA P is smaller than for other CB systems. According to
Hrivnak et al. [203] it is an old disk population
star, displays exceptionally strong CaII H and K
emission lines. Light curve has changed from that of
W UMa with minima of equal depths to beta Lyr type
with unequal depth. Analysis of light curves shows
greatly overcontact configuration with very large
temperature difference between components. Therefore
components are in geometrical but not in physical
contact like other CB systems. Also
Hrivnak et al. [203] has shown that it is possible to
solve light curves with hot spot on the secondary
component. In this case system is in marginal contact.
They have investigated the light curves assymetry and
have shown than light curves asymmetric. So system is
rather CB system. May belong to CBV class such as
V361 Lyr.

PW Pup Because of its period may belong to DGlate only, but
A2 is larger than usual and secondary spectra is too
early (G-M is typical values). Interacting with Halpha
emission (Bopp et al. [455]), and close to contact
(Eggen [456]).

QR Sge DW Period is larger than for other DW systems, there is
no period value in GCVS and VSX. The fastest runaway
WR star in Galaxy.

V5569 Sgr Large A1, it is "iron star" (only two such stars are
known), consisting of Be with red supergiant
component. Light curve is strongly variable e.g., see
Howell et al. [390]: A1 varies from 0.7 to 2 mag)

V1236 Tau According to Bayless & Orosz [185] is a double-lines
eclipsing binary with two low mass and near identical
components, secondary (less massive) is slightly
enlarged. May belong to DM or DR class?

BL Tel DG Too large A1. Out-of-eclipse light variations. The
variability of bright F primary is around 0.2 mag.
A1 changes from year to year. To explain the
variability of color indexes van Genderen [457]
supposed a cold asymmetric gas stream but we didn't
find any confirmation of semidetached configuration.

BD Tuc According to West et al. [458] A1 is about 1.4, A2 is
about 0.5, spectra is B0.5V+B4III, system is
semidetached. But their data must be confirmed. May
belongs to SH, but spectra is needed.
See also Loudon & Budding [459].

eps UMi For DGearly period is long and spectra is late, for
DGlate period is short, A1 is large, for SA A1 is
large. Marginal?

LX Vel Is included in list of X-ray massive binaries of
Liu et al. [460]. Is S2H system?

VV Vir CBV Has been variously classified as a nearcontact system
by Shaw [330], as a contact binary by
Giuricin et al. [461], as a Beta Lyra (EB)
semidetached binary (GCVS) and an RR Lyrae by
Sandage, [95] variable. According to
Samec et al. [266] system is semidetached with hot
stream spot on a secondary (less massive, more cooler)
component, their light curve is asymmetric with MaxI
is being little greater than MaxII. So they classify
this system as CBV.

AG Vir CWA MinII-MinI>0.5 may be the result of mistaken moments
of minima due to asymmentic light curves (e.g. see
Michaels [462].) According to Pribulla et al. [276]
it is rather CWA than CB system despite of light curve
asymmetry. According to Pribulla the secondary minima
are systematically delayed after phase 0.5.

AW Vir CWA_CWW Lapasset et al. [463] based on lc analysys (unspotted
model) have concluded that subtype (A or W) is
undetermined because of nearly equal temperatures of
both components and other reasons, but their best-fit
solution formally corresponds to A-subtype.
While Niarchos et al. [464] have founded (based on
spotted solution) the W-subtype.