Contents of: V/115/./notes.dat

The following document lists the file notes.dat from catalogue V/115.
Also available: plain copy of the file with f77 program to read file into arrays or line by line
File is also available in FITS, Tab-separated format, or in HTML.

## (from tabmap V6.0 (2016-08-18)) 2019-11-13T07:11:08
#-- V/115 Semi-detached eclipsing binaries (Surkova+, 2004)
#---Table: V/115/./notes.dat Notes  (391 records)
#       Orb A1     ---   [AB] Origin of the orbit, as in tables 1 and 2
#       Seq I3     ---   Sequential number
#      Note A75    ---   Text of the note
O|   |
r|   |
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.

© Université de Strasbourg/CNRS

    • Contact