V802 Aql CWA Classified as CWW by Samec [2004IBVS.5527....1S], V802 Aql CWA secondary spectra is later than usual. V1713 Aql System will belong to CB or CW if subdwarf are V1713 Aql components of these classes. There is no individual V1713 Aql investigations. Confirmation of spectra is needed. V883 Ara Period is not suitable for any of the classes, there V883 Ara is no individual investigations, system is V883 Ara chemically peculiar and on eccentric orbit. IQ Cam DW The spectral type of secondary is earlier than for IQ Cam DW for other DW. IQ Cam is one of the best SN Ia IQ Cam DW progenitor candidates known today. Eclipsing nature IQ Cam DW is not known exactly. AD Cap SC There is no enough data to classify this system AD Cap SC properly. Pojmanski [93] gives magnitude range 9.65 AD Cap SC (0.33) in V band and minII=minI (ASAS-3 light curve). AD Cap SC This values are smaller than for other SC systems, AD Cap SC and period is smaller as compared with other SC. AD Cap SC Also in Antonopoulou [1987A&AS...68..521A] spectral AD Cap SC type is equals to K4V+K5V.AD Cap is chromospheric AD Cap SC active system of RS CVn type. More observations and AD Cap SC investigations are needed. AO Cas CE Too large P for CE systems, possible it is a CG AO Cas CE system, but too small A1 in this case. Ell AO Cas CE configuration is possible. In most studies the AO Cas CE system is found to be a semidetached and the primary AO Cas CE while less massive is more luminous than secondary. AO Cas CE According to Gies & Wiggs [1991ApJ...375..321G] and AO Cas CE Bagnuolo & Gies [1991ApJ...376..266B] the system AO Cas CE is semidetached, less massive secondary is subgiant AO Cas CE which fills its Roche lobe and more massive primary AO Cas CE is a MS star and doesn't fill its Roche lobe. Then AO Cas CE SH type is more suitable? But too early Sp2 for AO Cas CE typical SH type. V570 Cas A1 is large, may belong to SA, but all SA have EA or V570 Cas EB light curves, not E:. Period is given according V570 Cas to Alfonso-Garzon etal. [2012arXiv1210.0821A], but as V570 Cas can be seen, their light curve is very strange and V570 Cas does not resemble ones for eclipsing variables. So V570 Cas eclipsing nature must be confirmed firstly. V731 Cas S2C P is larger than for other S2C systems (<=0.25d for V731 Cas S2C others except V Sge which has period bout 0.5d). V731 Cas S2C According to Downes et al. [90] cataclysmic status V731 Cas S2C is uncertain. More investigations are needed. V741 Cas May belong to SA class, but primary spectra is some V741 Cas early, for SC both spectra is not appropriate. V741 Cas According to Duemmler et al. [2002A&A...395..885D] V741 Cas system is detached, but primary is close to contact. V741 Cas So is this system in intermediate state? SV Cen CE It is a CE type system rather because of period, SV Cen CE Sp types, masses and luminosity of both stars. But SV Cen CE A1 is large. Magnitudes in CEV agree with values SV Cen CE which are given in GCVS, different investigations SV Cen CE and light curves from VSX. V748 Cen According to van Genderen et al. [1974MNRAS.167..283V] V748 Cen secondary is M4III star, filling its Roche lobe, V748 Cen primary is a hot small star. Probably system is V748 Cen symbiotic and may belong to D2S class, but to know V748 Cen it exactly primary spectra should be determined V748 Cen properly. Also Large A1, is included to list of V748 Cen symbiotic stars of Belczynski et al.[167]. V1133 Cen May be classified as CB only, but luminosity class V1133 Cen for secondaries of CB is IV-V, not III. There is no V1133 Cen publications, so system is needed to be investigated. ZZ Cep DM Too large A1, far from line M for DM systems ZZ Cep DM (see Fig.1 in Malkov et al. 2007, AA 465, 549). The ZZ Cep DM binary is the brigther star of the triple system ZZ Cep DM ADS 16252. Spectral class of the system were ZZ Cep DM derived by Herbig [258]. Analysys of the V light ZZ Cep DM curve was firstly performed by Kandpal & Srivastava ZZ Cep DM [259] and by Cester et al. [142]. The system is ZZ Cep DM detached. Derived absolute dimensions of the ZZ Cep DM secondary component contradicts to spectral type of ZZ Cep DM Herbig. The secondary component lies far above the ZZ Cep DM MS band as would a subgiant star. The nature of the ZZ Cep DM system remains unclear. GO Cyg CB Sp2 is earlier than for other CB systems. GO Cyg CB Near-contact system according to Ulas et al. GO Cyg CB [2012NewA...17..296U], in which the primary GO Cyg CB (massive and hotter) component is slightly greater GO Cyg CB than its Roche lobe, while the cool component GO Cyg CB is slightly smaller than it. GO Cyg is an unevolved GO Cyg CB system with both its components very close to the GO Cyg CB ZAMS. GO Cyg has the most massive components among GO Cyg CB the known CB systems. Light curves are symmetric, so GO Cyg CB it is not CBV system. V729 Cyg CG Was denoted as CB system in old version of CEV and V729 Cyg CG in Csizmadia & Klagyivik [120], but period is V729 Cyg CG greater and spectral type is earlier than for other V729 Cyg CG CB systems. We changed ev. class to CG and spectral V729 Cyg CG type according to Rauw et al.[198]. The masses of V729 Cyg CG the components equal to (38-55)M and (10-15)M for V729 Cyg CG primary and secondary respectively [198]. V1329 Cyg D2S A1 in GCVS and therefore in CEV for B band is around V1329 Cyg D2S 6 mag. According to Chochol et al. V1329 Cyg D2S [1999CoSka..29...31C] magnitude range is around V1329 Cyg D2S 11.7-14.2, so A1=2.5. And mean brightness slowly V1329 Cyg D2S decreases (see their lc). AV Del SA According to Mader et al. [272] it is semidetached AV Del SA system and may belong to SC ev. class. Sp class for AV Del SA secondary is unknown, Sp type for primary equals to AV Del SA F8 and is too early for SC. Also period value, A2 AV Del SA value and mass of the primary (more massive and AV Del SA hotter) are smaller than for other SC systems. AV Del SA There is no chromospherical activity (see [272]) on AV Del SA both light curves and spectra. So SC status is not AV Del SA proofed properly. BI Del DG System is included to the Catalogue of BI Del DG Chromospherically Active Binaries of Eker et al. [50] BI Del DG but without type designation. Spectral type not known BI Del DG exactly, lies with DR systems on the Sp1-logP and BI Del DG A1-A2 planes, differs from other DG systems. May be BI Del DG DR? Need more investigations for confirmation. A1 is BI Del DG larger than 0.75. BV Eri CBF Period is smaller than for other CBF systems. BV Eri CBF According to Gu et al. [1994IBVS.4076....1G] value BV Eri CBF of period is valid. It is CB according to Gu BV Eri CBF [1999A&A...346..437G], light curves resembles the BV Eri CBF CBF ones. So system may be the CBF with the smallest BV Eri CBF period. SV Gem SH Large A1 according to GCVS, but ASAS gives SV Gem SH 10.55-10.62 in V band, and Guilbault et al. SV Gem SH [2001IBVS.5090....1G] and remarks in VSX (by Otero): SV Gem SH it stopped eclipsing around 1940. Reflection SV Gem SH variability with the orbital period is seen in survey SV Gem SH data between 1989 and 2009. Also small amplitude SV Gem SH ellipsoidal variations superposed causing a small SV Gem SH secondary minimum at phase 0.5. Period constant over SV Gem SH the last 102 years. Is system Ell or not eclipsing? V772 Her DM Triple system, see Boyd et al. [1985IBVS.2747....1B] V772 Her DM for details. SZ Hor CWA Large dA, photometric data are right, why it is SZ Hor CWA contact? EB light curve (from ASAS-3), there is no SZ Hor CWA individual investigations. RT Lac SA Too large A2. RT Lac is among the most peculiar RT Lac SA stars of RS CVn type systems. While most of this type RT Lac SA binary has equal-mass components, the RT Lac RT Lac SA components have unequal masses. Ibanoglu et al. [262] RT Lac SA has reported that brightness of the system at three RT Lac SA phases, i.e., mid-primary and quadratures, shows RT Lac SA quasi-periodic changes. The brightness at the primary RT Lac SA eclipse (phase 0.0) shows the largest variation RT Lac SA with a maximum amplitude of about 0.3 mag in the B RT Lac SA and V filter. The light variations at second maximum RT Lac SA (phase 0.75) resemble those at primary eclipse but RT Lac SA with a maximum amplitude of about 0.2 mag, while the RT Lac SA variations at first maximum (phase 0.25) are RT Lac SA generally in the opposite sense, but with a lower RT Lac SA amplitude (about 0.1 mag). In addition, although not RT Lac SA strictly periodic, the average cycle of the light RT Lac SA variations is almost the same for both second RT Lac SA maximum and primary eclipse. Such a significant RT Lac SA out-of-eclipse variations may be lead to large A2 RT Lac SA value. In CEV we use photometric data from [262] RT Lac SA obtained in 1992 because of the smallest difference RT Lac SA Max1-Max2 in that observational period. According to RT Lac SA [262] more massive, smaller and hotter component is RT Lac SA mostly responsible for the change in the light RT Lac SA curve because of its chromospheric activity. More RT Lac SA over Ibanoglu et al. [195] have shown that The less RT Lac SA massive, larger star fills its own lobe. Therefore, RT Lac SA a gas stream from the larger, less massive star to RT Lac SA the more massive one will be expected. It may also RT Lac SA belongs to SC ev. class, but its period is smaller RT Lac SA than for other SC systems. It spectral type is later RT Lac SA than for SA. TT Lyr SH A1 is larger than 2, secondary spectra is K0 (Liao & TT Lyr SH Qian [213]), but why it is SH? V361 Lyr CBV According to Hilditch et al. [114] this star is a V361 Lyr CBV typical CBV system with asymetrical light curve. V361 Lyr CBV More massive and hotter primary fills its Roche V361 Lyr CBV lobe, while cooler and smaller secondary is detached. V361 Lyr CBV However Hilditch stressed out that this system is a V361 Lyr CBV rare because of its small period and significant V361 Lyr CBV difference in eclipse depth as compared with other V361 Lyr CBV CBV binaries. In CEV we use magnitude in secondary V361 Lyr CBV maximum (around 0.75P). IT Nor C Had a CG type in old CEV version, but too low period IT Nor C and late Sp as compared with other CG systems. Value IT Nor C of P is not known exactly. According to VSX P equals IT Nor C to P=1.754145, but in GCVS, [1] and in CEV now IT Nor C P=0.6357943. According to Shaw [1994MmSAI..65...95S] IT Nor C P=0.3509, Sp=A0. According to Brancewicz & Dworak IT Nor C [1980AcA....30..501B] system is semidetached, both IT Nor C components close to fill their Roche lobe. CB? AI Phe DR Period is long for DR class. Don't belong to AI Phe DR long-period RS CVn systems, but active according to AI Phe DR Karatas et al. [125]. VZ Psc CB_CWA P is smaller than for other CB systems. According to VZ Psc CB_CWA Hrivnak et al. [1995ApJ...455..300H] it is an old disk VZ Psc CB_CWA population star, displays exceptionally strong CaII H VZ Psc CB_CWA and K emission lines. Light curve has changed from VZ Psc CB_CWA that of W UMa with minima of equal depths to beta Lyr VZ Psc CB_CWA type with unequal depth. Analysis of light curves VZ Psc CB_CWA shows greatly overcontact configuration with very VZ Psc CB_CWA large temperature difference between components. VZ Psc CB_CWA Therefore components are in geometrical but not in VZ Psc CB_CWA physical contact like other CB systems. Also Hrivnak VZ Psc CB_CWA et al. [1995ApJ...455..300H] has shown that it is VZ Psc CB_CWA possible to solve light curves with hot spot on the VZ Psc CB_CWA secondary component. In this case system is in VZ Psc CB_CWA marginal contact. They have investigated the light VZ Psc CB_CWA curves assymetry and have shown than light curves VZ Psc CB_CWA asymmetric. So system is rather CB system. May VZ Psc CB_CWA belong to CBV class such as V361 Lyr. PW Pup Because of its period may belong to DGlate only, but PW Pup A2 is larger than usual and secondary spectra is too PW Pup early (G-M is typical values). Interacting with Halpha PW Pup emission (Bopp et al. [1991PASP..103..444B]), and PW Pup close to contact (Eggen [1983AJ.....88.1676E]). TZ Pyx Period is not determined properly. Otero [270] and TZ Pyx Dvorak [21] give about P=2.31854, but Kreiner [1] TZ Pyx gives P=1.15928. If later value is correct than light TZ Pyx curve will be of EA type without secondary minimum. TZ Pyx If period is twice longer (as Otero and Dvorak give) TZ Pyx than light curve will be of EA type with primary and TZ Pyx secondary minima of almost equal depth. We use Otero TZ Pyx data in CEV. Otero also pointed out to apsidal motion. TZ Pyx This fact is needed to be proofed. Class of this TZ Pyx system is not known exactly, but Deb & Sing TZ Pyx [2010arXiv1011.2574D] classified binary as detached TZ Pyx (according to the shape of light curves from ASAS-3 TZ Pyx and following the boundary lines of Derekas et al. TZ Pyx [2007ApJ...663..249D]). System looks like DM with TZ Pyx two components of almost equal physical properties TZ Pyx on the A1-A2 plane. More investigations are needed TZ Pyx to determine spectral type and evolutionary class. QR Sge DW Period is larger than for other DW systems, there is QR Sge DW no period value in GCVS and VSX. The fastest runaway QR Sge DW WR star in Galaxy. V5569 Sgr Large A1, it is "iron star" (only two such stars are V5569 Sgr known), consisting of Be with red supergiant V5569 Sgr component. Light curve is strongly variable e.g., see V5569 Sgr Howell et al. [2009PASP..121...16H]: A1 varies from V5569 Sgr 0.7 to 2 mag) V1236 Tau According to Bayless & Orosz [185] is a double-lines V1236 Tau eclipsing binary with two low mass and near identical V1236 Tau components, secondary (less massive) is slightly V1236 Tau enlarged. May belong to DM or DR class? BL Tel DG Too large A1. Out-of-eclipse light variations. The BL Tel DG variability of bright F primary is around 0.2 mag. BL Tel DG A1 changes from year to year. To explain the BL Tel DG variability of color indexes van Genderen BL Tel DG [1983A&A...119..265V ] supposed a cold asymmetric BL Tel DG gas stream but we didn't find any confirmation of BL Tel DG semidetached configuration. BD Tuc According to West et al. [1992MNRAS.254..419W] A1 is BD Tuc about 1.4, A2 is about 0.5, spectra is B0.5V+B4III, BD Tuc system is semidetached. But their data must be BD Tuc confirmed. May belong to SH, but spectra is needed. BD Tuc See also Loudon & Budding [1993Ap&SS.201..287L]. eps UMi For DGearly period is long and spectra is late, for eps UMi DGlate period is short, A1 is large, for SA A1 is eps UMi large. Marginal? LX Vel Is included in list of X-ray massive binaries of Liu LX Vel et al. [2000A&AS..147...25L]. Is S2H system? VV Vir CBV Has been variously classified as a nearcontact system VV Vir CBV by Shaw [1994MmSAI..65...95S], as a contact binary VV Vir CBV by Giuricin et al. [1983A&AS...54..211G], as a Beta VV Vir CBV Lyra (EB) semidetached binary (GCVS) and an RR Lyrae VV Vir CBV by Sandage, [1993AJ....106..703S] variable. VV Vir CBV According to Samec et al. [266] system is VV Vir CBV semidetached with hot stream spot on a secondary VV Vir CBV (less massive, more cooler) component, their light VV Vir CBV curve is asymmetric with Maximum I is being little VV Vir CBV greater than Maximum II. So they classify this VV Vir CBV system as CBV. AG Vir CWA MinII-MinI>0.5 may be the result of mistaken moments AG Vir CWA of minima due to asymmentic light curves (e.g. see AG Vir CWA Michaels [1988IBVS.3202....1M].) According to AG Vir CWA Pribulla et al. [2011AN....332..607] it is rather CWA AG Vir CWA than CB system despite of light curve asymmetry. AG Vir CWA According to Pribulla the secondary minima are AG Vir CWA systematically delayed after phase 0.5.