EK Cep DM Too large A1, far from line M for DM systems EK Cep DM (see Fig.1 in Malkov et al. 2007, AA 465, 549). EK Cep DM According to Popper [144] the radius and luminosity EK Cep DM of the secondary components are enlarged in EK Cep DM comparison with the MS star. Popper suggested the EK Cep DM pre-MS status for this system. EK Cep DM Later Marques et al. [260] have confirmed the pre-MS EK Cep DM nature of the low mass secondary component of EK Cep. BM Ori DM Possible pre-ms system FF Aqr DW Period is significantly greater than typical value FF Aqr DW for DW type. According to Pojmanski [45] this star FF Aqr DW is DCEP-FU: variable. According to Sipahi et al. [263] FF Aqr DW it is one of the few binary systems which consists of FF Aqr DW the hot subdwarf and cool chromospherically active FF Aqr DW giant components. According to Marilli et al. [264] FF Aqr DW it is one of the peculiar system which is defined as FF Aqr DW pre-cataclysmic binaries or pre-symbiotics. RR Cae DW Pre-cataclysmic system (see Bruch RR Cae DW [1999AJ....117.3031B]), A1 is greater than 3. RR Cae DW Post-common-envelope binary according to RR Cae DW Parsons et al. [2010arXiv1005.3958P]. UU Sge DW Too large A2 and A1 is greater than 3, lies far from UU Sge DW other DW systems. UU Sge is the nucleus of planetary UU Sge DW nebula Abell 63 and thus post-CE binary. According to UU Sge DW Afsar & Ibanoglu [261] radius and temperature of the UU Sge DW secondary component are larger than those expected UU Sge DW for MS star of the same mass. Derived limb darkening UU Sge DW coefficients of the secondary corresponds to a UU Sge DW temperature about 10000K. Perhaps the large value of UU Sge DW A2 is due the reflection effect and overheated face UU Sge DW of the secondary. BE UMa DW Period is greater than 1d. Young pre-cataclysmic BE UMa DW variable (Shimanskii et al. [197]). Strong reflection BE UMa DW effect. Liebert et al. [1995ApJ...441..424L] BE UMa DW discovered a rarefied shell with a radius of r BE UMa DW approx 1.5 pc in the field of BE UMa. This shell, BE UMa DW which is the remnant of a planetary nebula, confirms BE UMa DW the evolutionary similarity of the system to other BE UMa DW young pre-cataclysmic variables, but suggests a BE UMa DW relatively old age. GK Vir DW A1 is greater than 3 (about 6). Post-common-envelope GK Vir DW binary according to Parsons et al. GK Vir DW [2010arXiv1005.3958P]. QS Vir DW A1 is greater than 3. Post-common-envelope binary QS Vir DW according to Parsons et al. [2010arXiv1005.3958P]. CM Dra DM BY Dra variable, low mass and radius, CM Dra DM compatible spectra and periods, is chromospherically CM Dra DM and flare active. YY Gem DM BY Dra variable, low mass and radius, YY Gem DM compatible spectra and periods, is chromospherically YY Gem DM and flare active; YY Gem also is one of the most YY Gem DM flare active star. BB Scl DM According to Watson et al. [248] it is visual triple BB Scl DM system HD9770, consists of A+B and C components. A BB Scl DM is of K1V type and possible binary and B is BB Scl DM eclipsing binary system of BY Dra type with both BB Scl DM stars are low mass and radius (~0.7) and BB Scl DM chromospherically active. They also noted that period BB Scl DM of binary is not typical for BY Dra systems and BB Scl DM shorter then usual. CI Cyg D2S D2S have Sp1 around O, but CI Cyg has Bep type for CI Cyg D2S hotter component (according to CEV and GCVS). CI Cyg CI Cyg D2S is a symbiotic system, according to Kenyon et al. CI Cyg D2S [155] secondary is a MS star (usually secondary star CI Cyg D2S is white dwarf) with accretion disk. But according to CI Cyg D2S Siviero et al. [153] secondary is rather WD star CI Cyg D2S because the accretion disk around MS star would not CI Cyg D2S be able to account for the outburst states of CI Cyg D2S CI Cyg. So secondary spectral type in now known CI Cyg D2S properly. AR Pav D2S Too large A1. ASAS-3 gives max=11.0, minI=13.0, AR Pav D2S minII=max in V filter (not in CEV till). Values in AR Pav D2S GCVS are too large (about 6 mag for A1). According to AR Pav D2S Skopal et al. [2001IBVS.5195....1S] "AR Pav is an AR Pav D2S eclipsing symbiotic binary with an orbital period of AR Pav D2S 605 days (Mayall 1937). It consists of a M5 III giant AR Pav D2S (Murset & Schmid 1999) with a mass of ~2 M{sun} AR Pav D2S (Schild et al. 2001). The nature of the hot companion AR Pav D2S is under discussion. The presence of a large AR Pav D2S accretion disk around a main sequence star was AR Pav D2S suggested by Kenyon & Webbink (1984) and AR Pav D2S Skopal et al. (2000a), but, in contrast, AR Pav D2S Schild et al. (2001) considered a possibility that AR Pav D2S the hot component is a white dwarf and the red AR Pav D2S giant underfills its Roche lobe. According to the AR Pav D2S observed variations in the UV/optical continuum AR Pav D2S (e.g. Schild et al. 2001, Skopal et al. 2000a), the AR Pav D2S hot eclipsed object is highly variable in brightness, AR Pav D2S size and geometry". In Skopal et al. AR Pav D2S [2000CoSka..30...29S] from light curve one can see, AR Pav D2S that in active state magnitude range is about AR Pav D2S [10-13], in quiet phase mag range is about [10.3-13]. AR Pav D2S More observations are needed? RX Cas SA Belongs to W Ser type star, "active algol", RX Cas SA according to GCVS textual remarks 9.12<=Min II<=9.49 RX Cas SA and this was confirmed by Djurasevic RX Cas SA [1993Ap&SS.206..129D]. We think it is rather SA RX Cas SA because of long period. SX Cas SA Belongs to W Ser type star, "active algol". UU Cnc Semidetached system consisting of a K4 giant UU Cnc which fills its Roche lobe and unseen primary, UU Cnc obscured by the optically thick accretion disk UU Cnc (see Zola et al. [1994A&A...285..531Z]). Active UU Cnc interacting algol binary (like W Cru). But period of UU Cnc the system is not suitable for SA systems UU Cnc (as for W Cru!). W Cru Belongs to active algols and has the longest period W Cru among the group of W Ser binaries. So may be SA W Cru system? V505 Mon Marginal system, interacting algol with circumbinary V505 Mon matter and disk. See Mayer et al. V505 Mon [2001A&A...375..434M] for details. V453 Sco DG A2 is larger than 0.3. Josephs et al. V453 Sco DG [2001PASP..113..957J]: "From the orbital period, V453 Sco DG light curve, evidence of circumstellar gas, and V453 Sco DG faintness of the mass gainer all suggest that V453 Sco DG HD 163181 is related to the W Ser class of massive V453 Sco DG interacting binaries". Not DG? RW Tau SA Too large A1. May belong to W Ser type stars RW Tau SA (Plavec & Dobias [273]). CQ Aur DR Small A1 and large period. Belongs to long-period CQ Aur DR RS CVn systems, secondary is more massive and more CQ Aur DR larger (volume of the secondary is approximately CQ Aur DR 100 times larger than that of the primary component). CQ Aur DR Primary is the hotter one. According to Popper CQ Aur DR [1990AJ....100..247P] sp. type of system is F5+K1 if CQ Aur DR both components are the MS stars, but according to CQ Aur DR Kang [1993Ap&SS.201...35K] both components are the CQ Aur DR subgiants. RZ Eri DR Long-period RS CVn system. According to RZ Eri DR Vivekananda Rao et al. [1994JApA...15..165V] the RZ Eri DR primary is the hotter and more massive, but smaller RZ Eri DR (Rh=2.84, Mbolh=1.35, mh=1.69, Rc=6.94, Mbolc=1.41 RZ Eri DR and mc=1.63) so it may be the inverse DR system RZ Eri DR (like Z Her), but there is a solution with q greater RZ Eri DR than unity too. So status is unclear? According to RZ Eri DR Vivekananda Rao et al. [1994JApA...15..165V] RZ Eri DR spectra is F0IV+G5-G8III-IV. Also there is RZ Eri DR circumstellar envelope or shell around the system RZ Eri DR because IR excess was detected. Spectra differs RZ Eri DR from those of other DR systems. TZ For DG Two components with almost equal masses (1.95+2.05), TZ For DG but different radius: the hotter F star is smaller TZ For DG (about 4R), G star is greater (about 8.2R) and more TZ For DG massive. The rotation of the larger star is TZ For DG synchronized with orbital motion, while smaller star TZ For DG rotates much faster. Orbit is circular. Both TZ For DG components have evolved well from the MS, TZ For DG chromospherically active, but not RS CVn type. TZ For DG According to Bisikalo et al. [1999ARep...43..229B] TZ For DG it is long-period RS CVn? Primary (more massive) is in TZ For DG the core helium burning phase, but secondary is near TZ For DG the "red hook". RZ Sct SH A1>1. According to Wilson et al. [1985ApJ...289..748W] RZ Sct SH it is a double-contact system. This fact was confirmed RZ Sct SH by Olson & Etzel [1994AJ....108..262O]. The primary RZ Sct SH star (gainer) rapidly rotates. V803 Aql CWA System with A1>0.75, consists of two almost identical V803 Aql CWA components (Samec et al. [278]). TT Aur SH A1 is larger than 0.6, the system lies near R-line TT Aur SH (see Fig.1 in Malkov et al. 2007, AA 465, 549). TT Aur SH According to Ozdemir et al. [2001PASA...18..151O] TT Aur SH TT Aur is a special example of a close eclipsing TT Aur SH binary system consisting of a pair of young and TT Aur SH massive stars with almost equal radii. TY Pyx DR A2 is too large for DR class. A2 almost equals to A1. TY Pyx DR According to Rao & Sarma [1981AcA....31..107R] it is TY Pyx DR a unique member of RS CVn group with both components TY Pyx DR having the same mass, radii, temperature, luminosity TY Pyx DR and pre-MS contraction phase. Z Vul SH A1>1., the system lies near R line Z Vul SH (see Fig.1 in Malkov et al. 2007, AA 465, 549). Z Vul SH According to Pojmanski [45] A1=1.22 Z Vul SH and smaller than CEV gives, A2 equals to 0.34 Z Vul SH and then system will lay below R line. According to Z Vul SH Lazaro et al. [2009NewA...14..528L] it is Sd system Z Vul SH with two components of almost equal radii. Primary Z Vul SH (gainer, more massive, hotter and larger) rotates Z Vul SH faster than synchronous. SS Boo DR Inverse DR system (Montesinos et al. SS Boo DR [1988MNRAS.232..361M]) CG Cyg DR Inverse DR system (Montesinos et al. CG Cyg DR [1988MNRAS.232..361M]) WW Dra DR Inverse DR system (Montesinos et al. WW Dra DR [1988MNRAS.232..361M]) AR Lac DR Inverse DR system (Montesinos et al. AR Lac DR [1988MNRAS.232..361M]) RZ Cnc DR Inverse DR system (Montesinos et al. RZ Cnc DR [1988MNRAS.232..361M]) AR Mon DR Inverse DR system (Montesinos et al. AR Mon DR [1988MNRAS.232..361M]) AC Cnc S2C Too large A2. According to Hoard [110] and Downes AC Cnc S2C et al. [90] the system is probable member of the NL AC Cnc S2C type variable group of SW Sex or UX UMa type. The AC Cnc S2C main part of GCVS gives max=13.80 and minI=15.40 in V, AC Cnc S2C but in remarks file of GCVS brightness in maximum and AC Cnc S2C secondary minimum equal to 14.5 and 14.7 respectively. AC Cnc S2C Thus value of A2 equals to 0.9 if one uses maximum AC Cnc S2C brightness from main part of GCVS or A2 equals 0.2 for AC Cnc S2C maximum brightness given in remarks file. AC Cnc S2C Yamasaki et al. [146] have pointed out to AC Cnc S2C out-of-eclipse light variations. Range of variations AC Cnc S2C of the maximum brightness reaches 0.5 mag. According AC Cnc S2C to data from Yamasaki et al. [146] and Shugarov [147] AC Cnc S2C the mean value of maximum brightness equals to 14.5 AC Cnc S2C and then A2 has a normal value. Too early Sp2 AC Cnc S2C (usually Sp2>=M) V Sge S2C Too large A1, is novalike variable and prototype for V Sge S2C small group of V Sge subtype NL variables Steiner V Sge S2C [1998PASP..110..276S]. Authors denoted V617 Sgr, V Sge S2C DI Cru, WX Cen as NLV variables also. The three later V Sge S2C systems are not eclipsing. HM Aqr Post-AGB Star (proto-PN). V5112 Sgr Very long period is not suitable for any of the V5112 Sgr classes, in VSX is denoted as PPN variable. V5112 Sgr Post-AGB Star (proto-PN) according to Arkhipova et al. V5112 Sgr [2010AstL...36..269] (and references within). Spectra V5112 Sgr is uncertain, binarity is not proved, and it is only V5112 Sgr a suggestion. See Arkhipova et al. for details del Cas Long period is suitable for DGlate only, but not del Cas amplitudes and lum. class of secondary. According to del Cas Rhee et al. [2007ApJ...660.1556R] infrared excess del Cas is registered by IRAS. According to Hovhannessian & del Cas Hovhannessian [2001Ap.....44..454H] is a "Vega-type" del Cas disk system. ups Sgr System is the brightest member of the type of ups Sgr extremely hydrogen-deficient stars (HdB).The HdB stars ups Sgr are a rather rare class of evolved binary systems ups Sgr that are in a second phase of mass transfer where the ups Sgr primary has ended the core-helium burning phase. Dusty ups Sgr circumstellar disk is presented. See Netolicky et al. ups Sgr [2009A&A...499..827N] for details. eps Aur Such a long periods have only DGlate type systems but eps Aur their secondary spectra lies in range G8-M2, the eps Aur enigmatic binary. At least a part of other DGL systems eps Aur are classified as being similar to eps Aur. HR CMa Because of its period may belong to DGlate only, but HR CMa K0III must be assigned to secondary and A1 is smaller HR CMa than needed. Barium star, so secondary may be the WD. V415 Car DGL A1 is lower than typical value for DGL class. The V415 Car DGL eclipse is partial with the hotter secondary grazing V415 Car DGL the polar region of the primary, so A1 is small. V415 Car DGL The A star position is consistent with the model V415 Car DGL tracks on HRD, the evolved G-star primary is V415 Car DGL substantially too luminous and too blue to lie on the V415 Car DGL predicted model track V415 Car DGL (Brown et al.[2001AJ....122..392B]). V429 Car Because of its spectra may belong only to DGearly V429 Car systems, but has longer period (periods for DGearly V429 Car is shorter than 35 days). Eccentric. See Parkin & V429 Car Gosset [2011A&A...530A.119P] for details. AZ Cas Because of its very long period may belong to DGlate AZ Cas class only, if secondary spectra is later than G3. AZ Cas According to Podsiadlowski [1994MmSAI..65..359P] AZ Cas is VV Cep variable. It is Interesting and probable AZ Cas marginal system. CQ Cep DG WR binary, the shortest period among known such CQ Cep DG systems. Very asymmetric eclipses, wind-wind CQ Cep DG interaction. According to Demircan et al. CQ Cep DG [1997AN....318..267D] (based on lc solution) system is CQ Cep DG overcontact, and is member of OB1 Cep association. GP Cep S Is a quadruple system, consisting of WN6o/WCE+O3-6 and GP Cep S B0:I+B1:V-III Demers et al. [2002ApJ...577..409D], GP Cep S why it is S? Both pairs are eclipsing with P=6.6884 GP Cep S and P=3.4696. KR Com CWA Amplitudes are small compared to other CWA system. KR Com CWA Star is classified as CWA according to the Zasche1 & KR Com CWA Uhlar [2010A&A...519A..78Z], triple V380 Cyg DG Both spectra are earlier than B. Apsidal motion! The V380 Cyg DG system consists of an evolved massive primary with a V380 Cyg DG mass of 11.1 and a secondary which is still close to V380 Cyg DG the ZAMS and has a mass of 6.95. DE Dra DM Primary rotates much faster than synchronous rate, DE Dra DM relatively young and unevolved system. OW Gem DGL OW Gem consists of two supergiants and was classified OW Gem DGL as DG system but, according to GCVS data and ASAS-3 OW Gem DGL light curve, it has an extreme value of the phase of OW Gem DGL secondary minima (0.23P) which points to the high OW Gem DGL eccentricity of the orbit. System consists of two OW Gem DGL stars with quite different masses. Terrell et al. OW Gem DGL [351] have noted that if the two stars were formed OW Gem DGL together both cannot possibly be in the red giant OW Gem DGL stage. Also significant mass transfer is ruled out by OW Gem DGL very small relative radii of stars and the very large OW Gem DGL orbital eccentricity. Eggleton [2002ASPC..279...37E] OW Gem DGL proposed a suggestion that OW Gem is a former triple OW Gem DGL system with the primary having formed from the merger OW Gem DGL of a close binary. But the merger product might be OW Gem DGL expected to have rapid rotation, and although the OW Gem DGL primary star does appear to be rotating faster than OW Gem DGL the pseudosynchronous rate, it is not unusually OW Gem DGL rapid. Primary could have undergone a G/K supergiant OW Gem DGL stage just after the merger and had substantial OW Gem DGL momentum removed by stellar wind and magnetic braking OW Gem DGL angular during a period of enhanced activity. This OW Gem DGL hypothesis needs to be tested. FL Lyr DM System with solar like components, detached. There are FL Lyr DM a few solar type binaries due to selection effects. V1016 Ori Period is not suitable for any of the classes V1016 Ori (but very close to DGlate values). Spectra in CEV is V1016 Ori appropriate for DGlate too, but secondary spectra is V1016 Ori A0V (Vitrichenko & Plachinda [2001AstL...27..581V]), V1016 Ori is the secondary a pre-MS star (Lloyd & Stickland V1016 Ori [1999IBVS.4809....1L])? Like BM Ori? V718 Per May belong to DGlate class only because of its very V718 Per long period, but spectra is needed to be determined V718 Per properly. According to Grinin et al. V718 Per [2008A&A...489.1233G] eclipses are caused by large V718 Per variable amounts of circumstellar dust. Grinin et al. V718 Per have suggested that V718 Per is a pre-MS post-T Tau V718 Per single star. Deleted from CEV DV Psc Active RS CVn system, detached according to LC DV Psc solution of Zhang et al. [2010NewA...15..362Z], so DV Psc may be DR, but has very short period for DR class, DV Psc lc is asymmetric like for CBV class, but period is DV Psc shorter than typical CBV value. May be classified as DV Psc CB, but secondary spectra is needed. According DV Psc to Zhang & Zhang [2007MNRAS.382.1133Z] is DV Psc near-contact system. See also [2007MNRAS.382.1133Z] DV Psc for details. Marginal and interesting system. V5158 Sgr According to Torres et al. [82] system is a V5158 Sgr hierarchical triple system composed of a slightly V5158 Sgr evolved F6 star (the brighter object) near the end of V5158 Sgr its MS phase and an eclipsing binary with a K7-M0V V5158 Sgr star orbiting an F4V star. mu Sgr Very long period is not suitable for any of classes mu Sgr with such early spectra (DGearly, SH, CE, CG). mu Sgr Kondo et al. [1985BAAS...17..584K]: P Cyg variable mu Sgr profiles, a mass flow from the primary through inner mu Sgr Lagrangian point, interaction of this material with mu Sgr stellar wind of the secondary and is lost from a mu Sgr system. Marginal. But why period is long? V411 Ser May belong to DGearly, but lum. class of secondary V411 Ser differs from limits for other DGearlies (all have lum. V411 Ser class III-V). According to Conti et al. V411 Ser [1980ApJ...238..184C] systems is evolved and on its V411 Ser way to becoming WR system, both components well away V411 Ser from ZAMS. e is about 0.5 from radial curves.