| Orb --- | Seq --- | Note --- |
|---|---|---|
| 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. <V/124>) |
| 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). |
| B | 102 | FF Ori: The red light flashes of max. amplitude is 0.1m and duration is |
| B | 102 | about 1h is discovered. Full energy, provided in the flash is |
| B | 102 | 27.2L_{sun}_=10^36^erg/s, r=1.3kpc. |
| B | 103 | FH Ori: One of the features of this system is the apsid line motion with |
| B | 103 | significant rate: 20deg/year. r=1585pc. Period decreases. |
| B | 104 | FK Ori: Refered to probably members of Ori I assotiation. Period increases. |
| B | 104 | r=470pc. |
| B | 105 | FR Ori: A member of Ori I assotiation. Age of main component is 2*10^7^yr. |
| B | 107 | Z Per: Seven sudden leaps supepose quick decreasing of the period: |
| B | 107 | dP/dt=1.54*10^-6^days/year (Qian, 2001AJ....122.1561Q). T0=2425481.3717d. |
| B | 108 | DK Per: T0=2442492.373d. r=630pc |
| B | 109 | RV Per: T0=2442046.924d |
| B | 110 | WY Per: T0=2446002.3497d. |
| B | 111 | XZ Per: T0=2425150.453d. |
| B | 112 | AG Phe: r=197pc. |
| B | 116 | WX Sgr: Visual component m=12.5 is observed at r=0.4 arcsec, It can be a |
| B | 116 | physycal component with high confidence (Chambliss, 1992PASP..104..663C). |
| B | 118 | XY Sgr: T0=2419979.372d. |
| B | 120 | DV Sgr: T0=2431281.172d. |
| B | 123 | BS Sct: T0=2440148.631d. |
| B | 125 | SV Tau: r=630pc. |
| B | 127 | V Tuc: T0=2436139.1410d. |
| B | 130 | RR Vul: T0=2435035.428d. |
| B | 131 | AT Vul: T0=2429906.936d. |
| B | 134 | AY Vul: Maybie main component is a subgiant r=830pc. T0=2446622.49234d. |
| B | 136 | CD Vul: T0=2446298.505d. |