FF Aqr DW Period is significantly greater than typical value for DW type. According to Pojmanski [45] this star is DCEP-FU: variable. According to Sipahi et al. [263] it is one of the few binary systems which consists of the hot subdwarf and cool chromospherically active giant components. According to Marilli et al. [264] it is one of the peculiar system which is defined as pre-cataclysmic binaries or pre-symbiotics. HM Aqr Post-AGB Star (proto-PN). V803 Aql CWA System with A1>0.75, consists of two almost identical components (Samec et al. [278]). TT Aur SH A1 is larger than 0.6, the system lies near line of equal radii. According to Ozdemir et al. [491] TT Aur is a special example of a close eclipsing binary system consisting of a pair of young and massive stars with almost equal radii. CQ Aur DR Small A1 and large period. Belongs to long-period RS CVn systems, secondary is more massive and more larger (volume of the secondary is approximately 100 times larger than that of the primary component). Primary is the hotter one. According to Popper [492] sp. type of system is F5+K1 if both components are the MS stars, but according to Kang [388] both components are the subgiants. eps Aur Such a long periods have only DGlate type systems but their secondary spectra lies in range G8-M2, the enigmatic binary. At least a part of other DGL systems are classified as being similar to eps Aur. SS Boo DR Inverse DR system (Montesinos et al. [493]) RR Cae DW Pre-cataclysmic system (see Bruch [494]), A1 is greater than 3. Post-common-envelope binary according to Parsons et al. [495]. RZ Cnc DR Inverse DR system (Montesinos et al. [493]) UU Cnc Semidetached system consisting of a K4 giant which fills its Roche lobe and unseen primary, obscured by the optically thick accretion disk (see Zola et al. [496]). Active interacting algol binary (like W Cru). But period of the system is not suitable for SA systems (as for W Cru!). AC Cnc S2C Too large A2. According to Hoard [110] and Downes et al. [90] the system is probable member of the NL type variable group of SW Sex or UX UMa type. The main part of GCVS gives max=13.80 and minI=15.40 in V, but in remarks file of GCVS brightness in maximum and secondary minimum equal to 14.5 and 14.7 respectively. Thus value of A2 equals to 0.9 if one uses maximum brightness from main part of GCVS or A2 equals 0.2 for maximum brightness given in remarks file. Yamasaki et al. [146] have pointed out to out-of-eclipse light variations. Range of variations of the maximum brightness reaches 0.5 mag. According to data from Yamasaki et al. [146] and Shugarov [147] the mean value of maximum brightness equals to 14.5 and then A2 has a normal value. Too early Sp2 (usually Sp2>=M) ES Cnc DR Only one DR system with such small values of A1 and period. But according to Yakut et al. [540] eclipses are partial. Additionally system is a hierarchical triple in which all three are blue stragglers. HR CMa Because of its period may belong to DGlate only, but K0III must be assigned to secondary and A1 is smaller than needed. Barium star, so secondary may be the WD. V415 Car DGL A1 is lower than typical value for DGL class. The eclipse is partial with the hotter secondary grazing the polar region of the primary, so A1 is small. The A star position is consistent with the model tracks on HRD, the evolved G-star primary is substantially too luminous and too blue to lie on the predicted model track (Brown et al.[436]). V429 Car Because of its spectra may belong only to DGearly systems, but has longer period (periods for DGearly is shorter than 35 days). Eccentric. See Parkin & Gosset [434] for details. RX Cas SA Belongs to W Ser type star, "active algol", according to GCVS textual remarks 9.12<=Min II<=9.49 and this was confirmed by Djurasevic [245]. We think it is rather SA because of long period. SX Cas SA Belongs to W Ser type star, "active algol". AZ Cas Because of its very long period may belong to DGlate class only, if secondary spectra is later than G3. According to Podsiadlowski [497] is VV Cep variable. It is Interesting and probable marginal system. del Cas Long period is suitable for DGlate only, but not amplitudes and lum. class of secondary. According to Rhee et al. [498] infrared excess is registered by IRAS. According to Hovhannessian & Hovhannessian [499] is a "Vega-type" disk system. CQ Cep DG WR binary, the shortest period among known such systems. Very asymmetric eclipses, wind-wind interaction. According to Demircan et al. [214] (based on lc solution) system is overcontact, and is member of OB1 Cep association. EK Cep DM Too large A1, far from line M for DM systems (see Fig.1 in Malkov et al. [324]). According to Popper [144] the radius and luminosity of the secondary components are enlarged in comparison with the MS star. Popper suggested the pre-MS status for this system. Later Marques et al. [260] have confirmed the pre-MS nature of the low mass secondary component of EK Cep. GP Cep S Is a quadruple system, consisting of WN6o/WCE+O3-6 and B0:I+B1:V-III Demers et al. [347], why it is S? Both pairs are eclipsing with P=6.6884 and P=3.4696. KR Com CWA Amplitudes are small compared to other CWA system. Star is classified as CWA according to the Zasche1 & Uhlar [372], triple alf CrB DM The only one eclipsing binary in the CEV with two MS stars with such large temperature difference between two components (~B9 and G5 for primary and secondary respectively)! One of the widest eclipsing binaries with detached MS components. Large eccentricity of the orbit also points to unevolved status of the system. Binary is onserved as X-ray source because of activity of G5 secondary. W Cru Belongs to active algols and has the longest period among the group of W Ser binaries. So may be SA system? CG Cyg DR Inverse DR system (Montesinos et al. [493]) CI Cyg D2S D2S have Sp1 around O, but CI Cyg has Bep type for hotter component (according to CEV and GCVS). CI Cyg is a symbiotic system, according to Kenyon et al. [155] secondary is a MS star (usually secondary star is white dwarf) with accretion disk. But according to Siviero et al. [153] secondary is rather WD star because the accretion disk around MS star would not be able to account for the outburst states of CI Cyg. So secondary spectral type in now known properly. V380 Cyg DG Both spectra are earlier than B. Apsidal motion! The system consists of an evolved massive primary with a mass of 11.1 and a secondary which is still close to the ZAMS and has a mass of 6.95. WW Dra DR Inverse DR system (Montesinos et al. [493]) CM Dra DM BY Dra variable, low mass and radius, compatible spectra and periods, is chromospherically and flare active. DE Dra DM Primary rotates much faster than synchronous rate, relatively young and unevolved system. RZ Eri DR Long-period RS CVn system. According to Vivekananda Rao et al. [500] the primary is the hotter and more massive, but smaller (Rh=2.84, Mbolh=1.35, mh=1.69, Rc=6.94, Mbolc=1.41 and mc=1.63) so it may be the inverse DR system (like Z Her), but there is a solution with q greater than unity too. So status is unclear? According to Vivekananda Rao et al. [500] spectra is F0IV+G5-G8III-IV. Also there is circumstellar envelope or shell around the system because IR excess was detected. Spectra differs from those of other DR systems. TZ For DG Two components with almost equal masses (1.95+2.05), but different radius: the hotter F star is smaller (about 4R), G star is greater (about 8.2R) and more massive. The rotation of the larger star is synchronized with orbital motion, while smaller star rotates much faster. Orbit is circular. Both components have evolved well from the MS, chromospherically active, but not RS CVn type. According to Bisikalo et al. [501] it is long-period RS CVn? Primary (more massive) is in the core helium burning phase, but secondary is near the "red hook". YY Gem DM BY Dra variable, low mass and radius, compatible spectra and periods, is chromospherically and flare active; YY Gem also is one of the most flare active star. OW Gem DGL OW Gem consists of two supergiants and was classified as DG system but, according to GCVS data and ASAS-3 light curve, it has an extreme value of the phase of secondary minima (0.23P) which points to the high eccentricity of the orbit. System consists of two stars with quite different masses. Terrell et al. [351] have noted that if the two stars were formed together both cannot possibly be in the red giant stage. Also significant mass transfer is ruled out by very small relative radii of stars and the very large orbital eccentricity. Eggleton [502] proposed a suggestion that OW Gem is a former triple system with the primary having formed from the merger of a close binary. But the merger product might be expected to have rapid rotation, and although the primary star does appear to be rotating faster than the pseudosynchronous rate, it is not unusually rapid. Primary could have undergone a G/K supergiant stage just after the merger and had substantial momentum removed by stellar wind and magnetic braking angular during a period of enhanced activity. This hypothesis needs to be tested. V1003 Her CB Rucinski et al.[284] based on RV curve shown that binary is most likely the W UMa type but for full description high-precision photometry is required, later Deb & Singh [343] have classified it as CB system based on solution of ASAS light curve. They derived very low inclination (about 42 deg) and temperature difference is around 2000K while dA is almost 0!. So it is rather near-contact system with low inclination AR Lac DR Inverse DR system (Montesinos et al. [493]) FL Lyr DM System with solar like components, detached. There are a few solar type binaries due to selection effects. AR Mon DR Inverse DR system (Montesinos et al. [493]) V505 Mon Marginal system, interacting algol with circumbinary matter and disk. See Mayer et al. [503] for details. BM Ori DM Possible pre-ms system V1016 Ori Period is not suitable for any of the classes (but very close to DGlate values). Spectra in CEV is appropriate for DGlate too, but secondary spectra is A0V (Vitrichenko & Plachinda [504]), is the secondary a pre-MS star (Lloyd & Stickland [505])? Like BM Ori? AR Pav D2S Too large A1. ASAS-3 gives max=11.0, minI=13.0, minII=max in V filter (not in CEV till). Values in GCVS are too large (about 6 mag for A1). According to Skopal et al. [506] "AR Pav is an eclipsing symbiotic binary with an orbital period of 605 days. It consists of a M5 III giant with a mass of ~2 M{sun}. The nature of the hot companion is under discussion. The presence of a large accretion disk around a main sequence star was suggested by several authors (see cites inside Skopal et al. [506]), but, in contrast, Schild et al. [508] considered a possibility that the hot component is a white dwarf and the red giant underfills its Roche lobe. According to the observed variations in the UV/optical continuum, the hot eclipsed object is highly variable in brightness, size and geometry". In Skopal et al. [507] from light curve one can see, that in active state magnitude range is about [10-13], in quiet phase mag range is about [10.3-13]. More observations are needed? V718 Per May belong to DGlate class only because of its very long period, but spectra is needed to be determined properly. According to Grinin et al. [437] eclipses are caused by large variable amounts of circumstellar dust. Grinin et al. have suggested that V718 Per is pre-MS post-T Tau single star. Deleted from CEV DV Psc Active RS CVn system, detached according to LC solution of Zhang et al. [509], so may be DR, but has very short period for DR class, lc is asymmetric like for CBV class, but period is shorter than typical CBV value. May be classified as CB, but secondary spectra is needed. According to Zhang & Zhang [510] is near-contact system. See [510] for details. Marginal and interesting system. TY Pyx DR A2 is too large for DR class. A2 almost equals to A1. According to Rao & Sarma [511] it is a unique member of RS CVn group with both components having the same mass, radii, temperature, luminosity and pre-MS contraction phase. V Sge S2C Too large A1, is novalike variable and prototype for small group of V Sge subtype NL variables Steiner [512]. Authors denoted V617 Sgr, DI Cru, WX Cen as NLV variables also. The three later systems are not eclipsing. UU Sge DW Too large A2 and A1 is greater than 3, lies far from other DW systems. UU Sge is the nucleus of planetary nebula Abell 63 and thus post-CE binary. According to Afsar & Ibanoglu [261] radius and temperature of the secondary component are larger than those expected for MS star of the same mass. Derived limb darkening coefficients of the secondary corresponds to a temperature about 10000K. Perhaps the large value of A2 is due the reflection effect and overheated face of the secondary. V5112 Sgr Very long period is not suitable for any of the classes, in VSX is denoted as PPN variable. Post-AGB Star (proto-PN) according to Arkhipova et al. [513] (and references within). Spectra is uncertain, binarity is not proved, and it is only a suggestion. See Arkhipova et al. for details V5158 Sgr According to Torres et al. [82] system is a hierarchical triple system composed of a slightly evolved F6 star (the brighter object) near the end of its MS phase and an eclipsing binary with a K7-M0V star orbiting an F4V star. mu Sgr Very long period is not suitable for any of classes with such early spectra (DGearly, SH, CE, CG). Kondo et al. [514]: P Cyg variable profiles, a mass flow from the primary through inner Lagrangian point, interaction of this material with stellar wind of the secondary and is lost from a system. Marginal. But why period is long? ups Sgr System is the brightest member of the type of extremely hydrogen-deficient stars (HdB).The HdB stars are a rather rare class of evolved binary systems that are in a second phase of mass transfer where the primary has ended the core-helium burning phase. Dusty circumstellar disk is presented. See Netolicky et al. [515] for details. V453 Sco DG A2 is larger than 0.3. Josephs et al. [516]: "From the orbital period, light curve, evidence of circumstellar gas, and faintness of the mass gainer all suggest that HD 163181 is related to the W Ser class of massive interacting binaries". Not DG? BB Scl DM According to Watson et al. [248] it is visual triple system HD9770, consists of A+B and C components. A is of K1V type and possible binary and B is eclipsing binary system of BY Dra type with both stars are low mass and radius (~0.7) and chromospherically active. They also noted that period of binary is not typical for BY Dra systems and shorter then usual. RZ Sct SH A1>1. According to Wilson et al. [517] it is a double-contact system. This fact was confirmed by Olson & Etzel [518]. The primary star (gainer) rapidly rotates. V411 Ser May belong to DGearly, but lum. class of secondary differs from limits for other DGearlies (all have lum. class III-V). According to Conti et al. [519] systems is evolved and on its way to becoming WR system, both components well away from ZAMS. e is about 0.5 from radial curves. RW Tau SA Too large A1. May belong to W Ser type stars (Plavec & Dobias [273]). BE UMa DW Period is greater than 1d. Young pre-cataclysmic variable (Shimanskii et al. [197]). Strong reflection effect. Liebert et al. [520] discovered a rarefied shell with a radius of r approx 1.5 pc in the field of BE UMa. This shell, which is the remnant of a planetary nebula, confirms the evolutionary similarity of the system to other young pre-cataclysmic variables, but suggests a relatively old age. GK Vir DW A1 is greater than 3 (about 6). Post-common-envelope binary according to Parsons et al. [2010arXiv1005.3958P]. QS Vir DW A1 is greater than 3. Post-common-envelope binary according to Parsons et al. [495]. Z Vul SH A1>1., the system lies near R line (see Fig.1 in Malkov et al. [324]). According to Pojmanski [45] A1=1.22 and smaller than CEV gives, A2 equals to 0.34 and then system will lay below R line. According to Lazaro et al. [521] it is Sd system with two components of almost equal radii. Primary (gainer, more massive, hotter and larger) rotates faster than synchronous.