A 1 TW And: Improved elements can be found at (Vivekananda, Sarma, A 1 1997BASI...25...93V). High resolution spectrum can be found at (Popper, A 1 1996ApJS..106..133P). R=256pc. A 2 RY Aqr: There is a visual component (m=12.2) at 4.2" from the object which A 2 is thought to be a physical companion with high confidence (Chambliss, A 2 1992PASP..104..663C). Period variability can be due to a presence of third A 2 object with P~7 years. Primary component is near to filling it's Roshe A 2 lobe. R=180pc. A 3 KO Aql: Absolute and spectroscopic elements have been found (Mader et al., A 3 1996PASP..108..404M). System period is increasing. A 4 QS Aql: Elements have been found roughly. There is a visual component A 4 (m=6.6) at 0.17" from the object which is thought to be physically A 4 connected with the system with high confidence. A 5 TT Aur: Elements have been found with high accuracy. Exploration history of A 5 this system described at (Terrell, 1991MNRAS.250..209T). Presence of third A 5 component with P=12.2 years is possible. Disk around Primary component is A 5 observed (Ozdemir et al., 2001PASA...18..151O) dP/P=2*10^-10^, A 5 dM/dt=1.8*10^-10^M_{sun}_/year. T0=2448599.2964d. r=1.03kpc. A 6 IM Aur: O-C diagram of the system has remarkable sine-type variability with A 6 P=3.75 years (Chambliss, 1992PASP..104..663C, Borkovits et al., A 6 2002A&A...392..895B). This variability may be due to presence of third A 6 body. Period variability is explored at (Guelmen et al., A 6 1984IBVS.2469....1G). Ephemeris of the system can be also found in this A 6 work. R=350pc. A 7 Y Cam: There is a third light in the system L3~0.10. Third component mass A 7 is about 5.49M_{sun}_. This third object can be a relativistic one. A 7 T0=2443259.4335d. Primary component is known as a Pulsar delta Sct type A 7 (Kim, Lee et al., 2002A&A...391..213K). A 8 S Cnc: q_phot=0.095, r=371pc. Companion has less stellar mass found from A 8 the direct spectroscopic observations. Extended atmosphere is surrounding A 8 degenerated companion. System is at the finish mass transfer stage. A 8 Primary component has a sufficient asynchronous rotation. A 9 R CMa: Both component have excess of luminosity with respect to their A 9 masses. It's supposed that primary component luminosity excess is due to A 9 helium excess. The object is a member of old galactic disk. O-C diagram A 9 behavior is evidence of presence of third component. Evolution status is A 9 discussed at (Varricatt & Ashok, 1999AJ....117.2980V). A 10 HH Car: The Primary is located a little under the ZAMS on the GRD. The A 10 system is a good example of non-conservative mass transfer. A 11 RZ Cas: Photoelectric monitoring showed primary minimum shape variability A 11 and spasmodic variations of the orbital period (Narusawa Shin-Ya et al., A 11 1994AJ....107.1141N; Hegedous et al., 1992Ap&SS.187...57H). Secondary A 11 minimum depth is 0.08m. Emission lines emerging shows remarkable mass loss A 11 rate (Kuznetsova et al., 1982, Solar and stellar physics / Editor) A 11 dM/dt=3.3M_{sun}_/yr (Chaubey, 1993BASI...21..597C). X-Ray variability has A 11 been found by ASCA and ROSAT satellites. The Primary is undergoing A 11 delta Sco type pulsations with period 23.15min dM=0.02m (Ohsima et al., A 11 2001AJ....122..418O). A 12 TV Cas: Typical semidetached system. Exploration history can be found at A 12 (Winiarski et al., 1983AcA....33..291W). Spectroscopic elements can be A 12 found at (Walter, 1973; Khalesseh et al., 1992A&A...257..199K). R=275pc, A 12 T0=2436483.8091d. Age is 3.24*10^08^yr. A 13 TW Cas: Period variability is discussed at (Lloyd et al., A 13 2002Obs...122...85L). A 14 ZZ Cas: Elements are found very roughly. O-C diagram is thought to be A 14 influenced by third component with P~50.9yr (Kreiner et al., A 14 1991BAICz..42..345K). A 15 GG Cas: Third body presence is possible. A 16 BF Cen: Primary eclipse is full. The object is a member of NGC 3766. A 17 U Cef: Typical active Algole-type system. Light curve is distorted, A 17 emission lines are present, transient disk are formatted and orbital A 17 period variability are observed (Olson 1980ApJ...237..496O; Olson, A 17 1986AJ.....91.1421O). Works review concerning light and radial velocity A 17 curve solving can be found at (Rafert et al., 1991ApJ...377..278R). X-Ray A 17 luminosity at 1-10kev band assuming GINGA observation is 5*10^30^erg/s A 17 (Gimenez et al., 1993A&AS...97..261G). Photometric mass relation q=0.52. A 17 It does not equal to spectroscopic one. Physical system parameters A 17 assuming q=0.52: A=13.60R_{sun}_, m1=3.57M_{sun}_, m2=1.86M_{sun}_, A 17 R1=2.414R_{sun}_, R2=4.404R_{sun}_, logL1=1.92, logL2=1.03, r=205pc A 17 (Burnett et al., 1993AJ....106.1627B). Period increasing is observed A 17 (Surkova, 1993, Astronomical and Geodesic research: Stellar clusters and A 17 binaries: Scientific works collection. Ekaterinburg: UrSU, p. 97.). A 18 RS Cep: Long period Algole with light curve anomalies. Accretion disk A 18 temperature T=6000K. (Olson, 1986AJ.....91.1421O). System exploration A 18 history can be found at (Stuhlinger et al., 1984AJ.....89..562S). R=910pc. A 18 T0=24408.677d. A 19 XX Cep: O-C diagram indicates third body presence with m=0.9M_{sun}_ A 19 (Mayer, 1984BAICz..35..180M). A 20 XY Cep: Abslote elements obtained by different authers have remarkable A 20 differences. A 21 XZ Cep: The system is very similar to V448 Cyg but has some less mass. A 21 Gas streams and envelopes present. A 22 GT Cep: Elements are found roughly. A 23 YY Cet: System will become overcontact in 1*10^9^ years. Companion has mass A 23 and radius excess (McFarlane et al., 1986MNRAS.218..159M). A 24 U CrB: There is a quasi-stable disk surrounding more massive accretor and A 24 gas streams from the companion which is thought to be a magnetic active A 24 cold star (Albright et al., 1996ApJ...459L..99A). Radial velosity curve is A 24 analysed at (Yerly, 1999Obs...119Q.344Y). O-C diagram can be found at A 24 (Borkovits, Hegedus, 1996A&AS..120...63B), ephemerids at (Mayer et al., A 24 1991BAICz..42..225M). A 25 RW CrB: R=245pc. Period is decreasing dP/dt=4.29*10^-08^days/year (Qian, A 25 2000AJ....119.3064Q). A 26 AB Cru: Both components are thought to be near upper MS limit. A 27 AI Cru: System age is about 1e07 yr. Now system is at a stage of slow mass A 27 loss. The system probably belongs to NGC4103. T0=2446.4063d. A 28 SW Cyg: Emission in the senter of the primary minimum and near third A 28 contact is observed (Hall, 1979AcA....29..653H). Gas stream from magnetic A 28 active cold companion is also observed. Accretion disk surrounding the A 28 Primary is symmetric active and stable (Albright et al., A 28 1996ApJ...459L..99A). Orbital period decreasing is accompanied be donor A 28 star brightness decreasing. (Simon, 1997A&A...327.1087S). Accretor has A 28 asynchronous rotation (w/w_k=12, V_equator_~300km/s). Period variability A 28 can due to apsidal moving. Third body presence possibility is also A 28 analysed at (Todoran et al., 1994AN....315..349T; Berrington et al., A 28 1994AJ....107.1868B; Qian et al., 2002A&A...396..609Q). A 29 KU Cyg: See (Olson et al., 1995AJ....110.2378O). Disk surrounding the A 29 Primary is observed. (Rd=32R_{sun}_, Ld=1*10^35^erg/s, Md=10^-08^M_{sun}_, A 29 T0=2433884.840d). A 30 WW Cyg: There is double peak emission. There is no remarkable period A 30 variability. A 31 V448 Cyg: Member of the cluster NGC 6871. System age is 8*10^06^yr. A 31 (Zakirov, 1992KFNT....8c..14Z). The structure of the disk-type gas A 31 envelope is described at (Volkova et al., 1993AZh....70...91V). R=1905pc, A 31 T0=2416361.107d. A 32 V548 Cyg: May be there is third body. A 33 W Del: Primary minimum is dissymmetric. Hbeta emission line is observed A 33 near full eclipse phase. A 34 Z Dra: Absolute photometric elements remarkably differ from those at A 34 (Sveshnivova, Kuznetsova, 1990, Eclipsed binaries rough absolute A 34 photometric elements catalog, Sverdlovsk: UrSU. 1, 224; 2, 232.) A 35 RZ Dra: May be the system is triple. Third component can be an MS K6 star A 35 with the orbital period P=83.5yr. A 36 TW Dra: Visual component (9.5m) was revealed at 3.4". This component can be A 36 a physical component with high confidence, Chambliss, 1992PASP..104..663C. A 36 From ROSAT data significant X-Ray variability has been found (Singth et A 36 al., 1995ApJ...445..840S). The Primary has some luminosity excess for ZAMS A 36 star. There is long-time period increasing (dP/dt=+4.46*10^-06^d/yr.) A 36 (Qian et al., 2002NewA....7..435Q). The Primary component pulsation has A 36 been found with P=0d.0556 (Kusakin et al., 2001IBVS.5106....1K). A 37 S Equ: Possibly triple system. Secondary minimum at Porb=0.5 has slight A 37 asymmetry. Spasmodic period variability lays on one's pretty fast A 37 increasing dP/dt=+1.27*10^-06^d/yr (Qian, Zhu et al., 2002ApJS..142..139Q) A 38 AS Eri: Fast del Sct-type primary component pulsations has been found. A 38 P=24.39min (Gamarova et al., 2000IBVS.4837....1G). A 39 TZ Eri: The system has non-Keplerian transient disk. Double-peaked emission A 39 is observed through all orbital cycle. R=270pc. The orbital period A 39 decreases permanently. A 40 AF Gem: Third component at 2" is observed. R=1000pc. T0=2449026.487d. A 41 RX Gem: There is third light from close component. Primary eclipse is not A 41 full. O-C diagram shows periodic oscillations with P=55.7year and 0.0645d A 41 aplitude (Qian, Liu, Tan et al., 2002PASP..114..766Q). q_phot=0.19 A 41 (Olson, Etzel, 2000AAS...197.4618O). R=455pc. A 42 RY Gem: The Primary is surrounded by an accretion disk. A 43 RW Gem: Out of eclipse light curve is asymmetric. Asymmetry is strong in A 43 secondary minimum. A 44 UX Her: Our elements have a good agreement with those at Svechnikova & A 44 Kuznetsova (1990, Cat. ) A 45 u Her: Strong asymmetry of the secondary minimum is observed. It may A 45 indicate existence of a strong gas streams in the system. The system is at A 45 the finish stage of mass transfer. UV-light curve has been obtained and A 45 resolved (Eaton, 1978AcA....28..601E). A 46 AD Her: Visual component at 4".6 has been revealed. It is thought to be A 46 physically connected with the system with high confidence. There is a A 46 double-peaked H-alpha emission line. Components masses has been found from A 46 the mass function f(m)=0.057 (Batten, Fletcher, 1978PASP...90..312B). A 47 RX Hya: R=300pc. Long time period variability is observed (Qian, A 47 2000A&AS..146..377Q). This variability is due to mass loss A 47 (3*10^-06^M_{sun}_/yr.). Pulsating component has been revealed (Kim, Kwon A 47 et al., 2002IBVS.5314....1K). A 49 TT Hya: Spectroscopic (Popper, 1989ApJS...71..595P) and photometric mass A 49 ratio are not the same. The Primary is surrounded by stable intensive and A 49 symmetrical accretion disk. T0=2448743.825d. r=194pc. A 50 TW Lac: There is a weak visual companion near this eclipsed binary. A 51 Y Leo: m1 has been found from the mass function f(m)=0.038 (Parenago, A 51 1950AZh....27...41P). A 52 T LMi: m1 has been found from the mass function f(m)=0.038 (Parenago, A 52 1950AZh....27...41P). A 53 SS Lib: Elements are very reliable. A 54 Del Lib: From ROSAT data significant X-Ray variability has been revealed A 54 (Singth et al., 1995ApJ...445..840S). A 55 AU Mon: This system is classified as one with detached subgiant at A 55 (Svechnikov and Kuznetsova, 1990, Catalogue of approximate photometric and A 55 absolute elements of eclipsing variable stars). Mass ratio is found A 55 from Plavets and Kratokhvila's tables. A 56 RE Mon: Transient accretiom disk around the Primary (Kaitchuk et al., A 56 1985PASP...97.1178K) and third light have been revealed (Vesper et al., A 56 1999AJ....118.2378V). A 57 TU Mon: R=1200pc. A 58 UX Mon: Double-contact system: the companion fills its Roche lobe as the A 58 Primary fills its critical rotational lobe. Rotational speed of the A 58 Primary is about 200km/s. Out-of-eclipse light curve is strongly A 58 disturbed. Several observers note optical variability dm=0.1 on 1 hour A 58 time scale. Periods of intensive mass transfer occurs in the system. A 58 T0=2433329.00d. A 60 UU Oph: Light curve is asymmetric. A 61 TY Peg: Our elements are differ slightly from those at Svechnikova and A 61 Kuznetsova's catalog (1990, Catalogue of approximate photometric and A 61 absolute elements of eclipsing variable stars). There is a long time A 61 scale decreasing of the orbital period. DP/dt=1.16*10^-06^d/yr A 61 (Qian, 2002PASP..114..650Q). A 62 AQ Peg: Physical and geometrical elements given by different authors are A 62 strongly differs from each other (Milano et al., 1982Ap&SS..82..189M; A 62 Chaubey, 1984BASI...12..237C). T0=2441222.7048d. A 63 AT Peg: R=360. T0=2442661.5281d. A 64 DI Peg: Triple system. Orbit semi-major axis of the outer components 10a.u. A 64 m3=1M_{sun}_. T0=2448213.8851d. r=178pc. A 65 RT Per: T0=2446038.9332d. Rate of long time period decreasing is A 65 dP/dt=-9.29*10^-08^d/yr (Qian, 2001AJ....122.2686Q). A 66 RW Per: Hall, Stuhlinger (1978AcA....28..207H) classified this system as A 66 semidetached algole-type system. Minima depth is changing. System A 66 exploration story can be found at (Olson et al., 1992AJ....103..256O). A 66 T0-2440898.333d. r=440pc. A 67 RY Per: Non-typical algol. System has a strong double-peaked emission. A 67 T0=2441655.780d. r=840pc. Speed of the Primary component rotation is two A 67 time greater than synchronous. A 68 ST Per: Olson (1987AJ.....94.1043O) revealed flux variability during full A 68 eclipse phase. O-C diagram can be found at (Borkovits at al., A 68 1996A&AS..120...63B). T0=2442436.5779d. Visual component (m=12.1) at 11.6" A 68 has been revealed and it is thought to be a physical companion. The system A 68 is possibly quadruple or multiple (Srivastava, 1988Ap&SS.143..175S). A 70 DM Per: Triple System. Third component provide 10% of the total system . A 70 flux M3=3.2M_{sun}_, P=98d, Sp B 6V. T0=2444855.5077d. r=575pc. A 71 IZ Per: There is no significant period variability (Srivastava, A 71 1987Ap&SS.129..143S). T0=2444577.5874d. A 72 Bet Per: Algol. Triple system. Third component - F0V - has orbital period A 72 1.87 yr. It can't be seen in UV band. Great deal of information about the A 72 system can be found at (Sahade, Wood, 1978, Interacting Binary Stars. A 72 Oxford: Perganon Press. P. 130.; Richards et al., 1996ApJ...459..249R). A 72 Small mass ratio (q_sn_=0.22) indicates that the system is at a finish A 72 stage of slow mass transfer. q_ph_=0.227. There is transient accretion A 72 disk surrounding B8 star. Companion is an active RS CVn-type subgiant. A 72 T0=2447780.5365d, r=29pc. A 73 Y Psc: Two fast change of orbital period lay on long time decreasing with A 73 dP/dt=4.90*10^-06^d/yr (Qian, 2002PASP..114..650Q). A 74 XZ Pup: m1 has been found from the mass function f(m=0.104). A 75 U Sge: One of the most bright and massive algols. Quasi-stable accretion A 75 disc has been revealed (Albright et al., 1996ApJ...459L..99A). Orbital A 75 period decreasing accompanied by brightness decreasing (Simon, A 75 1997A&A...327.1087S). Standard donor brightness deviations during full A 75 phase of eclipse is 0.039m (Olson, 1993AJ....106..342O). A 75 R=290pc. q_ph_=0.37. A 76 RS Sgr: There are two visual components. Period variability is negligible. A 76 T0=2445509.65553d. A 77 XZ Sgr: m1 has been found from the mass function f(m)=0.004. A 78 V356 Sgr: K1=47.6+5.8 km/s, q=0.25, m1=10.7M_{sun}_, m2=2.7M_{sun}_. A 79 V505 Sge: Using interpherometrical methods third component has been A 79 revealed (F7V, P=105-year). T0=2433490.4870d. r=128pc. A 80 U Sct: Companion radius is found from Plavets and Kratokhvilla's tables. A 81 RZ Sct: Double-contact system. Accretor fills its roshe lobe as the A 81 companion fills its critical rotational lobe. Our absolute elements differ A 81 strongly from those at (Van Hamme, Wilson, 1990AJ....100.1981V). A 81 T0=2436942.560d. A 82 RW Tau: There is a visual component (m=12.5) at 1" with is thought to be a A 82 physical companion. The depth of the full eclipse is greatest among algols A 82 (dm~5 in UV). Olson (1987AJ.....94.1043O) has revealed brightness A 82 variability of the cold magnetically active component. Standard brightness A 82 deviations are m=0.077. Transient ring surrounds the primary B8 component. A 82 There is a strong emission near quadratures. A 83 HU Tau: R=250pc. A 84 Lam Tau: Triple system. Third component: m3=0.7M_{sun}_., SpKOIV, P=0.09yr, A 84 i=69*. A 85 X Tri Flare activity has been found (Rovithis et al., 1983IBVS.2448....1R). A 85 Olson (1987AJ.....94.1043) has revealed optical variability during the A 85 full eclipse phase. There is a visual component (m=13.7) at 6.7". There is A 85 a long time period decreasing with several jumps (Qian, A 85 2002PASP..114..650Q). A 86 TX Uma: Gas stream from the subgiant and disk around the Primary are A 86 observed (Karetnikov at al., 1986AZh....63.1144K). T0=2448594.47957d. A 86 dP/dt=-7.13*10^-07^d/yr. (Qian, 2001AJ....122.2686Q). A 87 VV Uma: R=602pc. There is a regular variability in orbital period ~22yr. A 87 T0=2445006.2873d. A 88 RU Umi: Our elements differ strongly from those at (Bell et al., A 88 1993MNRAS.260..478B). q=0.32, i=83.95{deg}, m2=2.2M_{sun}_, r1=0.449, A 88 r2=0.2817, Sp K2-5. T0=2448695.43185d. r=292pc. A 91 UW Vir: There is a long time orbital period variability. (Qian, A 91 2000A&AS..146..377Q). A 94 DL Vir: Triple system. Third component has rho=0.029", A=5.9a.u., P=6.25yr, A 84 e=0.49, i=64{deg}, Sp G8III, m=1.9M_{sun}_, r=210pc. Attempts toresolve A 84 this system by interpherometric methods has failed. A 95 Z Vul: T0=2447744.4145d. dP/dt=5.7*10^-08^M_{sun}_/year. dP/P=2.87*10^-10^. A 96 RS Vul: There is a transient accretion disk surrounding the Primary and A 96 there are also gas streams from the companion with seems to an A 96 magnetically active cool star. T0=2445229.298d. B 1 TT And: To=2448483.3699d (Kreiner et al., 2002BAVSR..51..214H). B 2 UU And: Rate of secular period decreasing dP/dt=4.76*10^-7^d/year B 2 (Qian, 2001AJ....122.1561Q). B 3 XZ And: Three cyclic periods were found in O-C diagram: P1=137.5 years, B 3 P2=36.8 years, P3=11.2 years. T0=2449313.53034d. Halbegel B 3 (1984IBVS.2549....1H) classified main component spectrum as A1V B 5 FK Aql: T0=2437786.0511d. B 6 V337 Aql: Evolves in case A (Giuricin et al., 1981A&AS...43..251G). O-C B 6 diagram were analized in paper Mayer et. al. (1998A&AS..130..311M). B 6 T0=2441168.401d. B 8 V346 Aql: At r=2.5 arcsec observed a visual component m=11.4, which can B 8 probably be physycal (Chambliss, 1992PASP..104..663C). T0=2442959.4714d. B 9 R Ara: There is a visual component m=8.2 found At r=3.6arcsec. (Chambliss, B 9 1992PASP..104..663C). Light curve is complicated by third light and B 9 fluctuations about o.1m. Ultraviolet curve is evidence of high accrecion B 9 level (Gimenez, 1996RMxAC...5...21G; Kondo, 1985ApJ...295..580K). The B 9 system is in the rare-observing evolution stage now -- the stage of fast B 9 mass transfer. Nield (1991Ap&SS.180..233N) found that r2=0.20 -- lower B 9 than limit which allow to classify this system as semidetach. B 13 RZ Aur: T0=2445298.5793d. B 15 SU Boo: T0=2435222.5404d. B 16 RY Cnc: T0=2442480.4227d. B 20 XZ CMi: This star is interesting by it's large divergence of observations B 20 in primary minimum and very short period. r=464pc. B 22 del Cap: It is one of the brightest (m_max_=2.8) and nearest (r=11.4pc) B 22 binaries whith strond metall lines. On the magnetic active satellite can B 22 exist spots and flashes (Wonnacott et al., 1992MNRAS.259..251W). Malasan B 22 et al. (1989AJ.....97..499M) obtain r2=0,160, that significantly lower B 22 than critical surfase radius (Rcr.=0.287). The main component is seems to B 22 be surrounded by disk (Srivastava, 1988Ap&SS.140..337S). T0=2437810.8657d. B 23 ST Car: Giuricin et al. (1984MNRAS.206..305G) concludes, that it is an B 23 inverse Algol, i.e. main component fills its Roshe lobe, but satellite B 23 isn't. B 29 AB Cas: In this system main component is del-Sct pusating star. Period of B 29 pulsaton p=0.05828741d (Rodriguez, 1998A&A...340..196R). B 30 AQ Cas: Permanent disc around accretor is evidencely absent. Mass transfer B 30 rate is near 5*10^-7^M_{sun}_/year. Main komponent is also a fast rotator. B 30 It can be a result of angular momentum accretion from stream. Struve B 30 (1946ApJ...104..253S) and Halbegel (1984IBVS.2549....1H). T0=2426282.34d. B 33 V368 Cas: T0=2445435.3089d. B 41 SS Cet: Spectra were obtained through all the period. double-pick emission B 41 is observed near all phases. (Hunt et al., 1994BAAS...26.1461H). B 42 TX Cet: This system is similar to contact ones of early classes. B 45 TZ CrA: r=871pc B 47 SY Cyg: T0=2420001.5464d. B 48 UW Cyg: T0=2443690.0667d. B 49 UZ Cyg: The gas disk is found around the main component. Before sysem B 49 refered to semidetacheached subgiants, but now is is at the end of the B 49 fast mass transfer stage. T0=2441226.6585d. B 50 VV Cyg: T0=2420270.4515d. B 51 VW Cyg: Emission lines is observed before and after primary minimum. At the B 51 Svechnikov & Kuznetsova's catalogue (1990, Catalogue of approximate B 51 photometric and absolute elements of eclipsing variable stars) this B 51 system was refered to detached subgiants T0=2441116.8678d. B 52 ZZ Cyg: There is a visual component m=11.6 observed at r=8.5arcsec, which B 52 can be a physical component with high confidence (Chambliss, B 52 1992PASP..104..663C). B 53 AE Cyg: T0=2444586.2294d B 55 DL Cyg: Very unreliable estimation of absolute parameters is given at B 55 Borkovits et al. (1999A&A...349..515B). B 56 V346 Cyg: T0=2435686.7191d. B 58 V454 Cyg: The star in scattered cluster IC 4996. Age of cluster is B 58 7.5*10^6^years. B 60 V498 Cyg: Ephemerids for minimum times calculation is given at Mayer et al. B 60 (1991BAICz..42..225M). T0=2432771.3007d. B 61 RR Del: T0=2418183.412d. B 63 RR Dra: The transient disk was discovered around the main component B 63 (Kaitchuck, 1985PASP...97.1178K). T0=2417026.3840d. B 65 AI Dra: Spectral elements obtained, but only for main component (Duerbeck, B 65 Teuber, 1978AcA....28...41D). B 68 AL Gem: T0=2426324.4424d. B 71 X Gru: Maybie, there are gas streams making hotspots, but only for main B 71 component T0=2441858.8235d. B 73 TU Her: T0=2446990.500d. B 74 CC Her: T0=2426120.477d. B 75 DH Her: T0=2426575.467d. B 77 V338 Her: T0=2433771.3652d. B 78 VY Hya: T0=2423535.641d. B 81 UW Lac: T0=2437188.448d. B 82 VY Lac: Assimetry is observed at primary and secondary minimum. B 82 T0=2441178.4470d. B 83 AG Lac: T0=2424786.3339d. B 85 RW Leo: T0=2443324.7374d. B 86 VZ Leo: T0=2431164.3238d. B 87 RR Lep: T0=2444226.6650d. r=293pc. B 92 TZ Lyr: Visual component m=11.4 is observed at r=2.4 arcsec, It can be a B 92 physical component with high confidence (Chambliss, 1992PASP..104..663C). B 93 UZ Lyr: T0=2443689.940d. B 95 Z Nor: T0=2443343.987d. B 99 SW Oph: Visual component m=11.4 is observed at r=2.4arcsec, It can be a B 99 physical component with high confidence (Chambliss, 1992PASP..104..663C). B102 FF Ori: The red light flashes of max. amplitude is 0.1m and duration is B102 about 1h is discovered. Full energy, provided in the flash is B102 27.2L_{sun}_=10^36^erg/s, r=1.3kpc. B103 FH Ori: One of the features of this system is the apsid line motion with B103 significant rate: 20deg/year. r=1585pc. Period decreases. B104 FK Ori: Refered to probably members of Ori I assotiation. Period increases. B104 r=470pc. B105 FR Ori: A member of Ori I assotiation. Age of main component is 2*10^7^yr. B107 Z Per: Seven sudden leaps supepose quick decreasing of the period: B107 dP/dt=1.54*10^-6^days/year (Qian, 2001AJ....122.1561Q). T0=2425481.3717d. B108 DK Per: T0=2442492.373d. r=630pc B109 RV Per: T0=2442046.924d B110 WY Per: T0=2446002.3497d. B111 XZ Per: T0=2425150.453d. B112 AG Phe: r=197pc. B116 WX Sgr: Visual component m=12.5 is observed at r=0.4 arcsec, It can be a B116 physycal component with high confidence (Chambliss, 1992PASP..104..663C). B118 XY Sgr: T0=2419979.372d. B120 DV Sgr: T0=2431281.172d. B123 BS Sct: T0=2440148.631d. B125 SV Tau: r=630pc. B127 V Tuc: T0=2436139.1410d. B130 RR Vul: T0=2435035.428d. B131 AT Vul: T0=2429906.936d. B134 AY Vul: Maybie main component is a subgiant r=830pc. T0=2446622.49234d. B136 CD Vul: T0=2446298.505d.